{"Functions Text":"Several modelling works on this comet have shown that ion composition in the coma varies based on the sublimation rate of the nucleus","Functions Label":0}
{"Functions Text":"as well as strong AGN\/QSO and Supernova feedback that will heat and expel the gas (e.g.","Functions Label":0}
{"Functions Text":"Indeed, large atomic gas reservoirs, together with low molecular gas masses","Functions Label":1}
{"Functions Text":"and stellar masses","Functions Label":1}
{"Functions Text":"indicate that GRB hosts are preferentially galaxies that have very recently started a star formation episode.","Functions Label":1}
{"Functions Text":"J04414489+2301513 (a~15 AU,","Functions Label":2}
{"Functions Text":"The spectral windows adopted for the analysis of the FOCAS and NIRSPEC spectra were taken to be similar to the rest-frame wavelength intervals commonly used to fit the continua of quasars","Functions Label":2}
{"Functions Text":"and Yoon (2016a, 2016b) discuss the wave generation in a self-consistent manner by solving the adiabatic dispersion relation and wave kinetic equation for each spatial location.","Functions Label":3}
{"Functions Text":"We now extend the original formalism","Functions Label":4}
{"Functions Text":"in another direction.","Functions Label":4}
{"Functions Text":"Consequently, the image separation distribution is consistent with the SDSS measured stellar VDF","Functions Label":5}
{"Functions Text":"and the Second Southern Sky Redshift Survey (SSRS2) inferred stellar VDF","Functions Label":5}
{"Functions Text":"although the two stellar VDFs are significantly different from each other concerning their corresponding parameter values.","Functions Label":1}
{"Functions Text":"Earth-like exoplanets, mini-Neptunes, and T-type brown dwarfs may form water clouds, composed of liquid or solid particles, but warmer planets and brown dwarfs of L-type and later have been shown to form cloud particles made of a mix of materials that is dominated by Mg, Si, Fe, and O and to a lesser extent by Ti, Al, K and other elements","Functions Label":0}
{"Functions Text":"In four LSP blazars (0333 + 321, 0430 + 052, 2145 + 067, 2230 + 114), the putative UV excesses are not included in our SED fitting, as they should come from the cold accretion disk","Functions Label":2}
{"Functions Text":"We derived AV(s) by adopting a simplified model of the local distribution of the interstellar dust density","Functions Label":2}
{"Functions Text":"expressed by the relation \u03c1 = \u03c10\u00b7sech2(z\/hs), where z is the height of the star above the Galactic plane and hs is the scale-height of the dust, for which we adopted the value of 190 pc.","Functions Label":2}
{"Functions Text":"Especially during recent decades, high-resolution observations of solar super-fine structures indicate that small spicules, minor hot jets along small-scale magnetic channels from the low atmosphere upwards to the corona, petty tornados and cyclones, and small explosive phenomena such as mini-filament eruptions and micro- and nano-flares\u2014all of these small-scale magnetic activities contribute greatly to coronal heating","Functions Label":0}
{"Functions Text":"NaCl was first investigated using a chirped-pulse Fourier transform microwave (CP-FTMW) spectrometer with a laser ablation source","Functions Label":0}
{"Functions Text":"operating between 6.0 and 12.0 GHz to sample swiftly the rotational spectra of the different species present in the supersonic expansion.","Functions Label":0}
{"Functions Text":"The long-slit based observations also have drawbacks: the morphology of ENLR is sometimes irregular so that the derived size depends on the orientation of slits","Functions Label":3}
{"Functions Text":"Then, observations of oscillation modes in","Functions Label":0}
{"Functions Text":"and in B-type stars","Functions Label":0}
{"Functions Text":"provided us new Rosetta stones to constrain the transport of angular momentum in the whole Hertzsprung-Russell diagram.","Functions Label":0}
{"Functions Text":"Despite some variations in survey depth and area, these survey parameters are similar to the ongoing Kilo-Degree Survey (KiDS), Dark Energy Survey (DES), or the survey with the Hyper Suprime-Cam","Functions Label":5}
{"Functions Text":"Many reports on the eruption of filaments are concerned with torus instability or\/and kink instability","Functions Label":0}
{"Functions Text":"Many models in the literature also invoke the idea that AGN can effectively drive strong pressure-driven outflows and offset cooling if a large fraction of the accretion energy is thermalized","Functions Label":0}
{"Functions Text":"Dependent on the initial fields, varying weak (probably dominating) to strong r-process conditions can be obtained, the latter, however, only for precollapse fields beyond 1012 G","Functions Label":2}
{"Functions Text":"Only in a few rare instances has an appreciable shift in the location of the peaks been observed, e.g., the 1997 outburst of Mrk 501","Functions Label":1}
{"Functions Text":"and the activity of OJ 287 from the end of 2015 to the middle of 2017","Functions Label":1}
{"Functions Text":"More recently, other surveys also revealed that the fraction of high-EW Ly\u2009\u03b1 emitters increases towards fainter UV magnitudes","Functions Label":0}
{"Functions Text":"We used a compensated filter to eliminate the small wavelength modes linked with such numerical noise","Functions Label":2}
{"Functions Text":"The behavior for the low- and high-dust contents is quite different.","Functions Label":6}
{"Functions Text":"On the one hand, the escape fractions versus NHI,cl scales for \u03c4d,cl = 1 (filled symbols in Fig. 12) as predicted by","Functions Label":5}
{"Functions Text":"in their \u201csurface scatter\u201d approximation","Functions Label":5}
{"Functions Text":"On the other hand, however, this is not the case for the low-dust scenario presented in Fig. 12 (with unfilled symbols) where a larger value of NHI,cl implies a lower fesc.","Functions Label":6}
{"Functions Text":"Mrk 421 is a very hard spectrum \u03b3-ray source with a photon index of \u22481.77 and its semiminor and semimajor axes at 68 per cent confidence are of 0$_{.}^{\\circ}$0067 as derived in","Functions Label":2}
{"Functions Text":"While X-ray variability studies can provide accurate information on the atomic and ionized matter on scales of the BLR, the radio emission from luminous H2O masers (the so-called \u201cmegamasers\u201d) constitutes a fundamental instrument to study the geometry and kinematics of the molecular gas at sub-parsec distance from SMBH. H2O masers may trace distinct regions in the AGN environment, from nearly edge-on accretion discs to nuclear outflows in the form of jets or winds (for recent reviews see","Functions Label":3}
{"Functions Text":"The broad-band X-ray spectrum is orbital phase-dependent and can be approximately described as a power law with a high-energy cutoff and a cyclotron resonant scattering feature around 40\u2009keV","Functions Label":0}
{"Functions Text":"The temperature Tcl of each cloud is determined as the result of a one-zone calculation (for details, see","Functions Label":2}
{"Functions Text":"Indeed, only lower limits to the high-energy cut-off have been found with NuSTAR (210 keV","Functions Label":1}
{"Functions Text":"Consider the following three possibilities: (1) If energetic particles maintain a highly beamed pitch-angle distribution (which requires negligible pitch-angle scattering), curvature drift energy gain strongly dominates generalized betatron energy loss, and for all practical purposes we have a first-order Fermi acceleration mechanism as a consequence of incompressible contraction or merging of curved flux-rope magnetic fields","Functions Label":2}
{"Functions Text":"In particular, the classical simplified approach of neglecting rotation in GCs has become untenable from the observational point of view. In fact, there is an increasing wealth of observational results suggesting that, when properly surveyed, the majority of GCs rotate at some level. As of today, more than $50{{\\ \\rm per\\ cent}}$ of the sampled GCs show clear signatures of internal rotation (e.g.","Functions Label":0}
{"Functions Text":"Also, metals have been detected, using UV\/optical absorption lines, around","Functions Label":0}
{"Functions Text":"and HD 32297 (Na\u2009i,","Functions Label":0}
{"Functions Text":"The initially low polarization levels often rise during the plateau phase","Functions Label":0}
{"Functions Text":"with a polarization angle that typically remains nearly fixed throughout (e.g.","Functions Label":0}
{"Functions Text":"Nevertheless, the UV lines have so far mostly been used to detect absorbing gas with temperature range $10^5\\, \\mathrm{K} \\lt T \\lt 10^6\\, \\mathrm{K}$ from either O\u2009vi","Functions Label":0}
{"Functions Text":"We re-modeled fifty VLBA observations of 1308+326 obtained at 15 GHz (taken from the online MOJAVE archive webpage) between 1995.05 and 2014.07 with Gaussian components within the difmap-modelfit program","Functions Label":2}
{"Functions Text":"The modelfit program fits image-plane model components to the visibilities in the uv plane.","Functions Label":0}
{"Functions Text":"We did not apply self-calibration but used the calibration as provided by the MOJAVE team. Only circular components were used. The use of exclusively circular Gaussian components proved to be the most efficient way to parameterize the component properties. It reduces the number of free parameters, compared to the use of elliptical Gaussians, and allows a more secure identification of components across the epochs. Although it might have advantages to model the data of some of the epochs with elliptical components, our experience is that circular component modeling allows a more homogeneous analysis of all the epochs and more trustworthy identification of individual components in their long-term motion and evolution.","Functions Label":1}
{"Functions Text":"We used electron collisional excitation and ionization rates from the quantum mechanical computations of","Functions Label":2}
{"Functions Text":"for the energy levels of up to 5s (2S).","Functions Label":2}
{"Functions Text":"A cometary nature of these NEAs was suggested and a conclusion was made that they are either extinct fragments of comet Encke or represent (together with comet Encke) the remnants of a larger comet-progenitor of the stream","Functions Label":0}
{"Functions Text":"For the former, we calculated the ion and electron temperatures in each cell of the post-shock medium, taking into account the effects of Coulomb collisions (see","Functions Label":2}
{"Functions Text":"for the details of the implementation).","Functions Label":2}
{"Functions Text":"Once the existence of a relationship between age and chemical clocks was established (see, e.g.,","Functions Label":0}
{"Functions Text":"In the equation above, Plin(k) is the linear matter power spectrum computed using the Boltzmann code CLASS","Functions Label":2}
{"Functions Text":"assuming the Planck 2015 (Ade et al. 2016) fiducial cosmology.","Functions Label":2}
{"Functions Text":"Numerous attempts to calibrate SZ masses have been made in the literature using","Functions Label":0}
{"Functions Text":"SPT clusters","Functions Label":0}
{"Functions Text":"Andromeda hosts both very little gas and very little star formation, while the black hole is basically quiet and has some murmurs","Functions Label":0}
{"Functions Text":"while if we assume that redback companions are akin to the companions in CV systems whose outer envelopes have also been stripped through accretion, then we may expect a smaller value k2 \u223c 10\u22123","Functions Label":2}
{"Functions Text":"The case of solar pulsational stability has been studied in detail","Functions Label":0}
{"Functions Text":"while the space missions","Functions Label":0}
{"Functions Text":"and Kepler","Functions Label":0}
{"Functions Text":"have provided high-quality seismic data for stars of different flavours against which we can test models and further our understanding of stellar pulsations.","Functions Label":0}
{"Functions Text":"In this scenario, depending on the misalignment angle, the outer disk image will show narrow shadow lanes (e.g.,","Functions Label":0}
{"Functions Text":"Quasi-periodic oscillations (QPOs) have been detected from many Be binaries, such as","Functions Label":0}
{"Functions Text":"4U 0115+63","Functions Label":0}
{"Functions Text":"Yang et al. (2013) showed that at 2:1 and 6:1 resonances with a static\/slab ocean (see Section 2.2.2 of","Functions Label":0}
{"Functions Text":"), Bond albedo is lower than it is for synchronous rotation and decreases rather than increases with incident stellar flux, thus destabilizing the climate as the planet approaches the IHZ.","Functions Label":0}
{"Functions Text":"The Sun is situated at the inner edge of the Orion arm","Functions Label":0}
{"Functions Text":"Here, for each of the terms we use the sign conventions given in the source code for the pulsar timing software tempo21","Functions Label":2}
{"Functions Text":"Frequently a major issue in these applications is the use of formulations derived assuming isotropy in turbulence that is actually anisotropic","Functions Label":1}
{"Functions Text":", this being the typical case for solar wind and magnetosheath turbulence.","Functions Label":1}
{"Functions Text":"and found no Class II CH3OH masers in the sources of our sample","Functions Label":2}
{"Functions Text":"Simulations and theory together suggest that the magnetic field plays an important role in collimating the particles and giving them a jet like shape","Functions Label":0}
{"Functions Text":"A common mitigation strategy is to model the data as a Gaussian mixture of inlier and outlier distributions with differing variance","Functions Label":2}
{"Functions Text":"In","Functions Label":0}
{"Functions Text":", we applied our method to 85 972 images from 9 Ca II K archives to derive plage areas and produce the first composite of plage areas over the entire 20th century. In particular, we analysed the Ca II K archives from the Arcetri, Kodaikanal (8-bit digitisation), McMath-Hulbert, Meudon, Mitaka, Mt Wilson, Rome\/PSPT, Schauinsland, and Wendelstein sites. Five out of the nine analysed archives were amongst the most studied and prominent ones, while the remaining archives were from less studied data sources.","Functions Label":0}
{"Functions Text":"The strength of the UV-background heating is indicated by the dotted black curve. It represents the hydrogen photo-heating rate due to the UV-background photons following the model of","Functions Label":2}
{"Functions Text":"The latter is longer by roughly the mass ratio of Mars to Titan, which can be understood from Eq. (2) of","Functions Label":2}
{"Functions Text":"Unlike the subgrid recipes which involve kinetically prescribed decoupled winds and cooling-suppressed blastwaves, the FIRE simulations solve the \u2018overcooling\u2019 problem by explicitly modelling the radiation pressure, stellar winds, and ionizing feedback from young stars as taken directly from the population synthesis code starburst99","Functions Label":2}
{"Functions Text":"The galaxies presented by Bernard-Salas et al. (2009) have instead an average redshift of 0.0074, while the sample by","Functions Label":1}
{"Functions Text":"has an average redshift of 0.0044.","Functions Label":1}
{"Functions Text":"From studies on the optical\u2013IR colour\u2013magnitude diagram, it is known that FSRQs in general show an RWB trend, which is attributed to them having a luminous accretion disc","Functions Label":1}
{"Functions Text":"Mass transfer will continue for \u22481 Myr at a rate exceeding 10\u22129 M\u2299 yr\u22121 until hydrogen shell burning is finished and the star contracts to become a carbon\u2013oxygen WD with a thick helium layer and a small residual layer of hydrogen. The high accretion rate will heat the accreting WD significantly","Functions Label":0}
{"Functions Text":"It was found that the complex dielectric function from","Functions Label":2}
{"Functions Text":"for the sample obtained by heating bayerite at 1273 K, assuming a spheroid with depolarization parameters of (0.35, 0.003), produced an opacity with 11, 20, 28, and 32 \u03bcm features, so this component was included in the models.","Functions Label":2}
{"Functions Text":"For example, studies of young clusters embedded in moderate-mass MCs (\u223c104M\u2299)","Functions Label":0}
{"Functions Text":"have shown that their age histograms contain a large majority of young (1\u20132 Myr) objects, but also a tail of older (up to several Myr) ones suggesting an accelerating star formation activity, sometimes followed by a subsequent decline (see also","Functions Label":0}
{"Functions Text":"The Blandford\u2013McKee blast wave of the ultrarelativistic shock moving into a medium of uniform external density \u03c10 has radius R \u2243 2cT\u2009\u03932\/(1 + $z$) and explosion energy per unit solid angle E\/\u03a9 \u2243 \u03c10R3\u03932c2, which gives \u0393 \u2243 9(Eiso, 53\/n0)1\/8(T\/[(1 + $z$)day])\u22123\/8, where $E=10^{53}\\, \\mbox{erg}(\\Omega \/4\\pi)E_{iso,53}$ and n0 is the external density in cm\u22123","Functions Label":2}
{"Functions Text":"Note that such large values of the Lorentz factor of the emission region in the jet have been already postulated in terms of other models in order to explain extremely short flares observed in this source","Functions Label":5}
{"Functions Text":"Type II radio sources often show non-radial propagation trajectories (see Mann et al. 2003, and references therein). Wave-like large-scale disturbances propagating over the solar disk in extreme ultraviolet observations (usually referred to as \u00e2\u0080\u009cEIT waves\u00e2\u0080\u009d or \u00e2\u0080\u009cEUV waves\u00e2\u0080\u009d) are in close empirical correlation with type II radio bursts","Functions Label":0}
{"Functions Text":"In other words, the velocity equivalent of the observed line width, Wobs = c \u00d7 \u0394\u03bb\/\u03bb, at 1\/e of the peak intensity results from instrumental, Doppler, and turbulence (non-thermal) broadenings by (1)\\begin{equation} W_{\\rm{obs}}^2 = \\left(c\\times \\frac{\\Delta\\lambda}{\\lambda}\\right)^2 = W_{\\rm{instrumental}}^2 + W_{\\rm{Doppler}}^2 + W_{\\rm{turbulence}}^2, \\end{equation}Wobs2=c\u00d7\u0394\u03bb\u03bb2=Winstrumental2+WDoppler2+Wturbulence2,assuming that all three line broadening components have a Gaussian profile (Eq. (4.17) of","Functions Label":2}
{"Functions Text":"In the fitting procedure the spectroscopic parameters (i.e., the rotational, centrifugal distortion, and fine structure constants) were kept fixed at the values derived by","Functions Label":2}
{"Functions Text":"The pexrav model assumes an exponentially cutoff power-law spectrum reflected from neutral material","Functions Label":2}
{"Functions Text":"n0 is limited between 10\u22125 and 100\u2009cm\u22123, in line with what has been found in these sources","Functions Label":2}
{"Functions Text":"This affects weak and strong magnetic fields in the LoS magnetograms differently, with the daily variation remaining less than 30 G for field strengths below 1000 G and less than 75 G for field strengths below 2250 G. On average during a day this is roughly \u00b135 G","Functions Label":2}
{"Functions Text":"Nevertheless, the strength of these instrumental and observational effects does not account for the strong flux cancellation we observe in AR 11226 prior to eruption.","Functions Label":1}
{"Functions Text":"The presence of ISM grains makes it possible for the observed molecules to survive for a very long time, longer than 350 yr. The lifetimes in the presence of the large grains considered by","Functions Label":1}
{"Functions Text":"are typically a few times shorter than the age of the remnant.","Functions Label":1}
{"Functions Text":"However, the latest observations by Planck","Functions Label":3}
{"Functions Text":"indicate that there may be some problems with such an inflationary scenario","Functions Label":3}
{"Functions Text":"Their simulation results also reveal that the bipolar pulses reported in the Enceladus plume by","Functions Label":1}
{"Functions Text":"and Pickett et al. (2015) could most probably be ion holes.","Functions Label":1}
{"Functions Text":"The analytical expressions for the S\u00e9rsic model are taken from Prugniel & Simien (1997) (see also","Functions Label":2}
{"Functions Text":"SNe IIn span a wide diversity of late-time decay rates, ranging from some SNe IIn that have essentially flat light curves for many years, like SN 2005ip","Functions Label":0}
{"Functions Text":"down to those that have only weak CSM interaction and faster decline rates that are difficult to distinguish from radioactive decay or light echoes.","Functions Label":0}
{"Functions Text":"Recent works have studied lensing effects in the existing LIGO\/Virgo O1 and O2 events","Functions Label":0}
{"Functions Text":"In fact observations show either no or positive relationships between star formation rates and SMBH accretion rates but no negative trends are seen","Functions Label":3}
{"Functions Text":"The third Fermi\u2013LAT catalogue (3FGL catalogue:","Functions Label":2}
{"Functions Text":"has been used to include the contributions of sources inside the ROI.","Functions Label":2}
{"Functions Text":"Aside from electron dissociative recombination of C4H3NH+","Functions Label":1}
{"Functions Text":"neutral production of CH3C3N can occur in a few ways","Functions Label":1}
{"Functions Text":"Typical values for the underlying parameters are: $\\varepsilon _{\\operatorname{\\text{p}}}^{\\operatorname{\\text{pin}}}\\simeq 0.05-0.2$, $\\varepsilon _{\\operatorname{\\text{p}}}^{\\operatorname{\\text{f}}}\\simeq 0.1-0.5$ (see e.g.","Functions Label":2}
{"Functions Text":"Recently, quasars observed with multiple measurements, another potential cosmological probe with a higher redshift range that reaches to z \u223c 5, is becoming popular to constrain cosmological models in the largely unexplored portion of redshift range from z \u223c 2 to z \u223c 5. A sample that contains 120 angular size measurements in intermediate-luminosity quasars from the very long baseline interferometry (VLBI) observations","Functions Label":0}
{"Functions Text":"has become an effective standard ruler, which have been extensively applied to test cosmological models","Functions Label":0}
{"Functions Text":"An alternative scenario, such as dust formation in the KN that could also explain such a blue-red evolution, has been ruled out","Functions Label":0}
{"Functions Text":"The authors used their new results together with the available literature results covering up to z = 1.3","Functions Label":2}
{"Functions Text":"to further solidify the evidence supporting passive evolution and a formation redshift zform \u2248 2.","Functions Label":1}
{"Functions Text":"The upcoming LoTSS catalogs, covering a large sky area, will help us to explore further regarding","Functions Label":7}
{"Functions Text":"and the current puzzling dipole signal observed with radio catalogs","Functions Label":7}
{"Functions Text":"In case of lamp-post models","Functions Label":1}
{"Functions Text":"general-relativistic effects will rotate the polarization position angle along null geodesics from the corona towards the disc","Functions Label":1}
{"Functions Text":"and the situation becomes more general for incident disc irradiation, i.e. any incident state of polarization is possible. Our computations, apart from the unpolarized case, assumed two extreme cases of initial $p = 100\\,{\\rm {per \\, cent}}$ polarization in order to estimate its possible effects in comparison with the completely unpolarized light and in order to test that the code adheres to the stated orientation conventions.","Functions Label":1}
{"Functions Text":"While spatially extended optical jets and bipolar CO molecular outflows have been observed in numerous Class 0\/I protostars","Functions Label":0}
{"Functions Text":"near-infrared high-resolution spectroscopy and spectroimaging observations in the past two decades have made it possible to study the kinematics of the outflowing gas and physical properties at the base of the jet within a few hundred au of the driving source in Class 0\/I protostars (e.g.","Functions Label":0}
{"Functions Text":"XRD of their sample obtained from heating boehmite to 1173 K","Functions Label":1}
{"Functions Text":"suggests \u03b4-alumina to be present, though some amounts of \u03b8-alumina and \u03b1-alumina are present, as they deduce from XRD and infrared and NMR spectroscopy.","Functions Label":1}
{"Functions Text":"AGNs can release copious amounts of energy into the intracluster medium (ICM) through many ways, including: jetted outflows that inflate cavities, weak shocks, sound waves, or turbulence in the ICM (e.g.","Functions Label":0}
{"Functions Text":"It has been shown that the fraction of AGN in mergers tends to increase as the separation between the two galaxies decreases","Functions Label":0}
{"Functions Text":"On the other hand, a positive correlation exists between the average \u03a6 and the average Fidx with the linear PCC = 0.65 (refer to Figure 5(b)). Such correlation of \u03a6 with flaring activity in individual ARs has been reported in many previous studies (e.g.,","Functions Label":5}
{"Functions Text":"We have compared to N-body simulations the well-known GSM","Functions Label":1}
{"Functions Text":"We have concluded that, among the three, QGQ is the only model capable of providing a precise redshift-space correlation function on scales down to \u223c5\u2009h\u22121 Mpc over the range of redshifts covered by future surveys.","Functions Label":6}
{"Functions Text":"As BHs are heavier than typical stars, they are expected to relax into the steeper cusps. The relaxation time of BH populations is much shorter: 0.1\u20131 Gyr","Functions Label":1}
{"Functions Text":"The background Alfv\u00e9n or slow continuum can be due to the variation of the plasma density","Functions Label":0}
{"Functions Text":"Five other teams made independent detections of the same optical transient and host galaxy all within about one hour and reported their results within about five hours of one another","Functions Label":0}
{"Functions Text":"In particular, the SPS approach has been applied to observations of various Galactic and extragalactic environments (e.g.,","Functions Label":0}
{"Functions Text":"Internally, the ejecta release their energy through","Functions Label":0}
{"Functions Text":"or photospheric dissipation (e.g.,","Functions Label":0}
{"Functions Text":"and produce the prompt gamma-ray emission of GRBs.","Functions Label":0}
{"Functions Text":"The multi-DM search for single pulses (colored in yellow) on each of these visibility beams would need to be executed on a separate FRB cluster, followed by coincidence filtering to remove spurious events","Functions Label":7}
{"Functions Text":"In the obtained size distribution, erosive collisions are more important than catastrophic collisions (see Fig. 10 of","Functions Label":2}
{"Functions Text":"Taking into account the size distribution and erosive collisions, we derive t0 according to the collisional cascade (see Appendix E for derivation), (3)\\begin{eqnarray} t_0&\\sim& 1.3 \\left( \\frac{s_{\\rm p}}{\\rm 3000\\,km} \\right)^{0.96} \\left( \\frac{R}{\\rm 2.5\\,au} \\right)^{4.18}\\nonumber\\\\ &&\\quad\\times \\left(\\frac{\\Delta R}{0.4 R}\\right) \\left( \\frac{e}{\\rm 0.1} \\right)^{-1.4} {\\rm Gyr},\\label{eq:t0} \\end{eqnarray}t0~1.3sp3000\u2009km0.96R2.5\u2009au4.18where sp is the size of planetesimals, R is the radius of the planetesimal belt, and e is the eccentricity of planetesimals.","Functions Label":2}
{"Functions Text":"Their presence at high redshift can be hardly explained by pure SFGs, even requiring uncommon assumptions (e.g., large stellar rotation, binary stellar population, top-heavy initial mass function, extremely low metallicity) as discussed by a number of recent works (see","Functions Label":1}
{"Functions Text":"When the characteristic time of variability of the mass flux along the accretion disk is longer than the relaxation time of the local disk equilibrium, it is possible to use the approximation of local equilibrium","Functions Label":2}
{"Functions Text":"see also Bisnovatyi-Kogan (2011), to calculate the transient disk structure.","Functions Label":2}
{"Functions Text":"The heating by jets propagating through the galaxies could prevent gas from cooling and cut-off the gas supply for further star formation","Functions Label":0}
{"Functions Text":"With such a bin width of \u223c0.03\u2009dex, any biases in \u03be are less than $5{{\\ \\rm per\\ cent}}$ of the observational uncertainty for a BOSS CMASS-like sample (see","Functions Label":2}
{"Functions Text":"As they pass by, they modify the transverse magnetic field and velocity components but, do not alter the gas pressure or the mass density","Functions Label":0}
{"Functions Text":"at least in the linear limit and in a homogeneous background plasma.","Functions Label":0}
{"Functions Text":"Power asymmetry from CMB data has also been a matter of intense debate and scrutiny","Functions Label":0}
{"Functions Text":"Although thermochemical equilibrium models predict the formation of condensate clouds with various composition in these hot atmospheres","Functions Label":1}
{"Functions Text":"recent laboratory works highlighted that photochemistry could strongly affect the composition of exoplanet atmospheres and lead to the formation of aerosols in a variety of conditions, including the ones encountered in hot Jupiters","Functions Label":1}
{"Functions Text":"Equation (16) describes turbulent fluctuations from a Lagrangian point of view","Functions Label":2}
{"Functions Text":"Similarly, Kamazaki et al. (2001) found small condensations of 1000 au scale inside the SM1 core in the Oph A region based on 3 mm dust continuum observations with the Nobeyama Millimeter Array (see also","Functions Label":0}
{"Functions Text":"The masses of the condensations are around 0.01\u22120.1 M\u2299, comparable to or larger than the local Jeans mass.","Functions Label":0}
{"Functions Text":"The flares are accompanied by the variability of the equivalent hydrogen column density ($\\rm \\mathit{ N}_{\\rm H}$) and of the fluorescent iron lines, which is believed to be associated with clumpiness of the stellar wind, launched from the donor star","Functions Label":0}
{"Functions Text":"Large uncertainties in VCME restrict further improvements to the TT prediction of the shock. Possible solutions to this restriction could include adopting the CME\u2019s radial speed, which is derived from models (such as cone models) based on single spacecraft observations","Functions Label":1}
{"Functions Text":"The influence of tidal truncation is therefore limited to stellar multiples","Functions Label":0}
{"Functions Text":"or during the decay of higher order multiplicity","Functions Label":0}
{"Functions Text":"Many stars in the solar neighbourhood are born in regions where UV fields are sufficient to significantly shorten disc lifetimes","Functions Label":0}
{"Functions Text":"However, in Tomaru et al. (2019, hereafter Paper I) we show instead that thermally driven winds can explain this switch (see also","Functions Label":0}
{"Functions Text":"However, this may be an unlikely hypothesis, because A-type asteroids that could represent mantle material (almost pure olivine) from differentiated bodies do not exist extensively in the orbital space related to Psyche, but instead are distributed randomly in the Main Belt","Functions Label":1}
{"Functions Text":"When the line of sight to the compact object passes through one of these clumps, X-rays are absorbed by the moderately ionized material in the clump, leading to a so-called dipping event. This is also observed for other sources","Functions Label":5}
{"Functions Text":"This strengthened earlier results based on smaller samples (e.g.,","Functions Label":5}
{"Functions Text":"Later, numerical algorithms based on Monte Carlo techniques were developed to solve radiative transfer for more general cases. Now theoretical studies mostly rely on them (e.g.,","Functions Label":0}
{"Functions Text":"In this regard, the upcoming ADITYA-L1 mission","Functions Label":7}
{"Functions Text":"with the Visible Emission Line Coronagraph","Functions Label":7}
{"Functions Text":"will provide much better data and hence will help in arriving at much stronger conclusions on the evolution of CME legs.","Functions Label":7}
{"Functions Text":"We then used the phases determined in","Functions Label":2}
{"Functions Text":"during our last observing season as starting values,","Functions Label":2}
{"Functions Text":"Recent high-resolution hydrodynamical simulations of \u2018zoomed\u2019 cosmological haloes have shown that there is a significant difference between the velocity distributions of DM particles and galaxies themselves; whether galaxies (i.e. overdensities of stars in hydrodynamical simulations) or DM subhaloes are used makes comparatively little difference","Functions Label":1}
{"Functions Text":"Interaction of CRs with molecular clouds is accompanied by various processes generating observable radiation signatures, such as","Functions Label":0}
{"Functions Text":"as well as production of neutral pions whose decay generates gamma-rays in the GeV (e.g.,","Functions Label":0}
{"Functions Text":"The distance to GoHam is not known precisely, but a value d = 250 \u00b1 50 pc is required to satisfy all the existing observational constraints","Functions Label":2}
{"Functions Text":"We here adopt this value with the uncertainty.","Functions Label":2}
{"Functions Text":"Figure 13a shows that this evolution exhibits three distinct phases: (i) the early phase (between t\u2004=\u20040 and 250 s), where the velocity growth occurs exponentially (linearly on the logarithmic-linear scale), which is called the linear growth regime; (ii) the middle phase between t\u2004=\u2004250 and 665 s, where the growth rate is slower compared to the linear phase, which is called the Rutherford regime","Functions Label":2}
{"Functions Text":"and (iii) the final phase, which starts at t\u2004=\u2004665 s, where the instability suddenly develops in an explosive way, and finally saturates at a later time, which we call the post-Rutherford regime.","Functions Label":2}
{"Functions Text":"This model was successfully applied to explain several observed core distances","Functions Label":1}
{"Functions Text":"however it is not able to explain all observations","Functions Label":1}
{"Functions Text":"Comparisons of the two methods show quite good agreement and reasonable agreement with the full quantum calculations is found, particularly for the most important processes with the largest rates","Functions Label":5}
{"Functions Text":"Other mechanisms proposed are","Functions Label":0}
{"Functions Text":"spiral shocks associated with very young binary systems orbiting within a circumbinary disc","Functions Label":0}
{"Functions Text":"Recent studies increasing the statistics of sources with detection of molecular outflows have widened the range of measured energetics (e.g.","Functions Label":0}
{"Functions Text":"While the Loison et al. (2015) CH3C3N model corroborates the upper atmospheric abundance of C4H3N inferred by","Functions Label":5}
{"Functions Text":"a large disparity between the photochemical models (and within the ensemble of models produced by Loison et al. 2015) arises in the lower atmosphere due to the poorly constrained C4H3N branching ratios and reaction rate coefficients at temperatures appropriate for Titan.","Functions Label":6}
{"Functions Text":"In the case that there is an MS star close to an AGB star, a substantial fraction of the mass loss may be accreted onto the MS companion","Functions Label":0}
{"Functions Text":"As a result, the metallicity of the companion may change. Such early stage low-mass stars become chemically peculiar, and their future evolution will be strongly affected.","Functions Label":0}
{"Functions Text":"Even more interestingly, the detection of multi-periodic brightness variations in low-mass WDs","Functions Label":0}
{"Functions Text":"has brought about new classes of pulsating stars known as ELMVs and pre-ELMVs, respectively (ELM and pre-ELM variables, respectively).","Functions Label":0}
{"Functions Text":"Overall, we find that constraints on tides, radius, possible p\u2013g instabilities","Functions Label":5}
{"Functions Text":"and the EoS from GW190425 are consistent with those obtained from GW170817","Functions Label":5}
{"Functions Text":"For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm\u22123 is assumed","Functions Label":2}
{"Functions Text":"To convert from surface brightness to density, we use the following widely used approach","Functions Label":2}
{"Functions Text":"Nogueras-Lara et al. (2020a) have used the luminosity of red clump stars to conclude the majority ($\\sim 95\\, \\mathrm{per\\, cent}$) of the nuclear stellar disc formed more than $8\\, \\mathrm{Gyr}$ ago with some evidence of a more recent ($\\lt 1\\, \\mathrm{Gyr}$ ago) star formation burst","Functions Label":0}
{"Functions Text":"This is consistent with ongoing\/recent star formation within the central molecular zone","Functions Label":5}
{"Functions Text":"and is broadly consistent with the conclusions of Bernard et al. (2018) on the wider bar\/bulge but possibly suggesting the nuclear stellar disc is on average older than the surrounding bulge.","Functions Label":5}
{"Functions Text":"Furthermore, our photometric data also constrain the long-term variability of DES17X1boj to a level below what was seen in SN2009ip","Functions Label":1}
{"Functions Text":"and SN2016bdu","Functions Label":1}
{"Functions Text":"in the years before the brightest event (MV in range \u221213 to \u221214).","Functions Label":1}
{"Functions Text":"The orbit has a period of \u223c10 days (typical value of Kepler planets), and it is sufficiently close to the central star to be subject to significant photo-evaporation effect","Functions Label":2}
{"Functions Text":"Using the J0740 proper motion value from Table 1, the Sun\u2019s Galactocentric velocity and the distance (240\u2009km s\u22121 and 8.34 kpc, respectively;","Functions Label":2}
{"Functions Text":"we calculated these corrections to the pulsar period derivative: $\\dot{P}_{\\rm S}=3.0\\times 10^{-21}$, $\\dot{P}_{\\rm G,\\perp }=-1.6\\times 10^{-22}$, $\\dot{P}_{\\rm G,p}=3.8\\times 10^{-23}$ for the minimum and $\\dot{P}_{\\rm S}=6.9\\times 10^{-21}$, $\\dot{P}_{\\rm G,\\perp }=-2.2\\times 10^{-22}$, $\\dot{P}_{\\rm G,p}=8.9\\times 10^{-23}$ for the maximum pulsar distance estimates.","Functions Label":2}
{"Functions Text":"AREPO has been used to produce simulations of the Universe at a wide range of scales. At the largest scales, we have uniform volume cosmological simulations such as the Illustris","Functions Label":0}
{"Functions Text":"suites. These simulations have box sizes ranging from \u223c50 to \u223c300\u2009Mpc and baryonic mass resolutions ranging from \u223c105 to 107\u2009M\u2299.","Functions Label":0}
{"Functions Text":"In addition, the linear polarization P.A.s across pulse phase can constrain the beam size and inclination angles, with respect to the pulsar\u2019s rotation axis and our line of sight (LoS). For example, the rotating vector model (RVM) predicts a smooth \u2018S\u2019-shape, due to the projected vectors of the magnetic field lines as they sweep across our LoS (e.g.","Functions Label":0}
{"Functions Text":"This trend is consistent with previous results in the literature, which have shown that large-scale bias is more strongly correlated with halo-centric overdensity than it is with halo mass (see e.g.","Functions Label":5}
{"Functions Text":"BCGs constitute a special category of objects with peculiar star formation histories (SFHs) seen from both observations","Functions Label":0}
{"Functions Text":"and models","Functions Label":0}
{"Functions Text":"Studies of SMGs over the past few tens of years have provided valuable insights into their properties. These include","Functions Label":0}
{"Functions Text":"merger incidence (e.g.","Functions Label":0}
{"Functions Text":"From the median values of $\\bar{\\mathcal {R}}_{190814}=7\\rm \\, Gpc^{-3}\\, yr^{-1}$","Functions Label":2}
{"Functions Text":"$\\bar{\\mathcal {R}}_{\\rm 170817}=760\\rm \\, Gpc^{-3}\\, yr^{-1}$, and $\\bar{\\mathcal {R}}_{\\rm 190425}=460\\rm \\, Gpc^{-3}\\, yr^{-1}$","Functions Label":2}
{"Functions Text":"we obtain the effective surveyed space\u2013time volumes $VT=1.2\/\\bar{\\mathcal {R}}$ for each of these three events (\u20181.2\u2019 is the median of $\\mathrm{d}P\/\\mathrm{d}\\mathcal {N}$).","Functions Label":2}
{"Functions Text":"Alternatively, such a change in the PA can be obtained due to magnetic reconnection, e.g. in the ICMART model","Functions Label":1}
{"Functions Text":"where the local magnetic field orientation, which is orthogonal to the wave vector of the emitted photon, itself changes by 90\u25cb as the field lines are destroyed and reconnected in the emission region","Functions Label":1}
{"Functions Text":"We used dmcopy tool in CIAO: Chandra's data analysis system","Functions Label":2}
{"Functions Text":"to restrict the energy range to 0.7\u22127\u2009keV for both imaging and spectral analysis in all of the four data product files: event file, blank-sky observation, RMF and ARF.","Functions Label":2}
{"Functions Text":"Perhaps more customary today, and equivalently, is to introduce a hierarchy of formally independent time variables (e.g.,","Functions Label":2}
{"Functions Text":", so that","Functions Label":2}
{"Functions Text":"In addition, there are no dust condensations along the direction of isolated synchrones, which could have indicated short bursts of activity","Functions Label":1}
{"Functions Text":"or several separated short bursts, as in the case of P\/2013 P5","Functions Label":1}
{"Functions Text":"The prompt emission of GRB 090709A possibly showed evidence of a periodic signal","Functions Label":1}
{"Functions Text":"however this was ruled out with a more careful analysis of the prompt data from BAT, X-ray Telescope (XRT) and X-ray Multi-mirror Mission (XMM) observations of the X-ray afterglow","Functions Label":1}
{"Functions Text":"However, in the majority of these studies, the authors have targeted a constant spin period whereas a magnetar central engine is expected to have a rapidly decelerating spin period which would be very difficult to detect in standard searches for periodic signals.","Functions Label":1}
{"Functions Text":"Transit observations with Spitzer","Functions Label":3}
{"Functions Text":"have found a +208 \u00b1 110 ppm difference between the 3.6 and 4.2 \u03bcm bands, suggesting CO2 absorption.","Functions Label":0}
{"Functions Text":"While kink waves, both propagating and standing, are routinely observed in the corona (e.g.,","Functions Label":0}
{"Functions Text":"The investigations developed by Marcus et al. (2010) and","Functions Label":0}
{"Functions Text":"suggest that incorporating a realistic model of volatile transport and removal in an N-body code, may lead to reduced water contents on the resulting terrestrial-like planets, in comparison with those derived from classical models that assume perfect mergers.","Functions Label":0}
{"Functions Text":"The use of Planck and WISE data resulted in the discovery of the brightest known, dusty starburst galaxy at z > 1, the \u201cCosmic Eyebrow\u201d","Functions Label":0}
{"Functions Text":"which has also been independently recovered as one of the LPs presented in this survey work.","Functions Label":5}
{"Functions Text":"Classical bulges might have formed as a result of","Functions Label":0}
{"Functions Text":"multiple minor mergers","Functions Label":0}
{"Functions Text":"It is interesting to note, however, that if we assume a steeper exponent for the distribution function described by Eq. (7) (i.e., q = 0.80), we get a very good match with observations at all fluxes, when assuming a flux-dependent scaling factor (k = k(S); see Eq. (9)) for the","Functions Label":5}
{"Functions Text":"median size \u2013 flux relation (black solid lines on the right).","Functions Label":5}
{"Functions Text":"Line luminosities of detected CO-bearing disks span almost two orders of magnitude, in which the brightest disks have luminosities that are comparable to those of fainter Herbig Ae and T Tauri disks","Functions Label":0}
{"Functions Text":"While for operational reasons, S4 could not be measured close to the dust impacts, S4 was clearly identified in periods where the coma was very dusty","Functions Label":2}
{"Functions Text":"The accretion of gas and the dynamical evolution of BSBHs are likely to be coupled","Functions Label":0}
{"Functions Text":"such that the occurrence rate of BSBHs depends on the initial conditions and gaseous environments at earlier phases (e.g. thermodynamics of the host galaxy interstellar medium;","Functions Label":0}
{"Functions Text":"The","Functions Label":0}
{"Functions Text":"BOSS project","Functions Label":0}
{"Functions Text":"obtained additional imaging data of about 3000 deg2","Functions Label":0}
{"Functions Text":"These authors compute the collisional rate coefficients for collisions with electrons, either using perturbation methods such as those used by","Functions Label":2}
{"Functions Text":"utilizing the same halo finder as","Functions Label":5}
{"Functions Text":"In this scenario, the present \u03b3-ray emission from the Fermi bubbles arises predominantly through inverse Compton scattering of an energetic non-thermal cosmic ray (CR) electron population in the remnant structures with ambient radiation supplied by the interstellar radiation field (ISRF) and the cosmological microwave background (CMB). A subdominant component due to non-thermal bremsstrahlung may also be present, emitted primarily from regions of high gas and non-thermal electron density within the bubble (OY22). Models of this nature are broadly referred to as \u2018leptonic\u2019 models (see also","Functions Label":0}
{"Functions Text":"Although the contribution from discrete sources in the ROSAT data cannot be subtracted as accurately as it can for Chandra data, their contribution is only about 1\u2009per\u2009cent of the diffuse gas luminosity for these high-mass galaxies (see","Functions Label":2}
{"Functions Text":"Infrared and submilimetre observations of","Functions Label":0}
{"Functions Text":"SN\u20091987A","Functions Label":0}
{"Functions Text":"confirm the presence of \u223c0.1\u20131.0 M\u2299 of dust, indicating that a substantial fraction of refractory elements in their ejecta went to dust grains.","Functions Label":0}
{"Functions Text":"The use of the geodesic equation for a quasi-particle must be questioned, if this particle associates with pure quantum fluctuations","Functions Label":1}
{"Functions Text":"While this approach initially appeared to work remarkably well in the case of starburst galaxies","Functions Label":1}
{"Functions Text":"there is now ample evidence that there is no tight universal relation between the UV slope and the attenuation (e.g.,","Functions Label":1}
{"Functions Text":"The LPT for dark matter fluctuations in MG was developed in Aviles & Cervantes-Cota (2017), and further studies for biased tracers in","Functions Label":4}
{"Functions Text":"Among the rich variety of low-frequency waves observed in the Sun\u2019s atmosphere, flare-related quasi-periodic fast propagating wave trains have received much attention","Functions Label":0}
{"Functions Text":"Their quasi-periods usually range from 25 to 400 s. These wave trains were","Functions Label":0}
{"Functions Text":"and extensively observed in images acquired with the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory (SDO\/AIA;","Functions Label":0}
{"Functions Text":"In Table 3 we provide the coordinates, radial velocities, and the sum of the equivalent widths for the cluster member stars, both measured (\u201cm\u201d) and corrected (\u201cc\u201d) to the system of","Functions Label":2}
{"Functions Text":"In this paper, we consider an analysis of the PDF at redshift z = 1 in a survey volume of V = 100(Gpc\u2009h\u22121)3, which is smaller than the effective volume of upcoming surveys such as Spherex with Veff \u2248 150(Gpc\u2009h\u22121)3 and somewhat larger than existing surveys such as BOSS with Veff \u2248 55(Gpc\u2009h\u22121)3","Functions Label":1}
{"Functions Text":"However, there are increasing studies suggesting that a lower-mass binary scenario is more favorable for most SNe Ib\/c, considering the measured low ejecta masses","Functions Label":0}
{"Functions Text":"At present, data from large-scale spectroscopic surveys","Functions Label":0}
{"Functions Text":"have led to the discovery of this trend at different galactocentric radius, R, and average height, |Z|, across the Galaxy shedding light on the disc formation and evolution scenarios.","Functions Label":0}
{"Functions Text":"Some studies have indicated that not only [C\u202fII] emission is deficient in some sources, but other FIR cooling lines ([O\u202fI], [O\u202fIII], [N\u202fII]), as well (e.g.,","Functions Label":0}
{"Functions Text":"In particular, two major categories of MR have been proposed: the steady state model with a single X line and the outflow approaching the Alfv\u00e9n speed","Functions Label":0}
{"Functions Text":"The identification of Ka = 0 and lower-frequency Ka = 1 transitions, originating from J0 J and J1 J energy levels, was relatively straightforward and their assignment and analysis could be easily expanded up to 340 GHz (J\u02dd = 64) with the help of the Loomis-Wood-type plot technique from the AABS package","Functions Label":7}
{"Functions Text":"and SP-FIT\/SPCAT program suite","Functions Label":7}
{"Functions Text":"in the last decades there has been a debate on the coefficient of the metallicity term of the KB and PL relation (see e.g.","Functions Label":3}
{"Functions Text":"High velocity outflows from AGN host galaxies have been reported in numerous studies in the literature","Functions Label":0}
{"Functions Text":"using optical spectroscopy","Functions Label":0}
{"Functions Text":"The results obtained with these methods appear to be strongly dependent on a few assumptions, e.g., the degree of the polynomial adopted, the photometric technique, the centroid determination, calibrating instrument systematics over the out-of-transit only or the whole observation (e.g.,","Functions Label":0}
{"Functions Text":"identified C- and D-type asteroid spectral features for both prograde and retrograde families based on spectroscopic observations of JV-JXIII and suggested them to be similar to Jupiter\u2019s Trojan asteroids.","Functions Label":0}
{"Functions Text":"Following the method presented in","Functions Label":2}
{"Functions Text":"In L1544, the 14N\/15N ratio of several different molecules has been measured:","Functions Label":2}
{"Functions Text":"CN\/C15N = 500 \u00b1 75","Functions Label":2}
{"Functions Text":"The crystallization age of EC 002 also predates all those of the other dated achondrites, such as","Functions Label":1}
{"Functions Text":"and NWA 7325","Functions Label":1}
{"Functions Text":"However, Simpson et al. (2015) point out that the submillimetre sizes are consistent with resolved 12CO detections, while the sizes derived from 1.4 GHz imaging are about two times larger because of the cosmic ray diffusion, which can explain the results before higher frequency observations at ALMA were possible","Functions Label":1}
{"Functions Text":"For comparison, to obtain the Hubble Ultra Deep Field (UDF) image, \u223c400 hr of actual observation time (\u223c1 yr in real time) was needed","Functions Label":0}
{"Functions Text":"A tight relationship between O\/H and N\/O abundances is indeed observed in both H\u2009ii regions and local galaxies, especially at M\u22c6 \u2273 109.5M\u2299","Functions Label":5}
{"Functions Text":"Other works report, however, that LiRG can be randomly located in the HRD","Functions Label":6}
{"Functions Text":"The distinction is crucial to understanding the processes that may provide an explanation for the phenomenon,","Functions Label":3}
{"Functions Text":"One can show that the spatially varying background magnetic fields lead to the adiabatic focusing effect of charged energetic particle transport and introduces correction to the particle diffusion coefficients (see, e.g.,","Functions Label":0}
{"Functions Text":"Using the relatively strong neutral lines (i.e., \u201cO i\u201d 1355.60 \u212b and \u201cS i\u201d 1401.51 \u212b), we also perform an absolute wavelength calibration for the spectra at the \u201cO i\u201d and \u201cSi iv\u201d windows, respectively","Functions Label":2}
{"Functions Text":"Newer, alternate cosmological probes could help alleviate this issue. Recent examples of such probes include","Functions Label":3}
{"Functions Text":"QSO angular size measurements that reach to z \u223c 2.7","Functions Label":0}
{"Functions Text":"Here, we have included excitation through infrared pumping for all studied species, mostly through bands lying in the mid-infrared, where the flux in IRC\u2009+10216 is large","Functions Label":2}
{"Functions Text":"After a significant fraction of the core has crystallized, the temperature approaches the azeotropic point and the existing calculations indicate that the liquid phase is enriched in 22Ne relative to the solid","Functions Label":0}
{"Functions Text":"The mean speed of network jets is very similar, as reported in previous works (e.g.,","Functions Label":5}
{"Functions Text":"Theoretical stellar libraries like, e.g.","Functions Label":1}
{"Functions Text":"or PHOENIX","Functions Label":1}
{"Functions Text":"are generally available for both a large range in wavelength and in stellar parameters, whereas empirical libraries are found to be more incomplete in both respects. However, the advantage of the latter ones is that they are not hampered by the still large uncertainties in the calculation of model atmospheres.","Functions Label":1}
{"Functions Text":"The transverse velocities of pulsars (based on proper motion and distance estimates) are particularly large, with a mean close to 310 km s\u22121","Functions Label":0}
{"Functions Text":"Since for this present UM, the estimation of H0 from CMB alone is compatible with the local estimation of H0 by","Functions Label":1}
{"Functions Text":"thus, we can safely add both the data sets to see whether we could have something interesting.","Functions Label":1}
{"Functions Text":"The rationale behind this search is that the radio lobes of these AGNs are most likely bent because of the ram pressure that occurs due to the relative motion of the AGN host galaxy and the ICM (e.g.,","Functions Label":3}
{"Functions Text":", which makes these sources good tracers for finding galaxy clusters.","Functions Label":3}
{"Functions Text":"significantly increased the size of LAEs samples used by stacking \u22482000 and \u22484500 LAEs at redshift z \u2243 3 and 2.2 \u2264 z \u2264 6.6, respectively.","Functions Label":0}
{"Functions Text":"found typical Ly\u03b1 halo exponential scale lengths of 5\u201310 physical kpc.","Functions Label":0}
{"Functions Text":"The line force is exerted mainly by the radiation flux in the UV band (200\u20133200\u2009\u2009\u00c5), because the metal lines are densely distributed (e.g.","Functions Label":0}
{"Functions Text":"Other studies have used similar methods for budgeting oxygen","Functions Label":0}
{"Functions Text":"A harvest of astronomical observations from ground-based telescopes (e.g. UKIRT, IRTF, CFHT, and VLT) or satellites (e.g. IRAS, ISO, Akari, and Spitzer) of such lines of sight has led, since the late seventies, to the deciphering of the chemical compositions, column densities, and variations associated with these ice mantles (e.g.","Functions Label":0}
{"Functions Text":"The dynamics of the cyclotron line was shown to be dependent on the luminosity state of XRPs (see","Functions Label":0}
{"Functions Text":"for review).","Functions Label":0}
{"Functions Text":"The term \u03c6i + 1\/2 is the so-called flux limiter","Functions Label":2}
{"Functions Text":"A large proportion of the spiders, whether BWs or RBs, have been observed to exhibit (quasi-)periodic eclipses of the pulsars\u2019 radio emission (e.g.","Functions Label":0}
{"Functions Text":"that are generally attributed to excess material in the orbits","Functions Label":0}
{"Functions Text":"interfering with the propagation of the radio emission.","Functions Label":0}
{"Functions Text":"Studies of such eclipses are key for understanding mass loss from the irradiated companion stars, the properties of the medium causing the eclipses, interactions between the pulsar wind and the eclipse medium, and the mechanisms responsible for the apparent attenuation of pulsar radio emission during the eclipse.","Functions Label":3}
{"Functions Text":"This basic idea has allowed the development of global \u201cEnthalpy-Based Thermal Evolution of Loops\u201d (EBTEL) models that describe the evolution of the average temperature and density in the coronal part of the loops;","Functions Label":0}
{"Functions Text":"these models are generally in good agreement with one-dimensional hydrodynamic simulations","Functions Label":5}
{"Functions Text":"Alternatively, it is recently proposed that VHE gamma-rays from distant blazars may be the secondary gamma-rays produced in the rectilinear propagation of the UHECRs escaping from these blazars (e.g.","Functions Label":1}
{"Functions Text":"In the latter case, UHECRs interact with background photons, i.e. EBL photons and microwave background (CMB) photons, which creates UHE electrons and photons through Bethe\u2013Heitler (BH) pair production and photo-meson production. These UHE electrons and photons would interact with background photons again, and then pair cascades are induced; the secondary photons are inverse-Compton-scattered (ICS) CMB photons by the pair cascades.","Functions Label":1}
{"Functions Text":"whereas KEPLER was used to evolve the star along zero age main sequence and calculate nucleosynthesis yields and light curves","Functions Label":2}
{"Functions Text":"The observational analysis of PDRs, H\u202fII regions, and IBLs has improved considerably since the availability of far-infrared spectroscopic data from the Herschel Space Observatory (see","Functions Label":0}
{"Functions Text":"The timescale on which the coronal rain forms following the heating onset is much shorter than for the quiescent scenario; in the studied event condensations appear 10 min after the reconnection event, whereas observations of quiescent rain suggests it recurs in the same loop of the order of hours","Functions Label":1}
{"Functions Text":"An individual star-forming galaxy is expected to evolve along the relation of star-forming galaxies in the mass\u2013size plane","Functions Label":0}
{"Functions Text":"while the average size of the population as a whole increases with decreasing redshift due to processes such as mergers","Functions Label":0}
{"Functions Text":"and \u2019puffing up\u2019 due to strong active galactic nuclei (AGNs) feedback","Functions Label":0}
{"Functions Text":"but also new galaxies forming with larger radii","Functions Label":0}
{"Functions Text":"These outflows can explain the nearly constant temperatures inferred from the spectrum of optically bright TDEs","Functions Label":5}
{"Functions Text":"There is evidence for a few additional smaller shock fronts throughout the cluster volume","Functions Label":0}
{"Functions Text":"In support, observations of V404 Cyg do indicate the source","Functions Label":5}
{"Functions Text":"and was enshrouded by rapidly varying Compton-thick outflowing material","Functions Label":5}
{"Functions Text":"We segmented the sky into equal-area pixels using the HEALPix scheme","Functions Label":2}
{"Functions Text":"The derived central engine parameters are sometimes ad hoc or inconsistent. For instance, the analyses","Functions Label":1}
{"Functions Text":"and for GRB 130427A","Functions Label":1}
{"Functions Text":"led to a curious conclusion that the bulk Lorentz factor of the outflow of different layers are decreasing with time. This would lead to no, or at most very inefficient, internal shock emission. Yet both bursts have dominant non-thermal emission.","Functions Label":1}
{"Functions Text":"Conversely,","Functions Label":6}
{"Functions Text":"observe two sequences in the inner regions.","Functions Label":6}
{"Functions Text":"The thermal emission from the aligned dust grains is then polarized with polarization segments perpendicular to the field lines","Functions Label":2}
{"Functions Text":"The two coherent emission mechanisms are","Functions Label":0}
{"Functions Text":"and electron cyclotron maser (ECM) emissions","Functions Label":0}
{"Functions Text":"Nevertheless, there are examples of weakly magnetized WD pulsars, which can be explained even in the GR framework, e.g.","Functions Label":1}
{"Functions Text":"and AR Scorpii","Functions Label":1}
{"Functions Text":"where magnetic fields hardly affect their mass\u2013radius relations.","Functions Label":1}
{"Functions Text":"Both categories of method have been applied to large stellar spectroscopic surveys, including","Functions Label":0}
{"Functions Text":"RAVE","Functions Label":0}
{"Functions Text":"A similar decrease of eZ,rel,int with increasing mass is found for the bulk metal content of Solar System giants","Functions Label":5}
{"Functions Text":"where the mass where eZ,rel,int reaches 1 is extrapolated to be at about 11 MJup.","Functions Label":5}
{"Functions Text":"The scaling laws derived from the numerical simulations of downward overshooting","Functions Label":5}
{"Functions Text":"agree well with Zahn\u2019s analytical model.","Functions Label":5}
{"Functions Text":"Together with the findings of Blum et al. (2020), our results have important implications for the analysis of time delays and a potential solution to the H0 tension","Functions Label":1}
{"Functions Text":"The resulting gas density probability distribution function","Functions Label":2}
{"Functions Text":"with an additional few\u2009per\u2009cent of the mass in a power-law tail at high density","Functions Label":2}
{"Functions Text":"This discrepancy in results might originate in the nature of the collisions studied in these different experiments:","Functions Label":1}
{"Functions Text":"and Higa et al. (1996) performed collisions of a particle with a flat surface, while Hei\u00dfelmann et al. (2010) observed particle-particle collisions in a free-floating environment.","Functions Label":1}
{"Functions Text":"The minimum gap-opening mass depends on the viscosity and scale-height of the disc","Functions Label":0}
{"Functions Text":"or even Earth-mass planets","Functions Label":0}
{"Functions Text":"could produce detectable gaps.","Functions Label":0}
{"Functions Text":"We confirmed that this is indeed negligible for [O i] 6300 \u212b emission based on observations of comet C\/2012 S1 (ISON) that were performed at a similarly high airmass with ARCES, and found that the production rates derived from the ISON [O i] 6300 \u212b measurements were consistent with values determined using other methods","Functions Label":5}
{"Functions Text":"Among the better recent claims of QPOs in the gamma-ray band are of","Functions Label":1}
{"Functions Text":"and of \u223c71 d in the blazar B2 1520+31","Functions Label":1}
{"Functions Text":"found as part of a continuing analysis of blazar Fermi\u2013LAT observations.","Functions Label":0}
{"Functions Text":"Matthaeus et al. (2007) presented a similar spectrum in different regimes: energy range, inertial range, and intermediate regime where the spectrum is proportional to k\u22121 to coincide with observations","Functions Label":0}
{"Functions Text":"Previous studies have considered the implications of structure models","Functions Label":0}
{"Functions Text":"on the shape of the afterglow light curve","Functions Label":0}
{"Functions Text":"coronal dissipation fraction fc \u2248 0.45","Functions Label":2}
{"Functions Text":"However, comparing the observational constraints reported in Table 3 (without R18 data) and Table 4 (with R18), one can see that the inclusion of R18 data","Functions Label":1}
{"Functions Text":"does not seem to improve the constraints on the model parameters. In fact, the estimation of the Hubble constant H0 remains almost similar to what we found in Table 3.","Functions Label":1}
{"Functions Text":"According to recent theoretical analyses of gap structure around a planet","Functions Label":0}
{"Functions Text":"the depth and width of the gap are controlled by the planetary mass, the turbulent viscosity, and the gas temperature.","Functions Label":0}
{"Functions Text":"It is found that generally the FIP bias is higher in AR and QS regions (mainly occupied by closed loops) than in CH regions (generally taken up by open magnetic field lines)","Functions Label":0}
{"Functions Text":"MBHBs are in fact expected to emit a large amount of EM radiation in different bands","Functions Label":0}
{"Functions Text":"and possibly even through pre-merger signals","Functions Label":0}
{"Functions Text":"The distance of this source is around d \u223c 11\u2009kpc","Functions Label":2}
{"Functions Text":"Many studies suggest that BH growth precedes spheroid assembly","Functions Label":1}
{"Functions Text":"however, other studies find no significant evolution with redshift (e.g.","Functions Label":1}
{"Functions Text":"Electrostatic solitary waves have been observed in Saturn\u2019s magnetosphere","Functions Label":0}
{"Functions Text":"Because the relatively small [Na\/Fe] variation is expected from the chemical evolution model for metal-rich bulge stars and the O-depletion is indistinct in some metal-rich GCs, such as NGC 6121 and 47 Tuc (see","Functions Label":7}
{"Functions Text":"the direct comparison of bulge stars with similarly metal-rich GCs on the Na\u2013O plane would require further spectroscopic observations for such GCs in the bulge.","Functions Label":7}
{"Functions Text":"The fact that disc accretion rate was not the single factor that controlled the size or temperature of the Compton cloud, used to model the hard state spectra, lead to the conclusion that some unknown parameter, related to the truncation radius of the disc, is responsible for the hard X-ray tail","Functions Label":0}
{"Functions Text":"V\u00e1zquez-Semadeni, Gonz\u00e1lez-Samaniego & Col\u00edn (2017) have recently shown that the simulations of Col\u00edn et al. (2013) in fact produce stellar age histograms highly resemblant of the observed ones","Functions Label":5}
{"Functions Text":"On the other hand, the discovery of isolated L dwarfs in young clusters","Functions Label":0}
{"Functions Text":"and very cold very nearby Y dwarf objects (e.g.,","Functions Label":0}
{"Functions Text":"show that very low-mass isolated brown dwarfs exist and overlap with the planetary masses.","Functions Label":0}
{"Functions Text":"Alternative mechanisms such as","Functions Label":0}
{"Functions Text":"shocks from supernova remnants","Functions Label":0}
{"Functions Text":"are often invoked.","Functions Label":0}
{"Functions Text":"Based on this evidence, Troja et al. (2017) suggested that a structured jet model (e.g.","Functions Label":2}
{"Functions Text":"provided a coherent description of the entire broad-band data set. Within this framework, the peculiar properties of GRB170817A\/AT2017gfo could be explained, at least in part, by its viewing angle","Functions Label":2}
{"Functions Text":"On the other hand, it is also suggested that the gamma rays could be emitted by the hadronic processes. The relativistic protons accelerated in the Crab pulsar outer gap interact with the matter inside the nebula. and this process may contribute in the high-energy gamma-ray range (see, e.g.,","Functions Label":3}
{"Functions Text":"X-ray reverberation in black hole X-ray binaries was first robustly detected in GX 339\u20134 by","Functions Label":0}
{"Functions Text":"when the source was in its hard state.","Functions Label":0}
{"Functions Text":"and fit Kurucz ATLAS9 stellar atmosphere models","Functions Label":2}
{"Functions Text":"Such mini-outbursts or night-side activities have been observed before at","Functions Label":0}
{"Functions Text":"and comet 103P\/Hartley 2 by the EPOXI mission","Functions Label":0}
{"Functions Text":"Under the assumption of the steady state of collisional cascade, the power-law size distribution of bodies is analytically obtained and the power-law index depends on the size dependence of the collisional strength of bodies (see Eq. (32) of","Functions Label":2}
{"Functions Text":"The radial velocities show a distinct and well-known gradient across the SMC with higher velocities in the eastern part (see also fig. 5 of","Functions Label":1}
{"Functions Text":"High-resolution mid-infrared (MIR) interferometric observations have revealed a two-component morphology in the brightness distribution: (i) a larger scale, elongated component in direction of the ionization cone (along PA \u2248 107\u00b0) with a full-width at half-maximum (FWHM) size of roughly 0.8 \u00d7 1.9 pc, which is responsible for 80 per cent of the total MIR flux and was interpreted either as the directly illuminated funnel walls of the dusty molecular torus or as part of the (filamentary\/clumpy) outflow; (ii) a disc-like component with an FWHM size of roughly 0.2 \u00d7 1.1 pc and elongated along PA \u2248 46\u00b0","Functions Label":0}
{"Functions Text":"and in the seeding of large-scale magnetic fields in the universe (e.g.","Functions Label":0}
{"Functions Text":"These bright PNe seem to resemble the younger, metal-rich population in the outer stream of M31, as revealed by HST pencil-beam pointings on the Giant Stream","Functions Label":5}
{"Functions Text":"The properties that make RR Lyrae standard candles are","Functions Label":0}
{"Functions Text":"the period\u2013luminosity relation in the near-infrared (NIR) filters and in particular in the K 2.2 \u03bcm band (see e.g.","Functions Label":0}
{"Functions Text":"Among these, the very nature of the turbulent cascade of the solar wind flow and its relationship with the small-scale processes still need to be described in full","Functions Label":7}
{"Functions Text":"This is basically consistent with the detection rate and the distance distribution of BH\u2013NS merger candidates detected during LVC O3 (e.g.,","Functions Label":5}
{"Functions Text":"The characterized convex synchrotron radio spectrum peaks at around 100 MHz in the case of compact steep spectrum (CSS) sources, at about 1 GHz in the case of GHz-peaked spectrum (GPS) objects, and up to a few GHz (e.g., 5 GHz) in the case of high-frequency peakers (HFPs;","Functions Label":0}
{"Functions Text":"Even though arguments","Functions Label":6}
{"Functions Text":"microlensing","Functions Label":6}
{"Functions Text":"exist that favour a compact corona, we used extended coronae.","Functions Label":6}
{"Functions Text":"Stringent non-detections in radio","Functions Label":0}
{"Functions Text":"observations exclude nearby CSM at high significance.","Functions Label":0}
{"Functions Text":"Mid-IR (MIR) and far-IR (FIR) observations have revealed bright atomic lines from H\u2009ii regions ([S\u2009iii], [Ne\u2009iii], [Ne\u2009ii], [O\u2009iii], etc.) and PDRs ([C\u2009ii], [O\u2009i]) (e.g.,","Functions Label":0}
{"Functions Text":"Those blended emission lines can be easily detected at the position of the flare ribbon, including known and unknown emission lines, such as the C i line at 1354.29 \u212b, the Fe ii lines at 1353.02 \u212b, 1354.01 \u212b, and 1354.75 \u212b, the Si ii lines at 1352.64 \u212b and 1353.72 \u212b, and the unidentified lines at 1353.32 \u212b and 1353.39 \u212b (e.g.,","Functions Label":0}
{"Functions Text":"Some multiscale polarization observations and numerical simulations suggest that turbulent motions, rather than magnetic fields, are dynamically important to form complex gas morphologies of protostellar envelopes","Functions Label":0}
{"Functions Text":"For the regression the mpfit library","Functions Label":2}
{"Functions Text":"was used, with the variable errors handled according to York (1966) in the implementation of Tellinghuisen (2020).","Functions Label":2}
{"Functions Text":"These are produced from the collapse of the helium core of a red supergiant that had lost most of its hydrogen envelope before exploding, so the ejecta expand into the stellar wind from the pre-SN star","Functions Label":0}
{"Functions Text":"We use a fully coupled ocean model because alongside atmospheric heat transport, ocean heat transport plays a vital role in the climate of Earth","Functions Label":2}
{"Functions Text":"Importantly, the instrument on board Cassini, the Radio Plasma Wave Science instrument, does not have the ability to determine the polarity of the electric fields associated with the ESWs observed with 100% certainty as it lacks the ability to perform interferometry","Functions Label":1}
{"Functions Text":"The first identified phosphorus compound in the ISM was PN through observations of its rotational transitions in Orion-KL, W51M, and Sgr B2","Functions Label":0}
{"Functions Text":"While we do not find the signature in the ACF amplitude, this does indicate that a [Fe\/H] dependence might be expected, as was also suggested by 3D hydrodynamical simulations of convection","Functions Label":5}
{"Functions Text":"For the X-ray data, we use","Functions Label":2}
{"Functions Text":"the Chandra 4 Ms source catalog in the CDFS field","Functions Label":2}
{"Functions Text":"The typical sensitivity limits of these X-ray data are","Functions Label":2}
{"Functions Text":"\u223c10\u221217 to 10\u221216 erg cm \u22122 s\u22121 for the CDFS and HDFN fields.","Functions Label":2}
{"Functions Text":"However, the virialization of dark matter perturbations in the non-linear regime cannot be independent from the properties of DE","Functions Label":2}
{"Functions Text":"This correlates with the analysis","Functions Label":1}
{"Functions Text":"which demonstrated that the preliminary track annealing led to unpredictable changes in track lengths, resulting in a lower accuracy of nuclear charge determination.","Functions Label":1}
{"Functions Text":"For SIBEC-DM given by the field Lagrangian in Eq. (1), the self-interaction is constrained to Rc\u2004\u20041 kpc, otherwise an early radiation-like period and a large comoving Jeans\u2019 length washes out too much structure to be consistent with observations","Functions Label":1}
{"Functions Text":"This stochastic acceleration process typically causes the particle distributions to have a pronounced curvature in the energy spectrum","Functions Label":2}
{"Functions Text":"see fig. 5 from","Functions Label":2}
{"Functions Text":"Due to its simplicity and in order to allow comparison with previous work (e.g.,","Functions Label":1}
{"Functions Text":"), we used the cutoffpl model for all subsequent analysis.","Functions Label":1}
{"Functions Text":"Cosmologists have worked hard to decipher the dark energy code, but we still ignore the physical nature of the DE and hence of the ultimate cause of the observed acceleration of the Universe. Such theoretical conundrum is the so-called Cosmological Constant Problem (CCP)","Functions Label":0}
{"Functions Text":"The dashed blue line is the limit above which a halo must grow in order to overwhelm the impact of LW radiation, Mmin, LW","Functions Label":2}
{"Functions Text":"Using Eq. (1) from","Functions Label":2}
{"Functions Text":", we derived the precession time of T \u2248 530 yr.","Functions Label":2}
{"Functions Text":"This value is quite large for the wiggling waves that we see.","Functions Label":1}
{"Functions Text":"Such a gap could be opened by a super-Neptune-mass planet, depending on the parameters of the disk, such as the turbulent viscosity","Functions Label":1}
{"Functions Text":"In this context, the investigation of the evolution of group members in the nearby universe acquires a great cosmological interest because more than half of galaxies reside in such environments. Furthermore, since the velocity dispersion of galaxies is significantly lower in groups than in clusters, the merger probability and the effects of interaction on galaxy evolution are much higher. Consequently, groups provide a zoom-in on phenomena driving the galaxy evolution before the galaxies fall into denser environments (e.g.,","Functions Label":3}
{"Functions Text":"Over the past decade, many attempts to address this issue have been carried out, such as from the perspective of conventional nuclear physics and even exotic physics beyond the standard BBN framework","Functions Label":0}
{"Functions Text":"If there is no break in the spectrum, the energy budget for these particles would be untenable","Functions Label":1}
{"Functions Text":"This electric field is generated by the density gradient and different mobilities of electrons and ions","Functions Label":2}
{"Functions Text":"We can assume additional trapping due to the interaction of hydrogen with helium in the material, since helium bubbles serve as trapping sites for hydrogen atoms through synergistic effects","Functions Label":3}
{"Functions Text":", leading to a lower critical dose in the case of mixed hydrogen and helium exposure","Functions Label":3}
{"Functions Text":"The technique was originally devised under the premise that the intervening absorption lines in QSO spectra arose from discrete absorbing clouds, but this picture was challenged early by the smoothly distributed IGM captured in cosmological hydrodynamical simulations (e.g.","Functions Label":0}
{"Functions Text":"interferometric observations in the (sub)millmetre domain","Functions Label":0}
{"Functions Text":"In addition, observations of magnetic fields in voids provide bounds on their strength, depending on the analytical model: From the simplest ones, it is possible to obtain lower bounds, although when improving such models a bounded range of magnetic field strength values can be provided, ranging from 10\u221225 to 10\u221215 nG","Functions Label":1}
{"Functions Text":"From observations, field stars in dwarf galaxies do exhibit different abundance ratios from MW field stars, e.g. lower [\u03b1\/Fe] ratios and variations in neutron-capture element ratios at intermediate metallicities. However, these typically do not show up until [Fe\/H] \u223c \u22121.5","Functions Label":0}
{"Functions Text":"Since 2006, it has been suspected that mergers of compact objects could also produce the so-called long\u2013short GRBs (also known as the supernova-less long GRBs, which are apparently long-lasting but do not show any signal of supernovae down to very stringent limits), which share some properties of both long- and short-duration GRBs","Functions Label":0}
{"Functions Text":"Interesting explorations on the origin of PCEB (and specifically sdB+MS\/BD) circumbinary planets can be found in Zorotovic & Schreiber (2013),","Functions Label":0}
{"Functions Text":"Bear & Soker (2014), and V\u00f6lschow et al. (2016).","Functions Label":0}
{"Functions Text":"In fact, the E0 distribution for the high \u03ba solution is qualitatively similar to the FIDO one","Functions Label":5}
{"Functions Text":"which according to","Functions Label":2}
{"Functions Text":"is about of 0.5\u22121 Gyr after the merger","Functions Label":2}
{"Functions Text":"Secondly, there is growing evidence that the mass of any classical bulge, if present in the Milky Way, must be small","Functions Label":0}
{"Functions Text":"For these reasons, we prefer to present a second model, our Model II, which does not include any spherical central component, and which is still compatible with the rotation curve of the Galaxy, as given by Reid et al. (2014).","Functions Label":3}
{"Functions Text":"near-infrared high-resolution spectroscopy and spectroimaging observations in the past two decades have made it possible to study the kinematics of the outflowing gas and physical properties at the base of the jet within a few hundred au of the driving source in Class 0\/I protostars (e.g.","Functions Label":0}
{"Functions Text":"In our MHD simulations, \u03b2rot is adopted to be 0.4% based on the observational estimates of the core mass of \u223c1 M and the angular speed of the core rotation of 4 \u00d7 10\u221214 s\u22121. The angular speed was estimated based on the global velocity gradient along the major axis of the dense core observed with single-dish telescopes","Functions Label":2}
{"Functions Text":"A complementary result is the following: when the initial condition has positive net flux and its negative part has compact support, then the whole solution evolves into a positive function after a finite time","Functions Label":1}
{"Functions Text":"Theorem 18.29","Functions Label":1}
{"Functions Text":"The Artificial Neural Networks (ANNs) have found application in not only the traditional tasks in extragalactic astronomy","Functions Label":0}
{"Functions Text":"but also in more specialized problems such as","Functions Label":0}
{"Functions Text":"estimation of star formation properties","Functions Label":0}
{"Functions Text":"In the visual passband, the luminosity L depends on Z in the form of the so-called RR Lyrae luminosity\u2013metallicity relation (see e.g.","Functions Label":0}
{"Functions Text":"In the former scenario, galaxies experience a mass-loss from wind driven by active galactic nuclei (AGNs) or supernovae feedback, which lead to an expansion in size due to a change in the gravitational potential. In the latter, mergers either major involving merging with another galaxy of comparable mass, or minor that involves accretion of low mass companions, have to be dry to keep the low star formation rate","Functions Label":1}
{"Functions Text":"We approximate the NS as a polytropic star of index n = 0.5 (e.g.,","Functions Label":2}
{"Functions Text":"The turning point of increased relative production of carbon from massive stars takes place at A(O) ~ 8.7 dex (see Fig. 2 of","Functions Label":1}
{"Functions Text":"which equals to [O\/H] ~ 0.0 dex.","Functions Label":1}
{"Functions Text":"This observed behaviour of [C\/O] is in contrast to the steady increase of [C\/O] up to [Fe\/H] ~ 0.3 dex found, for example, by Franchini et al. (2021).","Functions Label":6}
{"Functions Text":"and that of the gamma-ray emission about the hadronic process have been also investigated (see, e.g.,","Functions Label":0}
{"Functions Text":"However, with the establishment of more and more high-energy observatories, some telescopes have possessed the performance of observing photons of exceeding to the PeV from the astronomic objects.","Functions Label":3}
{"Functions Text":"The JAGUAR catalogue provides emission line fluxes and EWs for the main lines based on modelling with the beagle code","Functions Label":2}
{"Functions Text":"Toward this goal, conventionally, new summary statistics that can only be measured with imaging have been proposed. These include the three-point correlation function","Functions Label":0}
{"Functions Text":"Direct detection of progenitor stars is still elusive for SNe Ic, which prevents us from further testing the theoretical evolution of massive stars","Functions Label":0}
{"Functions Text":"FTD models driven only by the Babcock\u2013Leighton mechanism","Functions Label":5}
{"Functions Text":"currently have the best agreement with observations","Functions Label":5}
{"Functions Text":"because the length of the simulated overlap is short and it occurs only during the minimum at low latitudes.","Functions Label":5}
{"Functions Text":"In some sources it has been found that coronae can have extremely high energy cut-off (e.g. NGC 5506,","Functions Label":0}
{"Functions Text":"and therefore thermal energy, which is inferred by measuring the curvature of NuSTAR spectra at high energy and in this context K\u2013N effects cannot be neglected.","Functions Label":0}
{"Functions Text":"This work focused on the chemistry in atmospheres with T > 1000 K and a C\/O ratio of 1 (representing C enhancement compared to the solar value of 0.54), because chemical models predict that the abundances of hydrocarbon and nitrile species increase by several orders of magnitude in these atmospheres compared to atmospheres with a low C\/O ratio","Functions Label":3}
{"Functions Text":"Therefore, they can be considered as better candidates for the formation of complex organic molecules with longer carbon chains.","Functions Label":3}
{"Functions Text":"As of today, many more mass ejection channels have been discussed: matter that becomes unbound on secular time-scales (\u223c1 s) from the post-merger accretion torus","Functions Label":0}
{"Functions Text":"and do not fully rule out a spatially non-flat Universe","Functions Label":1}
{"Functions Text":"Meanwhile, enormous efforts have been made to refine the reaction rates of key BBN reactions in the past 20 yr","Functions Label":0}
{"Functions Text":"but the probability of solving or alleviating the 7Li problem by improving our knowledge of relevant nuclear reaction rates still cannot be eliminated.","Functions Label":3}
{"Functions Text":"The comet's surface revealed a wide diversity in morphology such as layering","Functions Label":0}
{"Functions Text":"The morphology resulting from this particular type of wind\u2013binary interaction is shown in Fig. 3 in","Functions Label":0}
{"Functions Text":"In reality, the MW stellar halo contains a wealth of substructure that is not yet phase mixed, in the form of stellar streams (e.g.,","Functions Label":0}
{"Functions Text":"The key achievement of LPF was placing two gold-platinum cubes known as \u201ctest masses\u201d into a freefall so pure that it was characterized by accelerations at the femto-g level (e.g.,","Functions Label":0}
{"Functions Text":"the level required to detect the minute disturbances caused by passing gravitational waves.","Functions Label":0}
{"Functions Text":"Grillo, Lombardi & Bertin (2008) introduced a methodology to estimate cosmological parameters using strong-lensing systems (SLS; see also","Functions Label":0}
{"Functions Text":"However, if a single stellar loop were flaring, the cooling time of the confined plasma would be proportional to the loop length","Functions Label":2}
{"Functions Text":"However, the discovery of ubiquitous propagating transverse oscillations with CoMP","Functions Label":0}
{"Functions Text":"and SDO","Functions Label":0}
{"Functions Text":"led to the possibility of continuous diagnostics in time, i.e., dynamic coronal seismology.","Functions Label":0}
{"Functions Text":"Because of the faintness of the transient and its proximity to the larger, brighter main source, an automated detection algorithm such as SExtractor","Functions Label":2}
{"Functions Text":"implemented in GAIA36 2016A, was unsuccessful in deblending the two sources.","Functions Label":1}
{"Functions Text":"For example, SNe that explode within dense molecular clouds may be limited to disrupting their natal gas clouds, whilst SNe that explode into lower density environments can drive hot expanding bubbles to much larger distances (tens to hundreds of pc) and influence galactic scale processes (e.g.","Functions Label":0}
{"Functions Text":"Simultaneous observations were made with","Functions Label":2}
{"Functions Text":"the Swift UV\/Optical Telescope (UVOT;","Functions Label":2}
{"Functions Text":"with the u filter applied.","Functions Label":2}
{"Functions Text":"Especially for late M dwarfs the cut-off at 4.545 \u03bcm leads to non-negligible loss in incoming radiation of up to \u22485% (see also","Functions Label":2}
{"Functions Text":"Hence, HZ boundaries obtained with the models lie closer to the star than would be expected when accounting for this missing portion of irradiation.","Functions Label":2}
{"Functions Text":"Particles up to gigaelectronvolt energies are accelerated by strong shocks driven by CMEs of very high speeds (\u223c2000 km s\u22121) and intense, soft X-ray flares (see","Functions Label":0}
{"Functions Text":"Theoretical work suggests major mergers can provide the torque to displace such an overwhelming fraction of the angular momentum of the gas, allowing for the highest accretion rates on to the central black hole whilst transforming the galaxy morphology","Functions Label":0}
{"Functions Text":"As relevant observational evidence is steadily growing, particular attention has been devoted to tackling with SNR temporal evolution in an inhomogeneous medium, aiming at deciphering the observed asymmetries of emission morphology or clarifying the effects on the synthetic radio polarization maps exerted by various configurations of the interstellar magnetic field (e.g.,","Functions Label":3}
{"Functions Text":"In order to make the sample as complete as possible, we retrieved and added all known spectroscopic RSGs in both optical and mid-infrared (MIR) bands from Simbad","Functions Label":2}
{"Functions Text":"In Table 3 we provide the coordinates, radial velocities, and the sum of the equivalent widths for the cluster member stars, both measured (\u201cm\u201d) and corrected (\u201cc\u201d) to the system of","Functions Label":2}
{"Functions Text":"This type of geometric configurations for the BBH\u2013disk accretion systems has been revealed by many numerical simulations and analysis","Functions Label":0}
{"Functions Text":"Local thermodynamic equilibrium (LTE) is a good approximation for the H2CO level populations under optically thin and high-density conditions","Functions Label":2}
{"Functions Text":"For comparison, we show in Fig. 13 the predictions of the most recent one","Functions Label":1}
{"Functions Text":"where the updated nuclear reaction network was used.","Functions Label":0}
{"Functions Text":"This is consistent with the ${\\approx } 30\\, {{\\rm per\\, cent}}$ amplitude modulations observed in the source at 3 GHz","Functions Label":5}
{"Functions Text":"being caused by refractive interstellar scintillation in the Milky Way interstellar medium","Functions Label":5}
{"Functions Text":"The previously reported anti-correlation between tdepl and sSFR","Functions Label":5}
{"Functions Text":"is also further supported by our galaxies at z\u2004=\u20044.4\u2005\u2212\u20055.9 (Fig. 6, middle panel).","Functions Label":5}
{"Functions Text":"Our numerical experiments, however, do not seem to support claims of the steepening of the R \u221d M\u03b1 relation for CGs towards values \u03b1 \u2273 1","Functions Label":6}
{"Functions Text":"Our results appear to stand apart from similar studies in full spherical shells (e.g.,","Functions Label":6}
{"Functions Text":"in that the differential rotation is strongly quenched as a function of the magnetic Reynolds number.","Functions Label":6}
{"Functions Text":"We calculate this by using the slug stellar population synthesis code","Functions Label":2}
{"Functions Text":"We use the $\\mathcal {N}_\\mathrm{LyC}$ for each H\u2009ii region as determined from the radio observations outlined in Table \u20092 (i.e.","Functions Label":2}
{"Functions Text":"and solve for the direct radiation pressure using equation (4).","Functions Label":2}
{"Functions Text":"However, uncertainties on the observational and theoretical sides mean that the true level of disagreement is unclear. For example, while","Functions Label":1}
{"Functions Text":"derived a PN abundance of 10\u22128 relative to H2 in IK Tau, De Beck et al. (2013) and Velilla Prieto et al. (2017) derived higher abundances, (3\u20137) \u00d7 10\u22127, in this source.","Functions Label":1}
{"Functions Text":"Then, we consider the REFLKERR where the hard X-ray Comptonisation spectrum is computed with the COMPPS model","Functions Label":2}
{"Functions Text":"which appears to be a better description of thermal Comptonisation when compared to Monte Carlo simulations","Functions Label":1}
{"Functions Text":"We derive a ratio \u223c0.05, which is very similar to the average ratio derived in the disc of M 31 (see e.g.","Functions Label":5}
{"Functions Text":"Supervised learning has been used","Functions Label":0}
{"Functions Text":"and to determine the redshift of galaxies","Functions Label":0}
{"Functions Text":"This seems to be the case for the outflows driven by young stars from a very broad mass range, as previous reported by several authors","Functions Label":0}
{"Functions Text":"The left-hand panel of Fig. 2 shows sources from Gaia\u2019s DR2 LPV catalogue","Functions Label":2}
{"Functions Text":"chosen to lie within a 15\u00b0 aperture of the LMC.","Functions Label":2}
{"Functions Text":"Recent results from solar flares observed from space","Functions Label":0}
{"Functions Text":"demonstrate an NUV spectrum originating largely from Hydrogen Balmer continuum emission.","Functions Label":0}
{"Functions Text":"However, it has been shown that these events can be explained using physics beyond the standard model, as many models suggest that AAEs lend support for axionic dark matter, sterile neutrinos, supersymmetry, or heavy dark matter","Functions Label":1}
{"Functions Text":"Note that the minimum value of the drag parameters we used here is 1 \u00d7 10\u22129 km s\u22121, which was revealed as the lowest possible value","Functions Label":2}
{"Functions Text":"Nevertheless, an early ROSAT observation of the old open cluster M 67, which lies at \u223c840 pc","Functions Label":0}
{"Functions Text":"Earlier observations of the physical sizes of SMGs by CO detection and 1.4 GHz imaging suggest larger sizes (e.g.","Functions Label":1}
{"Functions Text":"These low ratios are consistent with the values found for several other stars with strong chromospheric activity","Functions Label":5}
{"Functions Text":"For instance, shallow gradient in metallicity is seen in SBS 0335\u2212052 (","Functions Label":1}
{"Functions Text":"while no significant variations were seen in Mrk 35","Functions Label":1}
{"Functions Text":"However, our result is consistent with other NLFFF results","Functions Label":5}
{"Functions Text":"In late-type AGN-host galaxies, the gas kinematics appears complex at all scales, showing several components such as bars, rings, and (warped) discs, with high velocity dispersion regions (e.g.","Functions Label":0}
{"Functions Text":"Although the current corotation radius is rco \u2248 2.25 RJ, Jupiter at its time of formation was much larger than it is today","Functions Label":2}
{"Functions Text":"and this means that the corotation radius was also larger than the current one if the conservation of the angular momentum of Jupiter is assumed. Considering the transport of the angular momentum from Jupiter to the disk, the angular momentum should have been conserved since the disk disappeared.","Functions Label":2}
{"Functions Text":"TDSs are also expected along the Parker Solar Probe orbit","Functions Label":0}
{"Functions Text":"The consideration of ambipolar diffusion processes in solar physics started many decades ago","Functions Label":3}
{"Functions Text":"but it has undergone a true explosion in terms of its use in large numerical models (e.g.","Functions Label":3}
{"Functions Text":"Such numerical calculations often encounter a problem: given the comparatively high values of \u03c7a in different cosmic environments, the advance in time may grind to a halt in magnetised regions when a standard Courant-Friedrichs-Lewy condition is adopted for the timestep based on \u03b7a.","Functions Label":3}
{"Functions Text":"For this reason, we obtained a considerable amount of biases (150\u2212300 frames) and twilight flat-fields (25\u2212100 frames) each night to reduce the Poisson noise to less than 0.2 mmag","Functions Label":2}
{"Functions Text":"However, as rapidly rotating stars evolve off the main sequence they slow down considerably and become much cooler making it relatively easy to search for planets around them. This fact was exploited by dedicated planet searches around intermediate mass sub-giants leading to dozens of planet discoveries","Functions Label":0}
{"Functions Text":"Most studies to date find that cusp-core transformations are challenging at the likely mass-scale of UFDs (M200c \u223c 109\u2009M\u2299; M* \u223c 105\u2009M\u2299; e.g.","Functions Label":1}
{"Functions Text":"However, different works used different mono-energetic bins to represent this channel, e.g.,","Functions Label":6}
{"Functions Text":"2.5 GV","Functions Label":6}
{"Functions Text":"This is probably ram pressure caused by the relative motion of galaxies with respect to the ICM","Functions Label":0}
{"Functions Text":"The influence of tidal truncation is therefore limited to stellar multiples, either in bound systems","Functions Label":0}
{"Functions Text":"The fitted radio spectral index \u03b11 from this study is \u22120.53 \u00b1 0.04, consistent with broad-band spectral indices determined using radio, optical, and X-ray data at various epochs, where the typical value is approximately \u22120.58 (e.g.","Functions Label":5}
{"Functions Text":"Along with an increasing number of observational cases, the study of fast kink oscillations in coronal loops has been significantly advanced","Functions Label":0}
{"Functions Text":"see Figure 8 for a comparison of the arc redshift distributions adopted by the pre-HFF and new HFF+ lensing models;","Functions Label":2}
{"Functions Text":"We also used some observational data obtained within several other programmes","Functions Label":2}
{"Functions Text":"It has only recently become widespread to model the formation of galaxies ab initio (e.g.","Functions Label":0}
{"Functions Text":"Currently, a limited number of observations","Functions Label":0}
{"Functions Text":"are available to explore the environment dependence of the metallicity, and most of our current understandings are based on simulations","Functions Label":0}
{"Functions Text":"Several solutions have been successfully proposed in order to deal with stellar oscillations and granulation phenomena, such as:","Functions Label":0}
{"Functions Text":"using daytime spectra of the Sun in order to measure the solar oscillations (e.g.,","Functions Label":0}
{"Functions Text":"This picture is consistent with the observed low temperature, large radius, and super-Eddington luminosity (see","Functions Label":5}
{"Functions Text":"However, there are two notable discrepancies between the HST observations and the xstar model predictions. The first is that the $[{\\rm O\\, \\small{III}}]\\, {\\lambda }$5008 emission line is observed to be 230 per cent brighter than predicted by xstar. This excess emission could be attributed to the extended source of $[{\\rm O\\, \\small{III}}]\\, {\\lambda}$5008 seen in the nucleus of NGC 3327","Functions Label":1}
{"Functions Text":"Volonteri et al. (2015b) suggest that in the merger phase, the AGN dominates the bolometric luminosity but the accretion can be very stochastic (see also","Functions Label":0}
{"Functions Text":"This image reconstruction problem inspired several computational approaches like","Functions Label":0}
{"Functions Text":"and machine learning","Functions Label":0}
{"Functions Text":"Interstellar scintillation (ISS) is difficult to distinguish from intrinsic variability without fully time-resolved data (see e.g.","Functions Label":1}
{"Functions Text":"and references therein), and can coexist with it","Functions Label":1}
{"Functions Text":"However, to obtain precise photometric transit and spot parameters, we recommend the use of a planetary pixel radius between 15 and 50 pixels","Functions Label":2}
{"Functions Text":"From the IPAC forced-photometry service","Functions Label":2}
{"Functions Text":"at the same locations, we obtain the metadata for each observation, including the magnitude limit mlim of the observation, the seeing of the observation, and the standard deviation \u03c3pix on the background at the pixel on which the SN is located.","Functions Label":2}
{"Functions Text":"A large number of kinematic arches with various morphologies not known prior to Gaia were found","Functions Label":0}
{"Functions Text":"In parallel, theoretical works and simulations have tried to explain the physical mechanisms that reproduce the measured global properties","Functions Label":0}
{"Functions Text":"In Equation (3), \u0394E denotes the width of the respective energy bin; for the typical radial velocity of solar wind in the flanks and the downwind hemisphere of the inner heliosheath, we assumed uR = 140 km s\u22121 as measured by Voyager 2, whereas uR = 40 km s\u22121 for the heliosheath in the Voyager 1 direction","Functions Label":2}
{"Functions Text":"Solar wind velocity distribution moments are described in","Functions Label":0}
{"Functions Text":"The constant, 4.64, is the r-band magnitude of the Sun in the AB system","Functions Label":2}
{"Functions Text":"Assuming the width of the gaps corresponds to 4RHill","Functions Label":2}
{"Functions Text":"On the contrary, ground-based telescopes usually have instruments which can cover several spectral lines simultaneously, e.g.","Functions Label":1}
{"Functions Text":"Gregor\/GRIS","Functions Label":1}
{"Functions Text":"One of the major error sources is the uncertainty in \u03be in various studies, including ours, based on spectra at different wavelengths","Functions Label":2}
{"Functions Text":"to the H band","Functions Label":2}
{"Functions Text":"Recently, Papaloizou (2015) proposed a semi-analytical model of three-planet resonances taking into account only the interactions between consecutive planets in the chain, with a particular focus on the Kepler-60 system (12:15:20 resonant chain, see also","Functions Label":0}
{"Functions Text":"For the purpose of this study, we equipped the code with an on-the-fly non-equilibrium chemical network, which was implemented via the public chemistry library\u202fKROME","Functions Label":2}
{"Functions Text":"Since the rotation period of the secondary star should not change (and the effect of differential rotation for star spots at different latitudes is small for M dwarfs","Functions Label":2}
{"Functions Text":"we conclude that the star-spot signal cannot be originating on the secondary component.","Functions Label":2}
{"Functions Text":"The broad-band spectral energy distribution (SED) of blazars is characterized by a two-hump structure, one peaking at low energies in the optical\/IR\/X-ray region and the other one peaking at high energies in the X-ray\/MeV region","Functions Label":0}
{"Functions Text":"One possibility to solve this issue is that the potential Psyche asteroid family was created at an early time, e.g. within the first 500\u2009Myr of Solar system history","Functions Label":1}
{"Functions Text":"This would allow the family fragments to be ground down by collisional evolution and be unobservable today. The same models show that, even in this case, today there should be several surviving fragments having diameters around 20\u2009km and above the detection limit.","Functions Label":1}
{"Functions Text":"The first study to determine masses for a sample of metal-poor halo giants with both seismic information","Functions Label":0}
{"Functions Text":"and chemistry from high-resolution APOGEE","Functions Label":0}
{"Functions Text":"spectra, was by","Functions Label":0}
{"Functions Text":"The authors used scaling relations at face value and reported masses larger (M\u2004> \u20041 M\u2299) than what would be expected for a typical old population.","Functions Label":0}
{"Functions Text":"Similar results were obtained by Casey et al. (2018), also using scaling relations for three metal-poor stars.","Functions Label":5}
{"Functions Text":"These findings led to the need for further tests of the use of asteroseismology in the low metallicity regime.","Functions Label":0}
{"Functions Text":"Theoretical stellar libraries like, e.g. BaSeL","Functions Label":1}
{"Functions Text":"are generally available for both a large range in wavelength and in stellar parameters, whereas empirical libraries are found to be more incomplete in both respects.","Functions Label":1}
{"Functions Text":"However, since such diagnostics usually involve the [N\u2009ii]\/[O\u2009ii] or the [N\u2009ii]\/[S\u2009ii] line ratios, they are strongly dependent on the assumed relation between the N\/O ratio as a function of the oxygen abundance O\/H, which is affected by a large scatter and whose evolution with cosmic time and\/or dependence on galaxy mass is also indicated as a possible origin of the observed evolution of the emission-line properties in high-zgalaxies","Functions Label":1}
{"Functions Text":"This is illustrated in Fig. 5, where thick blue and red data points show mild high-energy excesses of the electron spectra derived by Kraus (2018),","Functions Label":2}
{"Functions Text":", Kerszberg (2017) over broken power-law models derived from the fits to lower energy data.","Functions Label":2}
{"Functions Text":"NATs, which are especially common in clusters, (e.g.,","Functions Label":0}
{"Functions Text":"result from sustained relative motion between an RG and its ambient ICM; that is, the RG effectively evolves in a wind that deflects the RG jets and their discharge downwind.","Functions Label":0}
{"Functions Text":"The number of convincing dual AGN systems, mostly detected by X-ray and radio observations (e.g.,","Functions Label":6}
{"Functions Text":"are relatively few compared to the theoretically predicted abundance","Functions Label":6}
{"Functions Text":"Mass\u2013radius relation is employed to estimate radius in case of white dwarfs and neutron stars (see e.g.","Functions Label":2}
{"Functions Text":"We convert the ASAS-SN distributions into estimates of the true luminosity function using the V\/Vmax method","Functions Label":2}
{"Functions Text":"Subsequent studies found the same trend of [\u03b1\/Fe] with mass","Functions Label":0}
{"Functions Text":"leading to the dominant interpretation that in more massive ETGs, the duration of star formation was substantially shorter than in less massive ones, with timescales short enough (e.g. 0.5 Gyr) to avoid the dilution of the \u03b1 element abundance (produced by Type II supernovae) by the onset of Fe production by Type Ia supernovae. This is considered to be one of the main pieces of evidence for the shortening of star formation.","Functions Label":0}
{"Functions Text":"In this model, the dissipation of the kinetic energy of the equilibrium tide inside the star is often taken to be constant throughout the system evolution and calibrated on observations","Functions Label":0}
{"Functions Text":"The quasar survey data are also used for studies to constrain cosmological parameters","Functions Label":0}
{"Functions Text":"We make the simplifying assumption that the cloud temperature does not vary with radius; for solar composition, photoionization equilibrium is achieved at temperatures T \u223c 104 K across a wide range of ionization parameter (equation 5), and the gas temperature will therefore vary weakly with radius (e.g.","Functions Label":2}
{"Functions Text":"or parametric equations tuned by direct comparison with the outcome of numerical simulations of collisions of live galaxy pairs (e.g.","Functions Label":0}
{"Functions Text":"Regarding the radiation-hydrodynamic evolution, the conservation equation $\\Delta_\\alpha T^{\\alpha \\beta }_{\\rm (total)}=0$ is solved using the piecewise parabolic method","Functions Label":2}
{"Functions Text":"Other sources of dark energy include scalar fields such as","Functions Label":0}
{"Functions Text":"and phantom fields","Functions Label":0}
{"Functions Text":"Usually, the downstream sheath regions have larger density, temperature, mean magnetic intensity, and compressibility, and higher plasma \u03b2, as compared to the upstream solar wind","Functions Label":0}
{"Functions Text":"The large differences noted in Figure 9 are surely related to the different approximations underlying both the complex hydrodynamical simulations of ILLUSTRIS-1 and our simplified approach.","Functions Label":1}
{"Functions Text":"A key role is also played by the host cluster itself, because the mass profile of this latter becomes steeper and steeper in the core due to dynamical relaxation. Consequently, the environment gets denser with time; this trend is found to be quantifiable in terms of the number of dynamical times elapsed since the cluster formation (e.g.,","Functions Label":1}
{"Functions Text":"Therefore, each galaxy has to attain a sufficiently cold core in order to first survive in the cluster environment and then grow by accretion of matter from the ICM and mergers with other substructures.","Functions Label":1}
{"Functions Text":"The sample of","Functions Label":1}
{"Functions Text":"was X-ray selected (and optically selected for the sample of Zhu et al. 2021), which may lead to the radio jet power being very feeble compared to the bolometric luminosity in most of the RLAGNs.","Functions Label":1}
{"Functions Text":"The dimensionless accretion rate","Functions Label":2}
{"Functions Text":"and black hole mass of the source are $\\log (\\dot{\\mathscr {M}})$ = $2.63^{+0.16}_{-0.67}$ and log\u2009(MBH\/M\u2299) = $6.78^{+0.31}_{-0.06}$ with the reverberation mapping technique","Functions Label":2}
{"Functions Text":"respectively, where $\\dot{\\mathscr {M}}\\equiv \\dot{M}_{\\bullet }c^2\/L_{\\rm Edd}$, $\\dot{M}_{\\bullet }$ is mass accretion rates, c is speed of light, and LEdd is the Eddington luminosity.","Functions Label":2}
{"Functions Text":"As this model is nonrotating and the proto-neutron star convection happens after the core bounce, the gravitational strain shows a loud bounce signal at time zero, and then it is followed by a low-frequency peak PNS oscillation, which could be caused by the g-mode oscillation although the nature remains controversial","Functions Label":1}
{"Functions Text":"Then, interestingly, it followed by the quadruple radiation of the standing accretion shock instability","Functions Label":5}
{"Functions Text":"signal, which was suggested to be seen in the GW data","Functions Label":5}
{"Functions Text":"With regards to the inclusion of extra information, a recent example in template methods includes using surface brightness as a prior in spectral energy distribution templates","Functions Label":0}
{"Functions Text":", motivated by the knowledge of surface brightness dimming (1 + z)4.","Functions Label":0}
{"Functions Text":"In empirical methods this application is more straightforward, since algorithms are constructed such that it is not difficult to add extra input parameters.","Functions Label":3}
{"Functions Text":"The primary DEMs for this analysis is the quiet Sun (QS) and active region (AR) DEMs as needed for estimating the daily variations of the solar XUV spectral irradiance for the XPS Level 4 product","Functions Label":2}
{"Functions Text":"For \u03b2app and \u03b4var we used the fastest measured radial, non-accelerating apparent jet speed from the MOJAVE kinematic analysis","Functions Label":2}
{"Functions Text":"There have been rather strong claims of AGN QPOs in different bands of the electromagnetic spectrum, ranging from minutes through days through months and years (e.g.","Functions Label":0}
{"Functions Text":"Since CVs are intrinsically rather faint (typically, MV > 4 mag; e.g.","Functions Label":2}
{"Functions Text":", in general the correction for the interstellar extinction will represent an upper limit.","Functions Label":2}
{"Functions Text":"In contrast, when the primary X-ray continuum is scattered close to the SMBH, Doppler and general relativistic effects combined may give rise to a significantly broader line (FWHM tens of thousands km s\u22121), reported in at least \u223c36% of AGNs","Functions Label":1}
{"Functions Text":"see also, e.g.,","Functions Label":1}
{"Functions Text":"Along the dust lane of the elliptical galaxy, there is a molecular gas component of mass \u223c109\u2009M\u2299 as probed by various molecular lines","Functions Label":0}
{"Functions Text":"Note that the perpendicular heating rate is a nonnegligible fraction of that observed in the solar wind, where","Functions Label":2}
{"Functions Text":"If f > fm, the index of the power-law relation between A(f) and f changes","Functions Label":2}
{"Functions Text":"and is beyond the scope of this study.","Functions Label":7}
{"Functions Text":"Entire sample is shown in Toomre Diagram of rotational velocity (VLSR) and sum of quadrature of radial and vertical velocities ([$\\rm {\\it U}_{\\rm LSR}^2 + {\\it W}_{\\rm LSR}^2]^{1\/2}$)","Functions Label":2}
{"Functions Text":"These studies are based on the hypothesis that magnetic fields are passively transported by the plasma flow and provide a characterisation of advection and diffusion processes in the quiet photosphere from granular to supergranular scales (see, e.g.","Functions Label":0}
{"Functions Text":"To this we can add that Zimbardo and coworkers reported in a series of papers that spacecraft observations of SEP intensity-time profiles ahead of interplanetary shocks yielded power laws instead of the exponential profiles predicted by standard DSA. They interpreted this as a sign of superdiffusive spatial SEP transport in the shock vicinity resulting in superdiffusive shock acceleration. They predicted the superdiffusive shock acceleration to be more efficient, producing a harder accelerated power-law spectrum for SEPs, than standard DSA","Functions Label":1}
{"Functions Text":"As the hot Fe xxi line is absent in the non-flaring spectrum, the rest wavelength for the Fe xxi line (i.e., 1354.09 \u212b) is determined by averaging the line centers of the Fe XXI profiles which were used in the previous IRIS observations","Functions Label":2}
{"Functions Text":", while the rest wavelengths for the C i and Si iv lines, i.e., 1354.29 \u212b and 1402.77 \u212b, respectively, are determined from their quiet-Sun spectra","Functions Label":2}
{"Functions Text":"This layered-accretion scenario has been refined as additional non-thermal ionization sources (X-rays, UV radiation) and non-ideal magnetohydrodynamic (MHD) effects (ambipolar diffusion and the Hall effect) have been included (e.g.","Functions Label":0}
{"Functions Text":"The neon abundance can be compared and related to the results from stellar abundance analysis, as neon (and oxygen) originates from primary nucleosynthesis in massive stars (\u226510 M\u2299) and is therefore nearly independent of the evolution of LIMS, the progenitor stars of PNs","Functions Label":0}
{"Functions Text":"Assumption of the thermal blackbody radiation could overestimate the emissivity of ionizing photons at Z \u223c Z\u2299 owing to the line-blanketing effect, especially for stars with M* \u223c 10 M\u2299 (e.g.","Functions Label":2}
{"Functions Text":"These surveys offer unprecedented detection, astrometric, and spectrophotometric capabilities that allow us to characterize fainter and closer giant planets, such as the recent discovery of 51 Eri b (2 MJup at 14 au, T5-type, of an age of 20 Myr;","Functions Label":0}
{"Functions Text":"Such surveys also provide key spectral and orbital characterisation data for known exoplanets (e.g.,","Functions Label":0}
{"Functions Text":"were used as inputs for the turbulence quantities (e.g.,","Functions Label":0}
{"Functions Text":"Furthermore, mean free paths such as those discussed have,","Functions Label":5}
{"Functions Text":"Within these weak processes, although the modified Urca processes involving leptons are important, it has been shown that non-leptonic processes involving hyperons contribute more significantly towards bulk viscosity at temperatures lower than a few times 109 K","Functions Label":1}
{"Functions Text":"By pushing current observatories to their limit, recent studies derived constraints on the relative fraction of SN events that effectively contribute to the ICM enrichment. These measurements showed that SNIa and SNcc contribute relatively equally to the overall chemical enrichment in the ICM","Functions Label":1}
{"Functions Text":"Based on a literature review for papers where VLBI parallax measurements were determined using an in-beam calibrator, we find 24 similar measurements, the majority of which have been used to measure parallaxes to pulsars","Functions Label":5}
{"Functions Text":"the study of binary systems such as eccentric MSPs like PSRs J1903+0327","Functions Label":3}
{"Functions Text":"which are interesting due to their peculiar binary evolution","Functions Label":3}
{"Functions Text":"To confirm the importance of VO, water and an inversion layer","Functions Label":0}
{"Functions Text":"obtained repeated HST observations of the transmission spectrum and the secondary eclipse using the STIS and WFC 3 instruments.","Functions Label":0}
{"Functions Text":"The optical transmission spectrum displays rich variation, with multiple features consistent with VO absorption that Evans et al. (2018) could reproduce by assuming an isothermal T-P profile at 1500 K and a metallicity equivalent to 10\u00d7 to 30\u00d7 solar. Absorption bands of TiO appeared to be muted in the transmission spectrum, which was explained by Evans et al. (2018) as evidence of condensation of Ti-bearing species, which commences at higher temperatures than condensation of V-bearing species, producing for example, calcium titanates (Lodders 2002) while VO remains in the gas phase.","Functions Label":1}
{"Functions Text":"This resulted in","Functions Label":0}
{"Functions Text":"formation of globally unstable disks, and radial gas transport by dynamical friction","Functions Label":0}
{"Functions Text":"A tight relationship between O\/H and N\/O abundances is indeed observed in both H\u2009ii regions and local galaxies,","Functions Label":2}
{"Functions Text":"and it is set by the predominant nucleosynthetic origin of nitrogen from CNO burning of pre-existing stellar carbon and oxygen in low- and intermediate-mass stars experiencing the AGB phase (i.e. the \u2018secondary\u2019 nitrogen production mechanism,","Functions Label":2}
{"Functions Text":"For CC iron meteorites, we examine the isotopic compositions of Mo and Ni, respectively, because these are siderophile elements (so are therefore present in appreciable concentrations in iron meteorites, unlike Ti and Cr) whose compositions have also been relatively well studied in a number of iron meteorites as well as chondrites and their components","Functions Label":3}
{"Functions Text":"We predict the noise in the Planck lensing map assuming the detector sensitivity and beam sizes listed in the Planck Bluebook","Functions Label":2}
{"Functions Text":"The FNm can be written explicitly as an integral over the eccentric anomaly","Functions Label":2}
{"Functions Text":"F_{Nm} = \\frac{1}{\\pi }\\int \\limits _{0}^{\\pi } \\frac{\\cos \\left[N\\left(E - e\\sin E\\right) - mf(E)\\right]}{\\left(1 - e\\cos E\\right)^2}\\,\\,\\mathrm{d}E.","Functions Label":2}
{"Functions Text":"The second issue is the pseudo- versus classical bulge argument \u2013 the model we use assumes an inner classical spherical bulge; bulges instead may be pseudo-bulges, which may not have a spherical shape, and profile well-described by a spherical Hernquist profile","Functions Label":1}
{"Functions Text":"In fact, it is commonly believed that dynamical interactions in GCs facilitate the formation of close binary systems and exotic objects such as cataclysmic variables (CVs), low-mass X-ray binaries (LMXBs), millisecond pulsars (MSPs), and blue straggler stars (BSSs) (e.g.,","Functions Label":0}
{"Functions Text":"The luminosity during the 2020 giant outburst reached a record high, which was significantly higher than the critical luminosity","Functions Label":0}
{"Functions Text":"Lastly, the results from this approach critically depend on the choice of low-b cutoff fitting techniques, where different techniques might result in inconsistent T0 and \u03b3 measurements","Functions Label":0}
{"Functions Text":"Cepheids have also been found to show additional complications that include cycle-to-cycle variations in their light and radial velocity curves (see","Functions Label":3}
{"Functions Text":"It is of importance to planned future surveys to investigate suitable strategies for source-finding in linear polarization with interferometers such as LOFAR,","Functions Label":0}
{"Functions Text":"and with the ability to make precise Faraday rotation measurements","Functions Label":0}
{"Functions Text":"Specifically, we use m* values computed from Bruzual & Charlot (2003) models in the same fashion as described in previous SPT publications","Functions Label":5}
{"Functions Text":"The warm Neptune GJ436b, which is the lowest mass planet found evaporating to date","Functions Label":0}
{"Functions Text":"), shows transit absorption depths up to 60% in the Ly-\u03b1 line.","Functions Label":0}
{"Functions Text":"Semi-analytic modelling is a particular simulation method which is optimized to connect the observed properties of the galaxy population \u2013 abundances, scaling relations, clustering and their evolution with redshift \u2013 to the astrophysical processes that drive the formation and evolution of individual galaxies (e.g.","Functions Label":0}
{"Functions Text":"Minima and transition states (TSs) were optimized using the DL-FIND","Functions Label":2}
{"Functions Text":"program of the ChemShell suite","Functions Label":2}
{"Functions Text":"Over the last few decades, the PTA collaborations have not found GW signals, but the increasingly sensitive data sets offer increasingly stringent constraints on the SGWB","Functions Label":0}
{"Functions Text":"which suggests that at least some FRBs originate from magnetars born from the core collapse of massive stars (e.g.,","Functions Label":3}
{"Functions Text":"Approaches of this type are widely used in astronomy, for example to infer star formation histories or stellar mass distributions from observed colour\u2013magnitude diagrams (CMDs; e.g.","Functions Label":0}
{"Functions Text":"Infalling and rotational motions on scales from 100 to 3000 au have been observed in molecular lines with single-dish telescopes and interferometers","Functions Label":0}
{"Functions Text":"This must typically be done with a numerical Poisson solver","Functions Label":2}
{"Functions Text":"discussed four estimators which attempted to correct for biasing in the degree of linear polarisation in the presence of low signal-to-noise ratios.","Functions Label":0}
{"Functions Text":"Note that the majority of the studies related to the MIR bubbles are mainly carried out for a single H ii region or several H ii regions on scales of a few parsecs (e.g.,","Functions Label":1}
{"Functions Text":"Three events (Swift J1644+57;","Functions Label":1}
{"Functions Text":"have isotropic \u223c5\u2009GHz luminosities of between 1040 and 1042\u2009erg\u2009s\u22121 whereas the rest","Functions Label":1}
{"Functions Text":"have luminosities in the range 1037 to 1039\u2009erg\u2009s\u22121 at similar frequencies. The higher power events are believed to result from observing down the axis of a relativistic jet, resulting in the energy of photons being significantly boosted. Even accounting for boosting, these relativistic events have a higher total energy output than their thermal counterparts.","Functions Label":1}
{"Functions Text":"The sequence of dwarf and giants from","Functions Label":2}
{"Functions Text":"are also overplotted. The three parallel lines are the reddening vectors drawn from the tip of the giant branch (left), from the base of the MS branch (middle)","Functions Label":2}
{"Functions Text":"Given this deficit, we provide only a simplified estimate using radial velocities of OBA-type stars from","Functions Label":2}
{"Functions Text":"Since they belong to the same young population, we assume that they have a similar distance distribution and kinematics as the Cepheids.","Functions Label":1}
{"Functions Text":"The mainstream grains have 12C\/13C ratios between 10 and 100 (solar: 89), and the 14N\/15N ratios of most of them are higher than the solar ratio of 440, the ratio measured for the solar wind","Functions Label":0}
{"Functions Text":"We recall that this relation is valid only under the assumption that the mean star formation activity of the emitting galaxies is constant on a timescale of a few Myr, roughly comparable to the typical time spent by the stellar population responsible for the ionisation of the gas on the main sequence","Functions Label":2}
{"Functions Text":"Velocity fluctuations have been studied thoroughly (see, e.g.,","Functions Label":0}
{"Functions Text":"although the kinetic scales still remain quite unexplored for instrumental limitations, most notably in the sampling time resolution.","Functions Label":7}
{"Functions Text":"Detection of rebrightening during the outburst decay supports the argument that the formation of a compact jet and its interaction with the accretion environment are imprinted on the multiwavelength behaviour of the GBHTs","Functions Label":5}
{"Functions Text":"Orbiting SMBHBs produce a","Functions Label":0}
{"Functions Text":"and transient GW bursts","Functions Label":0}
{"Functions Text":"The relevant methodology is straightforward and well established. One needs to calculate the likelihood function of the data given the model \u2013 namely the probability of the occurrence of the data within the framework of the assumed model","Functions Label":2}
{"Functions Text":"However, an optimal metric \u2013 expressed as an entropy functional \u2013 is not known in advance and therefore needs to be chosen individually","Functions Label":2}
{"Functions Text":"For the SPT-SMGs, we used the sizes of","Functions Label":2}
{"Functions Text":"It was found that if we assume a single H desorption energy in models, the dust temperature range over which efficient H2 formation occurs is narrow (6\u201310 K for olivine grains)","Functions Label":0}
{"Functions Text":"In the magnetically arrested disk","Functions Label":1}
{"Functions Text":"scenario, the MRI and subsequent turbulence in the inner accretion disk are suppressed due to large-scale magnetic flux (see, e.g.,","Functions Label":1}
{"Functions Text":"Plenty of simulation works","Functions Label":0}
{"Functions Text":"have indicated that dissipation, acceleration, and thermalization of turbulent plasmas mainly take place near intermittent structures on kinetic scale, while the actual physical mechanisms behind dissipation remain unclear.","Functions Label":0}
{"Functions Text":"A small number (currently six) of confirmed TDEs, including ASASSN-14li, have also been detected at radio wavelengths and the population may form a bi-modal distribution, consisting of more common non-relativistic \u2018thermal\u2019 events and rarer relativistic jets. Three events (Swift J1644+57","Functions Label":0}
{"Functions Text":"have isotropic \u223c5\u2009GHz luminosities of between 1040 and 1042\u2009erg\u2009s\u22121","Functions Label":0}
{"Functions Text":"The higher power events are believed to result from observing down the axis of a relativistic jet, resulting in the energy of photons being significantly boosted.","Functions Label":0}
{"Functions Text":"On the other hand, long-duration gamma-ray bursts (lGRBs","Functions Label":0}
{"Functions Text":"are associated with the core collapse (CC) of dying massive stars","Functions Label":0}
{"Functions Text":"leading to supernovae (SNe;","Functions Label":0}
{"Functions Text":"Recent advances in understanding the properties of magnetohydrodynamic (MHD) turbulence","Functions Label":3}
{"Functions Text":"stimulate a renewed investigation on density statistics","Functions Label":3}
{"Functions Text":"Many studies of individual galaxies","Functions Label":0}
{"Functions Text":"have shown that the higher J lines of CO arise from warmer, denser gas than the cold gas responsible for the emission of for example CO J = 1\u22120.","Functions Label":0}
{"Functions Text":"The fewer radio studies of RQ AGN","Functions Label":3}
{"Functions Text":"generally lead to mixed results. This encourages to keep investigating it, as it indicates that the origin of the radio emission in RQ AGN is still an open question.","Functions Label":3}
{"Functions Text":"The estimated continuum slope is consistent but somewhat flatter than the typical slope of luminous quasars","Functions Label":1}
{"Functions Text":"The upper atmospheres (above optically thick clouds) of giant exoplanets and those of smaller planets around M stars can be probed using spectroscopy during primary and\/or secondary transits","Functions Label":0}
{"Functions Text":"Recent data from the Gaia mission","Functions Label":3}
{"Functions Text":"and other large-scale surveys, as well as analyses that combine kinematic data with information about chemical abundances and\/or specific stellar populations, have led to discoveries of additional substructures in the Galaxy and brought renewed attention to this topic (e.g.,","Functions Label":3}
{"Functions Text":"The full particle simulations are performed using","Functions Label":2}
{"Functions Text":"and NPIC code","Functions Label":2}
{"Functions Text":"both of which solve Maxwell equations and push particles using relativistic approaches. The VPIC code directly evolves electric and magnetic fields, whereas in the NPIC code the fields are advanced using the scalar and vector potentials.","Functions Label":0}
{"Functions Text":"Although the two codes have very different algorithms, all of the key results are in good agreement for this study, thus providing additional confidence in our conclusions.","Functions Label":5}
{"Functions Text":"Dynamic ocean heat transport on completely ocean-covered worlds (i.e., no continents) leads to warmer global mean temperatures and a reduction in day\u2013night temperature differences on synchronously rotating planets","Functions Label":3}
{"Functions Text":"In future works, our group plans to couple our GCM with a dynamic ocean model to study the interactions between oceans, continents, topography, and observable features.","Functions Label":7}
{"Functions Text":"In the outer regions of a Shakura-Sunyaev disk, the opacity is expected to be mainly due to free-free absorption, while Thomson scattering dominates the opacity in the inner regions of the disk (see Eqs. (2.16) and (2.19) of","Functions Label":2}
{"Functions Text":"The geometrical thickness of the disk scales with the radius R following a (slightly) different relation; it is proportional to R\u221221\/20 in the inner Thomson scattering-dominated, regions and to R\u22129\/8 in the outer regions. At the boundary between these two zones (i.e., at a radius Rjump) a jump is expected. We calculated Rjump according to our results for \u1e40in and assuming the same value for \u03b1 in both equations. We found Rjump between 3\u2005\u00d7\u2005104\u2006RG and 7\u2005\u00d7\u2005104\u2006RG in all the epochs considered.","Functions Label":2}
{"Functions Text":"Consequently, many libraries of limb-darkening coefficients covering a wide range of effective temperatures (Teff), surface gravity (log g), and metal-licities (M\/H) have been produced","Functions Label":0}
{"Functions Text":"using various radiative transfer codes, such as","Functions Label":0}
{"Functions Text":"MARCS","Functions Label":0}
{"Functions Text":"In fact, Sanders (1998) points out that, too close to the MBH, molecular clouds should get disrupted by its gravitational field preventing star formation; even if the Milky Way nucleus features a population of young stars very close to the MBH","Functions Label":0}
{"Functions Text":"supporting instead the idea of possible central star formation, it seems unlikely it can develop such steep profiles.","Functions Label":5}
{"Functions Text":"Traditionally, bulges were thought to invariably form early-on via","Functions Label":0}
{"Functions Text":"or mergers","Functions Label":0}
{"Functions Text":"with the disk gradually building up around them.","Functions Label":0}
{"Functions Text":"Whereas this inside-out galaxy formation scenario appears consistent with important integral characteristics of CBs (e.g., their red colors), it does not offer a plausible explanation for the presence of PBs in present-day LTGs.","Functions Label":1}
{"Functions Text":"In transition regions from diffuse ISM to dense clouds","Functions Label":0}
{"Functions Text":"\\hbox{$0.7 \\leqslant A_{V} \\leqslant 1.2$}0.7 \u2a7d AV\u2a7d 1.2 for the standard ISRF), better shielded from UV photons and where the amount of hydrogen is significantly higher, H-poor carbon can be transformed into H-rich carbon through H atom incorporation, a-C \u2192 a-C:H. Similarly, carbon accreted from the gas phase in these transition regions is likely to be and stay H-rich. Then, in the dense molecular clouds, most of the hydrogen is in molecular form and thus not available to produce a-C:H mantles on the grains.","Functions Label":0}
{"Functions Text":"They exploit the maps with different apertures and efficiencies and are applied individually or combined together, even with different weights (see e.g.","Functions Label":1}
{"Functions Text":"The authors used their new results together with","Functions Label":0}
{"Functions Text":"and low-redshift reference data for the Coma cluster","Functions Label":0}
{"Functions Text":"to further solidify the evidence supporting passive evolution and a formation redshift zform \u2248 2.","Functions Label":0}
{"Functions Text":"According to the theoretical studies, dense cores eventually harbor the first protostellar cores, the first quasi-hydrostatic object during the star formation process (hereafter the first core; e.g.,","Functions Label":0}
{"Functions Text":"which provide the initial condition of star formation.","Functions Label":0}
{"Functions Text":"Such transition might well imply an imminent increase of the SFR, driving the object in the realm of starbursts","Functions Label":1}
{"Functions Text":"or its cessation, bringing the system back onto or even below the main sequence","Functions Label":1}
{"Functions Text":"with the CO properties potentially able to distinguish between these two scenarios.","Functions Label":7}
{"Functions Text":"and the magnetic field can exceed 0.15 T in both the intranetwork and the network quiet region","Functions Label":2}
{"Functions Text":"While the universality of the latter finding is in doubt","Functions Label":3}
{"Functions Text":"it certainly introduces very important subtleties to the old paradigm","Functions Label":3}
{"Functions Text":"The most recent spectroscopic study is from","Functions Label":0}
{"Functions Text":"who reinvestigated the internal rotation measurements and also determined hyperfine coupling parameters due to the nitrogen quadrupole","Functions Label":0}
{"Functions Text":"Gas masses can also be estimated with an empirically calibrated relation between single-band dust continuum flux at the Rayleigh\u2013Jeans (R-J) tail and gas mass (e.g.,","Functions Label":0}
{"Functions Text":"These scaling relations are calibrated with local galaxies or with local galaxies and SMGs up to z \u223c 2. In this method, the gas-to-dust mass ratio is included in the conversion factor, and therefore does not need to be considered.","Functions Label":0}
{"Functions Text":"It remains unclear whether the empirical calibration methods are applicable to galaxies at z > 3 or how much scatter there is in the relationships.","Functions Label":1}
{"Functions Text":"The catalogue explores a wide range of linear diameters and masses, from sub-parsec (\u2264 0.1 pc) to parsec scale (1\u22125 pc) with masses from 1 M\u2299 to 105M\u2299. These wide ranges mean that we probably mix several types of objects, from single star-forming cores to clumps containing multiple cores, even to entire clouds, depending on the distance of object. Most of these sources, however, fulfil the definition of clump, according to the definition of","Functions Label":2}
{"Functions Text":"Compact BH jets show an LX\u2013LR correlation across \u223ceight orders of magnitude in X-ray luminosity","Functions Label":0}
{"Functions Text":"a subset of sources follows a radio-bright correlation with a power-law slope of \u03b2 \u2248 0.6 (where $L_R \\propto L_X^{\\beta }$, while others follow a steeper correlation with \u03b2 \u2273 1 at high X-ray luminosities, before re-joining the other track around LX \u2248 1035 erg\u2009s\u22121 (e.g.","Functions Label":0}
{"Functions Text":"This is not the Kozai\u2013Lidov resonance; in this case, the Kozai\u2013Lidov domain (domain II in","Functions Label":1}
{"Functions Text":"is characterized by libration around $\\omega _{\\rm r}=0{^\\circ }$ (or 180\u00b0) which is only briefly observed at the end of the backwards integrations","Functions Label":1}
{"Functions Text":"see Fig. 6","Functions Label":2}
{"Functions Text":"Out of the recent high-resolution Disk Substructures at High Angular Resolution Project (DSHARP) survey of 20 disks, 3 were found to harbor spirals: Elias 27, WaOph 6, and IM Lup","Functions Label":2}
{"Functions Text":"For example, most existing approaches rely on the adoption of a rigid physical model (e.g. analytic, two-parameter star formation histories combined with a standard dust attenuation curve and the assumption that all stars in a galaxy have the same metallicity) to describe galaxy SEDs (e.g.","Functions Label":0}
{"Functions Text":"this does not allow a physically consistent description of the contributions by stars, gas and dust to the integrated emission from a galaxy, nor the inclusion of a potential AGN component","Functions Label":1}
{"Functions Text":"To illustrate this, we show examples of calibration vectors for SDSS","Functions Label":2}
{"Functions Text":"eBOSS DR14","Functions Label":2}
{"Functions Text":"We also plot the results of previous blank-field surveys","Functions Label":2}
{"Functions Text":"For example, Chen et al. (2016) and","Functions Label":0}
{"Functions Text":"have produced filament catalogues in the SDSS","Functions Label":0}
{"Functions Text":"This \u2018funnel\u2019 accretion scenario is also found in other simulations with a spherical-like distribution of rotationally accreting material","Functions Label":5}
{"Functions Text":"At later times, the spectrum depends on the seed photon spectra, but it can roughly be estimated to be a flat spectrum from \u223c1 eV to \u223c0.1 TeV, while the supernova emission continues, which is expected based on more detailed calculations (e.g.,","Functions Label":2}
{"Functions Text":"This variety can be understood through a detailed radiative transfer calculation, which is analytically solvable only for simple cases (e.g., a static, plane-parallel slab by","Functions Label":0}
{"Functions Text":"Recently, Fern\u00e1ndez-Mart\u00edn et al. (2017) reported a slope of \u22120.108 \u00b1 0.006\u2009dex\u2009kpc\u22121 using optical spectra for H\u2009\u2009ii regions located at RG between 5 and 17\u2009kpc. That value of the slope is considerably much steeper than our determination and other previous estimates from the literature (e.g.","Functions Label":6}
{"Functions Text":"In view of the fact that the limiting magnitude of the follow-up wide-field survey projects is almost \u227221 mag (e.g.,","Functions Label":2}
{"Functions Text":"the maximum detectable distance for BH\u2013NS kilonovae would be \u2272200 Mpc, which can hardly cover the horizon of GW-triggered BH\u2013NS merger events that O3 found (as shown in Figure 10).","Functions Label":2}
{"Functions Text":"Therefore, by restricting attention to data in the distribution outskirts, this approach throws away information and reduces the sensitivity to the IGM thermal state significantly","Functions Label":0}
{"Functions Text":"In the classic study, Hernquist & Ostriker (1992) developed a set of basis functions for density and gravitational potential that can reproduce complex morphology of galaxies with a small number of terms (e.g.,","Functions Label":0}
{"Functions Text":"These expansions reproduce the force field of an N-body simulation with a precision of a few percent, so representing the gravitational potential in our model with an expansion of basis functions is tempting. However, a truly realistic solution needs to accurately capture not only the current structure of the Galaxy but also its evolution in time.","Functions Label":3}
{"Functions Text":"This suggests that low-mass stars mostly contribute to carbon around solar metallicity, whereas at super-solar metallicities, massive stars produce carbon together with oxygen, thereby flattening or even decreasing the [C\/O] ratio. This trend is in agreement with the metallicity dependent yields from","Functions Label":5}
{"Functions Text":"which provide higher carbon as [Fe\/H] increases from massive stars (i.e. also increasing the O production) but lower carbon from low and intermediate mass stars as [Fe\/H] increases (i.e. less production of C).","Functions Label":5}
{"Functions Text":"The dispersion relation of strong electromagnetic waves is altered due to the effective electron mass increased by the relativistic effect (e.g.,","Functions Label":2}
{"Functions Text":"Nevertheless, the debris that remains bound eventually contributes to the accretion flow around the SMBH. This part of the debris stream will finally be circularized by energy dissipation, leading to the formation of a small, initially ring-like, accretion disk around the black hole","Functions Label":0}
{"Functions Text":"It is worth noting that the \u201chead-to-tail\u201d scenario seems to support the idea that the filament is supported by sheared arcades","Functions Label":1}
{"Functions Text":"obtained the twin modes of MHD waves in LMXBs (including NS LMXBs and black hole LMXBs), which are considered as the sources of high-frequency QPOs.","Functions Label":0}
{"Functions Text":"The quantitative estimation of the radiated flare energy partition suggested about","Functions Label":0}
{"Functions Text":"and 55%\u201380% in WL for stellar flares (e.g.,","Functions Label":0}
{"Functions Text":"The nuclear semi-relativistic phase and the galaxy-scale molecular phase have been observed simultaneously in less than a dozen sources, with varied results:","Functions Label":0}
{"Functions Text":"in other cases data suggest momentum driven flows (e.g.","Functions Label":0}
{"Functions Text":"The growth of dust grains through accretion in the ISM has been proposed as a solution (e.g.","Functions Label":0}
{"Functions Text":"but there are doubts on the efficiency of accretion at high z, where high dust temperatures due to the CMB (see Section 3.3) keep the desorption time-scale for accreted materials short","Functions Label":1}
{"Functions Text":"Efforts have been made in quantifying mass, star formation rates, gas composition, and kinematics, as well as other LAE properties (e.g.,","Functions Label":0}
{"Functions Text":"This high AGN fraction detected so far, ~23%, makes the overdensity around 7C 1756+6520 similar to the interesting and well-studied cluster around the radio galaxy PKS 1138\u2212262 from this point of view as well","Functions Label":3}
{"Functions Text":"As a result, optical studies have produced the largest number (\u223c1200) of new extra-Magellanic SNR candidates. Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S\u2009ii]\/H\u2009\u03b1 > 0.4\u20130.5","Functions Label":0}
{"Functions Text":"This calibration is relatively insensitive to changes in gas pressure or ionization parameter, and we adopted it as fiducial approach in this paper (see","Functions Label":0}
{"Functions Text":", for a discussion).","Functions Label":0}
{"Functions Text":"Of course, care has to be taken to avoid combinations of biosignature molecules which can be generated abiotically together (see e.g.","Functions Label":0}
{"Functions Text":"short-term Fourier transform","Functions Label":0}
{"Functions Text":"are methods to infer DR.","Functions Label":0}
{"Functions Text":"It is also a great advantage to directly compare the distributions of molecular gas observed by ALMA and positions of massive YSOs identified by Spitzer and Herschel (e.g.,","Functions Label":1}
{"Functions Text":"without any serious contamination in the line of sight.","Functions Label":1}
{"Functions Text":"Hence, we think that the radio jet is transferring its energy and momentum to the ambient medium through an extended shock front, which creates turbulence in a dense clumpy ISM. Such a great impact of the radio jet has been observationally shown in many cases","Functions Label":1}
{"Functions Text":"and theoretically supported through detailed hydrodynamic simulations (e.g.","Functions Label":1}
{"Functions Text":"Events that took place in the far past are expected to have induced a thickening of the early Galactic disc, first by increasing the in-plane and vertical velocity dispersion of stars","Functions Label":0}
{"Functions Text":"The 70 \u03bcm band luminosities (from","Functions Label":0}
{"Functions Text":"is a good example of such a huge scatter in the FIR luminosity of elliptical galaxies.","Functions Label":0}
{"Functions Text":"The spectral synthesis match was performed using the Stellar Parameters Classification tool (SPC,","Functions Label":2}
{"Functions Text":"It determines effective temperature, surface gravity, metallicity, and line broadening by performing a cross-correlation of the observed spectra with a library of synthetic spectra, and interpolating the correlation peaks to determine the best-matching parameters.","Functions Label":2}
{"Functions Text":"Our Galaxy, however, contributes","Functions Label":2}
{"Functions Text":"from its interstellar medium and a presumed ${\\rm DM}_{\\rm Halo}\\sim 50 \\, {\\rm pc \\, cm^{-3}}$ from its halo","Functions Label":2}
{"Functions Text":"On the one hand, it is more energetically favorable for the system to populate new degrees of freedom, such as hyperons","Functions Label":3}
{"Functions Text":"For a cosmic void, embedding requires the underdense interior to be \u201ccompensated\u201d by an overdense bounding ridge, i.e., a compensated void","Functions Label":0}
{"Functions Text":"Secondly, there are three different KL mechanisms competing, thus the eccentricity of the inner binary of the CO triple can be pumped up by the torque either of the SMBH or the third companion in the CO triple, for which the KL time-scale is shorter (e.g.","Functions Label":2}
{"Functions Text":"A soft excess below 1.5 keV is also present","Functions Label":0}
{"Functions Text":"In all four cases of different initial amplitude, \u03c1IA, the phase speed decreases slighty (consistent with observations; see","Functions Label":5}
{"Functions Text":"In the microquasar Cygnus X-1, radio emission has been measured with a flat spectrum, i.e. \u03b1 = \u22120.06 \u00b1 0.05 and \u03b1 = 0.07 \u00b1 0.04","Functions Label":5}
{"Functions Text":"Larger data sets of star-forming clumps, identified as gaseous protoclusters, also exhibit a mass-size relation.","Functions Label":1}
{"Functions Text":"compiled the observations of Shirley et al. (2003), Fa\u00fandez et al. (2004), and Fontani et al. (2005) in their Fig. 1, and found via least-squares regression the relation R \u221d M0.38.","Functions Label":1}
{"Functions Text":"Meanwhile, both studies exhibit mass scatter of about 1 dex and are compatible with constant gas surface density, that is, R \u221d M0.5.","Functions Label":1}
{"Functions Text":"Other examples of AGN with at least two variable phases of the X-ray winds are","Functions Label":0}
{"Functions Text":"IRAS 17020+4544","Functions Label":0}
{"Functions Text":"Previous studies include","Functions Label":0}
{"Functions Text":"and magnetohydrodynamic (MHD) shocks","Functions Label":0}
{"Functions Text":"magnetic helicity flux from anisotropy of the turbulence produced by differential rotation","Functions Label":0}
{"Functions Text":"USSRH are a prediction of turbulent re-acceleration models","Functions Label":0}
{"Functions Text":"However, about half of our most massive clumps migrate radially outwards.","Functions Label":1}
{"Functions Text":"but requires either large torques or steep surface density gradients","Functions Label":1}
{"Functions Text":"Nevertheless, Swift J1834.9\u22120846 has some interesting characteristics that are not shared with the entire magnetar population. First, the environment of Swift J1834.9\u22120846 is extremely crowded, with a Fermi GeV source, an H.E.S.S. TeV source, an SNR, a GMC, and an OH maser in its vicinity","Functions Label":1}
{"Functions Text":"There are two main formation channels that are thought to compete in NSC formation:","Functions Label":0}
{"Functions Text":"or via orbital segregation and merger of massive star clusters that migrate towards the galactic centre via dynamical friction","Functions Label":0}
{"Functions Text":"The explosions, however, leave imprints in the interstellar medium that can remain visible at radio wavelengths for 10\u2005\u2212\u2005100 kyr","Functions Label":0}
{"Functions Text":"thereby allowing the association of pulsars with supernova remnants (SNRs).","Functions Label":0}
{"Functions Text":"It is thus worthwhile to investigate whether new physics might solve or at least alleviate the S8 discrepancy, a possibility that has been investigated in several works.","Functions Label":3}
{"Functions Text":"Models that have been contemplated in this sense include for example","Functions Label":0}
{"Functions Text":"extended or exotic DM and\/or dark energy (DE) models and interactions","Functions Label":0}
{"Functions Text":"As a result, two main accretion regimes, super- and subcritical accretion, are expected depending on whether the source luminosity is higher or lower than a \u201ccritical luminosity\u201d Lcrit, which strongly depends on the magnetic field of the NS","Functions Label":0}
{"Functions Text":"Unfortunately, in the case of the M\u200981 Group, this technique appears hardly applicable since the radial velocities of extragalactic and Galactic clouds share a similar LSR (local standard of rest) velocity range","Functions Label":1}
{"Functions Text":"The fast solar winds emanate from coronal holes at higher heliolatitudes","Functions Label":2}
{"Functions Text":"Aside from the histograms, we add a kernel smoothed curve, shown as shaded area, which is derived directly from the data set using an Epanechnikov Kernel Density estimator","Functions Label":2}
{"Functions Text":"with a bandwidth equal to 1.5 times the bin size.","Functions Label":2}
{"Functions Text":"Among the fibers, f1 is clearly tracing the central-densest part of the dust ridge well known from previous dust-continuum observations","Functions Label":2}
{"Functions Text":"For example, in studies of the evolution of MBHBs in circumnuclear discs, a modulated gas inflow from the outer gas distribution periodically fuels the accretion discs within the Hill radii of the individual MBHs (that, being smaller than the surrounding circumbinary disc, are commonly referred to as \u2018mini-discs\u2019 in the literature,","Functions Label":0}
{"Functions Text":"as a consequence of the non-axisymmetric and time-dependent potential of the binary.","Functions Label":0}
{"Functions Text":"For instance, it is well known that there is a persistent discrepancy between the Planck CMB measurements of H0 and the local measurements based on distance ladder","Functions Label":3}
{"Functions Text":"The values of the para-H2CO column density were obtained with APEX data (beam size ~30\u2033;","Functions Label":2}
{"Functions Text":"AGNs with predominant radio emission from jet deviate from radio\u2013IR correlation by showing radio-excess","Functions Label":2}
{"Functions Text":"Therefore, we examine if our NLS1s show radio-excess in the radio\u2013IR correlation.","Functions Label":2}
{"Functions Text":"For an analytical expression of the poloidal magnetic field, we follow the practice of","Functions Label":2}
{"Functions Text":"in which poloidal field is given in terms of the vector potential as in (8)\\begin{equation} B_{p}=-\\frac{\\partial A_{t}}{\\partial x}\\frac{\\vec{r}_{\\perp}}{r_{\\perp}}+\\left(\\frac{\\partial A_t}{\\partial r_{\\perp}}+\\frac{A_t}{r_{\\perp}}\\right)\\vec{x}. \\end{equation}Bp=\u2212\u2202At\u2202xr\u22a5r\u22a5+\u2202At\u2202r\u22a5+Atr\u22a5x.","Functions Label":2}
{"Functions Text":"Various values of \u03b2 in MCs have been derived by several authors, ranging from \u03b2\u2004\u223c\u20040.38","Functions Label":1}
{"Functions Text":"to \u03b2\u2004=\u20040.6\u2005\u00b1\u20050.3","Functions Label":1}
{"Functions Text":"More interestingly, there are hints suggesting that the impacts of projection effects extend beyond richness misidentification.","Functions Label":3}
{"Functions Text":"Secondly, when More et al. (2016) reported a detection of the so-called \u2018splashback\u2019 radius, a physically motivated boundary of cluster haloes, for redMaPPer clusters, the location of the splashback radius was found to be smaller than theoretical expectations (also see","Functions Label":3}
{"Functions Text":"for a similar detection).","Functions Label":3}
{"Functions Text":"Aperture photometry was performed with the DAOPHOT","Functions Label":2}
{"Functions Text":"package","Functions Label":2}
{"Functions Text":"Nevertheless, early attempts (e.g.,","Functions Label":0}
{"Functions Text":"that were made to study the impact of global magnetic fields (Lorentz-stress perturbations) on the eigenfrequencies and eigenfunctions of the standard solar model (model S in Christensen-Dalsgaard et al. 1996) focused on the details of the forward problem of frequency shifts induced by an axisymmetric magnetic field not aligned with the rotation axis.","Functions Label":0}
{"Functions Text":"For this work, we used two reference spectra:","Functions Label":2}
{"Functions Text":"and the spectrum of NGC\u20094387","Functions Label":2}
{"Functions Text":"an elliptical galaxy showing strong absorptions.","Functions Label":2}
{"Functions Text":"It has been classified as having a cometary-like morphology with an integrated subsolar metallicity of 12 + log(O\/H) = 7.73\u20137.78","Functions Label":0}
{"Functions Text":"Secondly, the propagation of LyC photons within the ISM is favoured by a negligible amount of dust and low column density of HI (N(HI) \u2264 1018 cm-2) in a 10-pc scale region around the emitting star clusters. This could be the case for galaxies embedded in dark-matter halos with masses less than 108 M\u2299","Functions Label":0}
{"Functions Text":"Subsequently,","Functions Label":1}
{"Functions Text":"measured chemical abundances of six stars in Gaia 1, suggesting an equally high metallicity, but based on their abundance study, the suggestion of an extragalactic origin was revoked.","Functions Label":1}
{"Functions Text":"While a more metal-rich nature found by the latter authors conformed with the results by Simpson et al. (2017), the evolutionary diagrams of both studies are very dissimilar and could not be explained by one simple isochrone fit.","Functions Label":1}
{"Functions Text":"On the other hand, many fewer studies, all recent, were devoted to the full mass spectrum, using optical photometry","Functions Label":0}
{"Functions Text":"The magnetic fields in the low solar atmosphere could be very strong","Functions Label":2}
{"Functions Text":"Mid-IR (MIR) and far-IR (FIR) observations have revealed bright atomic lines from H\u2009ii regions ([S\u2009iii], [Ne\u2009iii], [Ne\u2009ii], [O\u2009iii], etc.) and PDRs ([C\u2009ii], [O\u2009i]) (e.g.,","Functions Label":0}
{"Functions Text":"It is important to do so because different processes, e.g.","Functions Label":3}
{"Functions Text":"pristine accretion","Functions Label":3}
{"Functions Text":"are surely contributing to the same system","Functions Label":3}
{"Functions Text":"Works by other authors seem to support the idea that power-law beam electrons may precipitate throughout the entire flaring atmosphere down to the photosphere","Functions Label":1}
{"Functions Text":", causing its heating via inelastic collisions with the ambient plasma via a hydrodynamic response","Functions Label":1}
{"Functions Text":"and a comparison with the other EoSs of the BSk family","Functions Label":7}
{"Functions Text":"shall be left for future study.","Functions Label":7}
{"Functions Text":"This is perhaps a much too slow to account for the strong equipartition strength magnetic fields observed in the high-redshift galaxies with z > 1 (e.g.","Functions Label":3}
{"Functions Text":"or even for that in the slowly rotating nearby galaxies. This discrepancy leads one to invoke some additional mechanism such as cosmic rays (CRs) boosting the typical dynamo action.","Functions Label":3}
{"Functions Text":"Since the star-formation histories of galaxies (ETGs included, e.g.","Functions Label":2}
{"Functions Text":"can be stochastic and include multiple bursts, we also verify the full-spectrum fitting capabilities to retrieve more complex SFHs.","Functions Label":2}
{"Functions Text":"Current cosmological hydrodynamic simulations of galaxy formation employ a variety of subgrid models (e.g.","Functions Label":0}
{"Functions Text":"that artificially launch galactic winds, but the results are sensitive to numerical resolution and the exact subgrid model employed","Functions Label":0}
{"Functions Text":"The physical properties of SMGs derived from detailed studies of individual sources and large sky area submillimetre surveys suggest that SMGs represent an early evolutionary phase of all local ellipticals","Functions Label":0}
{"Functions Text":"The high-twist region in our result is also in agreement with the","Functions Label":5}
{"Functions Text":"and the location of the flare ribbons","Functions Label":5}
{"Functions Text":"We scan each trial of data and the on-source window in the 30\u20131000 Hz frequency band using a predefined bank of waveform templates","Functions Label":2}
{"Functions Text":"Previous studies of intermediate-age star clusters with eMSTOs usually showed tight SGBs throughout","Functions Label":6}
{"Functions Text":"but see","Functions Label":6}
{"Functions Text":"Nevertheless, with the arrival of more powerful supercomputers, other authors have used instead global 3D MHD simulations to model DR and stellar magnetism in the convection zone of solar-like stars","Functions Label":0}
{"Functions Text":"where P0, T0, and \u039b values are listed in Table 1, s is the depth from the nucleus surface, $f(s) = 1 - (1 - {s \\over R})^4$ for s \u2264 R, f(s) = 1 elsewhere, r \u2248 50 nm and R \u2248 5 mm are the radii of the grains of which cometary dust consists","Functions Label":2}
{"Functions Text":"and of the pebbles of which cometary nuclei","Functions Label":2}
{"Functions Text":"Three-dimensional simulations that include all three non-ideal MHD effects are also performed","Functions Label":0}
{"Functions Text":"To also cover lower luminosity galaxies, as the GOALS sample only includes luminous IR galaxies (LIRGs) and ultra-luminous IR galaxies (ULIRGs), we included 38 galaxies from Bernard-Salas et al. (2009) and","Functions Label":2}
{"Functions Text":"to reach the total sample of 196 galaxies with IR line fluxes in the 5.5\u2005\u2212\u200535\u2006\u03bcm interval in which an AGN component is not detected.","Functions Label":2}
{"Functions Text":"It has been shown that shocks at the self-intersection point is the main cause of orbital energy dissipation and the subsequent formation of an accretion disc","Functions Label":0}
{"Functions Text":"While both codes are public, we understand that this approach is not yet ubiquitous in the field of galaxy-scale strong lensing (for instance, it has been difficult thus far to reproduce\/check the results of","Functions Label":6}
{"Functions Text":"and Hezaveh et al. 2016), but we hope that our work can help make substructure lensing more reproducible.","Functions Label":6}
{"Functions Text":"In the regions we investigated, the Hapi region displays the lowest spectral slopes 8\u201311%\/100 nm (see also","Functions Label":1}
{"Functions Text":"together with the isolated bright features (IBFs) and the clustered bright features in the Imhotep region.","Functions Label":1}
{"Functions Text":"We introduce a method to search for signatures of DM annihilation from a Galactic subhalo population using the non-Poissonian template fitting (NPTF) framework","Functions Label":2}
{"Functions Text":"Our model consists of four zones; an inner disk (zone 1, as in","Functions Label":2}
{"Functions Text":"Several predictions for planet(s) shaping the disk of SAO 206462 have been proposed","Functions Label":0}
{"Functions Text":"The lack of close-in giant planets may also be explained by the intrinsically different planetary formation for these intermediate-mass stars (see the discussion in","Functions Label":1}
{"Functions Text":"Uncertainties in stellar radius estimates from photometric Kepler observations prevented a detailed assessment of the intrinsic planet size distribution","Functions Label":0}
{"Functions Text":"The calculations of LS","Functions Label":0}
{"Functions Text":"are the two EoS tables in more widespread use for astrophysical simulations.","Functions Label":0}
{"Functions Text":"varying within an order of magnitude over decades of observations","Functions Label":0}
{"Functions Text":"The [C II]\u2013FIR luminosity ratios of these quasar hosts range from 10\u22124 to a few \u00d710\u22123","Functions Label":1}
{"Functions Text":"following the trend of decreasing [C II]\u2013FIR ratio with increasing FIR luminosities found with the IR luminous star-forming systems","Functions Label":1}
{"Functions Text":"The column density is estimated from the fitted line profile by assuming local thermodynamic equilibrium (LTE)","Functions Label":2}
{"Functions Text":"In Equation (3), \u0394E denotes the width of the respective energy bin; for the typical radial velocity of solar wind in the flanks and the downwind hemisphere of the inner heliosheath, we assumed uR = 140 km s\u22121 as measured by Voyager 2, whereas uR = 40 km s\u22121 for the heliosheath in the Voyager 1 direction","Functions Label":2}
{"Functions Text":"In low-density regions (according to","Functions Label":0}
{"Functions Text":"\\hbox{$A_{V} \\leqslant 0.7$}AV\u2a7d 0.7 for the standard ISRF), UV photons are responsible for causing the photo-dissociation of CH bonds, a-C:H \u2192 a-C.","Functions Label":0}
{"Functions Text":"However, Ly\u03b1 emission is known to be extended beyond the continuum","Functions Label":1}
{"Functions Text":"and fluxes based on the TDOSE spectra would therefore be biased.","Functions Label":1}
{"Functions Text":"Methanethiol (or methyl mercaptan, CH3SH) was detected in the Sagittarius B2 (Sgr B2) region of the center of our Galaxy","Functions Label":0}
{"Functions Text":"In some cases, twisted magnetic flux tubes appear close enough to flow vortices, leading to magnetic and kinetic vortex structures closely coexisting in regions with high plasma-\u03b2","Functions Label":0}
{"Functions Text":"In the FS (BS), the 2D velocity map between the current and the previous (next) frame is constructed with almost the same method as","Functions Label":2}
{"Functions Text":"In the solar system, superrotation exists in the atmospheres of Venus, Titan, Saturn, and Jupiter, as well as the stratospheric atmosphere of Earth during the westerly phase of the quasi-biennial oscillation (e.g.,","Functions Label":0}
{"Functions Text":"Some of the gas accreting onto a dark matter halo is expected to penetrate surrounding hot gas in a form of filaments of dense and cold infalling gas and directly accrete onto the central galaxy at such high redshift, where the mass accretion rate and matter density tend to be high. Such direct gas supply through the filaments of cold gas could make the gas disk of the central galaxy more turbulent and gravitationally unstable, which leads to thick and clumpy stellar disk and bulge formation\/growth in some cases (e.g.,","Functions Label":1}
{"Functions Text":"Moreover, to account for the broad emission line found required by the 2003 data, we added a Gaussian component whose width was kept fixed to \u03c3 = 400 eV, in accordance with what literature papers (e.g.","Functions Label":2}
{"Functions Text":"To understand NSC formation, it is therefore critical to be able to disentangle such degeneracies. For example, follow-up spectroscopic observations aiming at decomposing the main stellar populations and the dynamical imprint of a MBH rely on a good mass model to predict the stellar population velocity profile (e.g.","Functions Label":3}
{"Functions Text":"Therefore, methods with more advanced mathematical algorithms were introduced.","Functions Label":0}
{"Functions Text":"Coronal Hole Identification via Multi-thermal Emission Recognition Algorithm (CHIMERA)","Functions Label":0}
{"Functions Text":"have been found to be very effective and are widely used in online solar data visualization tools1$^,$\u2009.2","Functions Label":0}
{"Functions Text":"Narrow-band imaging can efficiently detect LAHs at targeted redshifts through stacking","Functions Label":0}
{"Functions Text":"and narrow-band surveys enable ultradeep, blind samples of LAHs around distant galaxies","Functions Label":0}
{"Functions Text":"Examples of r-process sites that have been proposed and investigated by theoretical studies include (i) neutrino-driven winds from proto-neutron stars (NSs;","Functions Label":0}
{"Functions Text":"In fact, a variety of orientations have previously been observed, and the alignment of filaments and apparent field direction appear to vary between regions and for different gas densities (cf.,","Functions Label":0}
{"Functions Text":"for a review)","Functions Label":0}
{"Functions Text":"During the past two decades, several Type IIb SNe with such interesting features have been monitored and studied well, e.g.,","Functions Label":0}
{"Functions Text":"SN 2011fu","Functions Label":0}
{"Functions Text":"Although shown to be too simplistic by the first X-ray studies of clusters","Functions Label":1}
{"Functions Text":"the self-similar relations allow us to investigate if astrophysical processes are less significant in more massive clusters or at higher redshift.","Functions Label":1}
{"Functions Text":"Further observations revealed a transition in average densities at planet sizes \u223c1.5 R\u2295","Functions Label":0}
{"Functions Text":"with smaller planets having densities consistent with rocky compositions while larger planets having lower densities indicating significant H\/He envelopes.","Functions Label":0}
{"Functions Text":"The colour information is considered an important feature to find lenses (see e.g.","Functions Label":2}
{"Functions Text":"The use of colour queries is considered at least an interesting way to make a pre-selection and improve the final deep learning result purity.","Functions Label":2}
{"Functions Text":"At redshifts above z \u00e2\u0088\u00bc 1, it is nearly impossible to detect weak auroral lines for directly determining metallicity (but see","Functions Label":1}
{"Functions Text":"Therefore, GRB afterglows are good probes of burst environment and the interstellar dust and gas in distant, star-forming galaxies","Functions Label":3}
{"Functions Text":"At the same time, gas accretion rates were maximal","Functions Label":0}
{"Functions Text":"Several mechanisms have been suggested that control the efficiency of mass transfer, mass accretion, and mass loss, including the existence of an accretion disk that regulates the amount of mass and angular momentum that can be accreted","Functions Label":3}
{"Functions Text":"In this work, we only focus on the very bright objects, i.e. ${\\gt}10^{45}\\, \\rm erg\\,s^{-1}$, avoiding the comparison with lower luminosity given the current limitations on observational and theoretical models. In particular, from an observational standpoint, the covered area and depth of current surveys pose serious challenges when extracting statistical properties of the LF at the faint end","Functions Label":1}
{"Functions Text":"We use a constant SPH artificial viscosity coefficient \u03b1SPH \u2248 0.55 such that the corresponding disc viscosity coefficient","Functions Label":2}
{"Functions Text":"is \u03b1d = 0.01 at the inner radius.","Functions Label":2}
{"Functions Text":"These speeds far exceed the few km s\u22121 planet-frame velocities detected on other planets","Functions Label":1}
{"Functions Text":"The currently accepted distance of NGC 6231 is approximately 1580 pc, and its age is between 2and 8 Myr, with a significant intrinsic spread","Functions Label":0}
{"Functions Text":"These included","Functions Label":0}
{"Functions Text":"and short-duration GRBs (likely caused by the coalescence of two neutron stars or a neutron star and black hole, which lasts for less than 2\u2009s;","Functions Label":0}
{"Functions Text":"More recently, data from the Spectral and Photometric Imaging Receiver (SPIRE) instrument onboard Herschel ESA space observatory and Multiband Imaging Photometer for Spitzer (MIPS) onboard Spitzer allowed the identification of several dust clouds north of the M\u200981 galaxy with a total hydrogen column density in the range 1.5\u20135 \u00d7 1020 cm-2 and dust temperatures between 13 and 17 K","Functions Label":0}
{"Functions Text":"However, since there is no obvious difference among the individual clouds, there was no way to distinguish between Galactic or extragalactic origin although it is likely that some of the IR emission both toward M\u200981 and NGC 3077 is of Galactic origin.","Functions Label":1}
{"Functions Text":"several exhibit spiral arm morphologies","Functions Label":0}
{"Functions Text":"98 clusters are identified by the South Pole Telescope (SPT;","Functions Label":2}
{"Functions Text":"but are not included in the Planck PSZ2 catalogue.","Functions Label":6}
{"Functions Text":"The most stringent and precise constraints on the self-interaction cross-section have been put on the scales of galaxy clusters (e.g.","Functions Label":0}
{"Functions Text":"where observations require that $\\sigma _T\/m_chi \\lesssim 1\\, {\\rm cm^2g^{-1}}$.","Functions Label":0}
{"Functions Text":"This process may provide an explanation for the observed braking indices of young pulsars with n \u2260 3","Functions Label":1}
{"Functions Text":"in contrast to the prediction of a rotating magnetic dipole in vacuum","Functions Label":1}
{"Functions Text":"Observing stellar halos in integrated light is, in principle, more easily scalable to the sample sizes needed to explore the wide variation in the accreted component that is predicted by simulations (e.g.,","Functions Label":3}
{"Functions Text":"One reason why we may not detect many dusty reds as jellyfish galaxies might be due to the fact that these galaxies, despite having relatively high SFRs (only four times lower than that in blue spirals at fixed mass,","Functions Label":2}
{"Functions Text":"However, this does not explain the discrepancy with","Functions Label":1}
{"Functions Text":"who also used magnesium.","Functions Label":1}
{"Functions Text":"The detailed mechanistic route for the interstellar synthesis of MF is a subject of considerable debate","Functions Label":0}
{"Functions Text":"These physical conditions are consistent with what is found for Mrk 231","Functions Label":5}
{"Functions Text":"We then included an absorption component and fixed the photon index to 1.8, as expected for the intrinsic AGN emission (e.g.,","Functions Label":2}
{"Functions Text":"For internal consistency, all EWs in this work have been adjusted to the measurement scale of","Functions Label":2}
{"Functions Text":"If the core does collapse, the explosion proceeds via delayed explosion on short timescales","Functions Label":1}
{"Functions Text":"and 2D simulations suggest the explosion occurs before significant convection has had time to develop","Functions Label":1}
{"Functions Text":"and hence a symmetric explosion results.","Functions Label":1}
{"Functions Text":"While the velocity field is very regular, the velocity dispersion looks more complex. Instead of one peak extended along a southeast-northwest axis (Figs. 10, and 11), we find three (Fig. 13). The central one, elongated along the main axis of the galaxy and not perpendicular to it, is accompanied by two additional regions with wider lines to the northeast and southwest, separated by a total of 5.\u2032\u2032 9 \u00b1 0.\u2032\u20322. At these locations we observe the transition between rigid body rotation and steep rotation curve to a flat one (see also","Functions Label":5}
{"Functions Text":"As mentioned before, we conclude that strong bars drive the trends of bar fraction with (g \u2212r) colour, stellar mass, and SFR observed in other studies","Functions Label":4}
{"Functions Text":"A key question that remains unanswered is how BBHs are formed. Viable formation channels include","Functions Label":0}
{"Functions Text":"and dynamical encounters in dense stellar environments, such as globular clusters (e.g.,","Functions Label":0}
{"Functions Text":"The existence of relations between SFR and galaxy stellar mass (SFR\u2013Mass) and specific star formation rate and mass (sSFR = SFR\/Mass) have been established from z = 0 out to z > 2","Functions Label":0}
{"Functions Text":"Therefore the amplitudes estimated in","Functions Label":2}
{"Functions Text":"listed in Table 1, are used in this work as fixed values.","Functions Label":2}
{"Functions Text":"A second explanation is related to the stability of H-rich carbon in the ISM, which depends strongly on the radiation field intensity to local density ratio","Functions Label":0}
{"Functions Text":"We followed the implication of this approach described in","Functions Label":2}
{"Functions Text":"and refer the reader to that work for more details.","Functions Label":2}
{"Functions Text":"As for Earth, modeling of exoplanet atmospheres requires as fundamental input the spectral energy distribution of the hosting star, especially UV and shorter wavelengths (e.g.,","Functions Label":0}
{"Functions Text":"The radio to X-ray spectrum of the forward shock afterglow emission of GW170817\/GRB 170817A is f\u03bd \u221d \u03bd\u22120.6, which yields a p = 2.2 in the slow-cooling synchrotron radiation scenario","Functions Label":2}
{"Functions Text":"while a portion of the Compton component will escape to reach an observer, the remains (refer as ${\\tt{\\rm simplc}}$,","Functions Label":2}
{"Functions Text":"will strike back to the disc to generate the reflected component.","Functions Label":2}
{"Functions Text":"When the fastest layers catch up with the slowest, the charged particles contained in the layers are accelerated through mildly relativistic collisionless shocks (internal shocks;","Functions Label":0}
{"Functions Text":"Previous observations show that para-H2CO (3\u20132) is sensitive to gas temperature at density 105 cm\u22123","Functions Label":2}
{"Functions Text":"The main conclusion in all these studies is that a [C\u2009ii] deficit exists at high redshift, most likely due to the starbursting nature of these galaxies rather than their metallicity, since most of these systems are close to solar (see, e.g.","Functions Label":1}
{"Functions Text":"In principle, an increase in accretion rate would be expected to result in an increase in the scale height of the funnel (e.g.","Functions Label":3}
{"Functions Text":"However, while this must happen over some range of $\\dot{M}$ in order for the disc structure to transition from the thin disc expected for standard sub-Eddington accretion to the funnel-like geometry expected for super-Eddington accretion, as discussed by Lasota et al. (2016), once the disc reaches the point of being fully advection-dominated the opening angle of the disc should tend to a constant (H\/R \u223c 1, where H is the scale height of the disc at radius R).","Functions Label":3}
{"Functions Text":"Supervised learning has been used to","Functions Label":0}
{"Functions Text":"and to determine the redshift of galaxies","Functions Label":0}
{"Functions Text":"In the optically thin limit, the emission is significantly polarized","Functions Label":0}
{"Functions Text":", an effect that has been observed in higher-luminosity AGN sources","Functions Label":0}
{"Functions Text":"To take an even more practical approach, we chose a normalized color parameter based on the Spitzer Infrared Array Camera","Functions Label":2}
{"Functions Text":"as a commonly used photometer for the observation of exoplanets (see, e.g.,","Functions Label":2}
{"Functions Text":"This limit is referred to as the quasi-static approximation to MHD","Functions Label":0}
{"Functions Text":"although recent numerical studies on its turbulent properties and anisotropy have been done as well","Functions Label":0}
{"Functions Text":"Downward field-aligned current is connected to the dawnside ionosphere, and upward field-aligned current is connected to the duskside ionosphere. The pair of field-aligned currents causes magnetic disturbances at mid- and low- latitudes","Functions Label":2}
{"Functions Text":"Combined with the red clump sample of","Functions Label":1}
{"Functions Text":"stars in different evolutionary states in Gaia 1 are progressively being sampled.","Functions Label":1}
{"Functions Text":"This provides a natural route for forming GRBs in low-metallicity environments, as found for most GRB hosts","Functions Label":1}
{"Functions Text":"A detailed theoretical model for gamma-rays from the collision of cosmic ray with the solar atmosphere was presented by","Functions Label":0}
{"Functions Text":"The predicted gamma-ray flux at energies from 10 MeV to 10 GeV has a large uncertainty, being sensitive to the assumptions about the cosmic-ray transport in the magnetic field near the Sun.","Functions Label":0}
{"Functions Text":"Here, \u03c4\u03b3, \u03bd is the optical depth of the ejecta to \u03b3-rays and K\u03b3, \u03bd is the photon inelasticity at a given frequency, where the Klein\u2013Nishina cross section and the cross section for the Bethe\u2013Heitler pair production in the field of a carbon nucleus are taken into account","Functions Label":2}
{"Functions Text":"One possible reaction pathway begins with electron ionization of H2, followed by exothermic proton transfer reactions to form H+MF and subsequent three-body association to generate H+MF-Ln clusters","Functions Label":1}
{"Functions Text":"These methods include:","Functions Label":0}
{"Functions Text":"empirical relations to derive stellar mass in the form of mass-luminosity relations","Functions Label":0}
{"Functions Text":"It has been found that alkali atoms are present in cool brown dwarf atmospheres, indicating that silicate rainout may occur in these objects","Functions Label":3}
{"Functions Text":"There is evidence for radio emission spread over the host galaxy scale for a number of Seyferts when observed with adequate angular resolution and sensitivity","Functions Label":0}
{"Functions Text":"In this case, bodies that formed inward of the snowline (Io) accreted from essentially water-poor building blocks, whereas bodies that formed outward of the snowline (Ganymede, Callisto) formed from a primordial mixture of water ice and silicates (e.g.,","Functions Label":0}
{"Functions Text":"Within this scenario, the low water content of Europa is puzzling.","Functions Label":6}
{"Functions Text":"whereas the more accurate ExoMol POKAZATEL line list","Functions Label":0}
{"Functions Text":"is complete up to 4000 K.","Functions Label":0}
{"Functions Text":"Finally, based on the CASSCF wave functions, the internally contracted multi-reference configuration interaction method with the Davidson correction (icMRCI+Q)","Functions Label":2}
{"Functions Text":"is performed to consider the dynamic correlation and size-consistency error.","Functions Label":2}
{"Functions Text":"This final long-lived stage of disc dispersal gives rise to transition discs which have lifetimes between 105 and 106 yr, but remain optically thick \u2013 \u2018relic discs\u2019","Functions Label":0}
{"Functions Text":"We recall that, traditionally the loops in the polarization diagram (namely, a plot of Q\/I versus U\/I for a given wavelength and for a range of magnetic field strength or orientation values) are identified to be due to the level-crossings in the incomplete PBE regime","Functions Label":0}
{"Functions Text":"see also","Functions Label":0}
{"Functions Text":"The main group ureilites represent the mantle residues after the extraction of","Functions Label":0}
{"Functions Text":"and a sulfur-rich iron melt","Functions Label":0}
{"Functions Text":"We note that the blowout size can be increased with particle porosity and increasing stellar temperature","Functions Label":2}
{"Functions Text":"The goal of these simulations was twofold: (1) to determine how a coronal loop responds to different photospheric velocity patterns, and (2) to investigate how the electric current sheets are formed, as well as the details of the heating that occurs through the dissipation of magnetic energy","Functions Label":3}
{"Functions Text":"related the infrared characteristics to the underlying properties of the stars: objects that present He i features in emission or absorption are B3 or earlier; if the star presents Mg ii in emission but no He i, it is between B2 and b4; objects with Br\u03b3 emission but no evidence of He i or Mg ii are B5 or later.","Functions Label":0}
{"Functions Text":"Although SKA might provide number counts at sub-\u00b5Jy levels","Functions Label":1}
{"Functions Text":"however, one may need to be wary of possible caveats in using radio source number counts at these flux-density levels as one might start seeing at sub-mJy levels, in addition to the powerful distant radio sources, a substantially increasing fraction of very different populations of radio sources, e.g. nearby normal galaxies, starburst galaxies, and even galactic sources","Functions Label":1}
{"Functions Text":"However, the energy balance equations can be expressed in an alternative way by including terms that vanish under spatial averaging and ensure Galilean invariance of all terms","Functions Label":2}
{"Functions Text":"Our result is consistent with that found by","Functions Label":5}
{"Functions Text":"using XMM-Newton data,","Functions Label":5}
{"Functions Text":"and, according to their classification, it identifies M33 X-8 as a broadened disk source, or in other words, as a source whose spectrum is dominated by emission from a hot disk (see Table 2) and where the additional soft component may be the effect of an unrealistic description of the disk spectrum by the diskbb model.","Functions Label":2}
{"Functions Text":"In color-magnitude space, YSES 2b is very close to the innermost three planets of the HR 8799 multi-planetary system","Functions Label":1}
{"Functions Text":"In recent years, integral field spectroscopic (IFS) surveys","Functions Label":0}
{"Functions Text":"have overcome these problems with the use of instruments with larger FoVs and a fully spectral coverage (e.g","Functions Label":0}
{"Functions Text":"ATLAS3D,","Functions Label":0}
{"Functions Text":"subsequently identified 17 candidate late-M, L, and T dwarfs in 232 arcmin2 of HST\/Wide Field Camera 3 (WFC3) imaging of the Great Observatories Origins Deep Survey","Functions Label":0}
{"Functions Text":"using optical and near-infrared color selection, and determined a thin disk vertical scaleheight for these sources of 290 \u00b1 40 pc.","Functions Label":0}
{"Functions Text":"The spatially resolved observations showed that the CND region was a complex dynamical system. For instance, the east and west dots were dominated by a fast shock and a slower shock","Functions Label":0}
{"Functions Text":"Newer, alternate cosmological probes could help alleviate this issue.","Functions Label":3}
{"Functions Text":"Recent examples of such probes include","Functions Label":0}
{"Functions Text":"H\u2009ii starburst galaxy measurements that reach to z \u223c 2.4","Functions Label":0}
{"Functions Text":"Even though there is a lot of scatter in the D \u2212 HT diagram caused by variation in f from one comet to the next","Functions Label":2}
{"Functions Text":"This candidate appears to have one of the most compact orbits among the known SMBH binaries and has overcome the \u2018final parsec problem\u2019","Functions Label":1}
{"Functions Text":"The simplest of such methods uses a Wiener filtering technique","Functions Label":0}
{"Functions Text":"This approach assumes that the density\/velocity field is described as a Gaussian random field and the Wiener filtered reconstruction is the maximum-a-posteriori (MAP) solution for the problem.","Functions Label":0}
{"Functions Text":"Moreover, higher SFRs could be induced by an increased efficiency of star formation due to the enhanced fragmentation in gas-rich, turbulent, and gravitationally unstable high-redshift disks","Functions Label":0}
{"Functions Text":"reflected on their clumpy morphologies","Functions Label":0}
{"Functions Text":"Malanushenko and co-authors","Functions Label":0}
{"Functions Text":"have presented a method for deriving an NLFFF model from sparsely distributed EUV loop observations.","Functions Label":0}
{"Functions Text":"These studies have focused on modeling the field in active regions, where the high density results in bright EUV emission and the limited size of the region allows for a reasonable number of free parameters. Additionally, the complexity of these methods suggests that their primary application would be the detailed study of a specific region of interest, rather than casual production of models for programmatic use. In contrast, the purpose of our study has been to develop a method for the fast production of global coronal magnetic field models based on widely available synoptic magnetograms and coronal images.","Functions Label":1}
{"Functions Text":"and we restricted them to the limiting cases derived in Sect. 3.5 of","Functions Label":2}
{"Functions Text":"rather than allowing them to take arbitrary values.","Functions Label":2}
{"Functions Text":"The radial distance between the centres of the Orion and Sagittarius arms near the Sun is \u03bbrad \u2248 2 kpc (cf.","Functions Label":0}
{"Functions Text":"They also can reconnect with the ambient field (e.g.,","Functions Label":0}
{"Functions Text":"However, recent numerical simulations of thermal tides in optically thick atmospheres by","Functions Label":5}
{"Functions Text":"show behaviour of the flow that is in good agreement with a model that uses radiative cooling.","Functions Label":5}
{"Functions Text":"Therefore, in this work we assumeNewtonian cooling as a first model of the action of radiation on atmospheric tides.","Functions Label":2}
{"Functions Text":"The Planck survey provides a large amount of data for polarisation studies at cloud scales","Functions Label":0}
{"Functions Text":"carried out a comparison of the metallicity gradients in the ISM (traced by young SPs) obtained by different numerical and analytical models","Functions Label":0}
{"Functions Text":"Different MHD oscillation modes have been identified to be responsible for QPPs in a single flaring loop","Functions Label":0}
{"Functions Text":"If the evolution proceeds under self-similar, isothermal collapse then the break in the profile will shift to smaller scales, eventually reaching the radius of the protostar","Functions Label":2}
{"Functions Text":"As described in Section 2.4, we find quiescent counterparts in Pan-STARRS and also add in coverage of southerly declinations by using the DeCAPS catalog (","Functions Label":2}
{"Functions Text":"; cross-matching for both catalogs is as explained in Appendix A.3).","Functions Label":2}
{"Functions Text":"However, these trends do not agree with those obtained by fitting the Burkert profile to nearby galaxies in the SPARC dataset and the classical Milky Way dSphs. This poses an issue for SIBEC-DM with Rc\u2004\u2273\u20041 kpc and a largely CDM-like matter power spectrum at late times","Functions Label":1}
{"Functions Text":"as was used in our simulations, although these scenarios are not well-motivated.","Functions Label":1}
{"Functions Text":"Previously, it has been argued that stars and BHs crossing the disk on low-inclination orbits get captured by Chandrasekhar dynamical friction into the disk","Functions Label":0}
{"Functions Text":"Given the nature of the variability, we measure the period via the reduced \u03c72 of a sinusoidal fit as a function of frequency (ideally suited to sinusoidal variability, e.g.","Functions Label":2}
{"Functions Text":"MaNGA observed approximately 10\u2009000 galaxies, selected as an unbiased sample in terms of stellar mass (${\\it M}_{\\star } \\gt 10^{9}\\, {\\rm M}_{\\odot }$) and environments","Functions Label":0}
{"Functions Text":"The (\u03bc, \u03c3) pairs allowed in the window relevant for the operational gravitational wave detectors","Functions Label":2}
{"Functions Text":"are mainly constrained by (i) the results from searches for microlensing events on stars in our Galactic neighbourhood and (ii) the effect PBH gas accretion would have on the CMB temperature and ionization history","Functions Label":2}
{"Functions Text":"attribute the bimodality to unusually rapid gas accretion at earlier times, which is also characterized by a short time-scale to convert gas to stars.","Functions Label":1}
{"Functions Text":"The importance of additional processes such as internal waves (e.g.,","Functions Label":0}
{"Functions Text":"Additionally, wide binaries are in principle hard to detect, yielding some uncertainty in identifying them and consequently in drawing any conclusion on the PBH abundance","Functions Label":2}
{"Functions Text":"The high Fe charge states (\u27e8Fe\u27e9\u2004\u2265\u200412) and abnormally high O7+\/O6+ ratio (\u22651) are the result of flare-related heating in the corona","Functions Label":2}
{"Functions Text":"and therefore they are independently reliable ICME indicators","Functions Label":2}
{"Functions Text":"We introduce a method to search for signatures of DM annihilation from a Galactic subhalo population using the non-Poissonian template fitting (NPTF) framework","Functions Label":2}
{"Functions Text":"which has previously been applied to characterize unresolved point sources in the inner Galaxy","Functions Label":3}
{"Functions Text":"By using the truncating method to neglect the higher-order derivative terms, the approximate correction formulas of parallel or perpendicular diffusion coefficients were obtained (see, e.g.,","Functions Label":0}
{"Functions Text":"For instance, partial ring distributions were frequently observed for solar wind protons at intermediate heliocentric distances, when the spacecraft approached the SWIC","Functions Label":0}
{"Functions Text":"We note that our 1D methods employed for modeling the collapse, core bounce, and initial explosion do not capture the full physics of the central engine (for a discussion, see","Functions Label":1}
{"Functions Text":"and this is a source of uncertainty in our yield calculations.","Functions Label":1}
{"Functions Text":"Some of these events may correspond to gravitationally lensed events with magnification factors ranging from a few tens to a few hundreds","Functions Label":0}
{"Functions Text":"Moreover, most miscentred clusters are merging or disturbed clusters with lower X-ray or SZ surface brightness, which makes them more difficult to be detected. The discrepancy of SZ signal is at a level of 10 per\u2009cent in our richness range","Functions Label":1}
{"Functions Text":"Allison, Sadler & Meekin (2014) identified four H\u2009i absorbers, including one previously unknown source, with the archival data of the H\u2009i Parkes All-Sky Survey (H\u2009i PASS; see","Functions Label":0}
{"Functions Text":"In particular, the central question of whether glycine (CH2(NH2)C(O)OH) exists or not in the ISM is one of the most pursued targets in astrochemistry.","Functions Label":3}
{"Functions Text":"its detection has never been confirmed","Functions Label":3}
{"Functions Text":"However, the masses corresponding to impact flashes recorded on the Moon are several orders of magnitudes larger than mo","Functions Label":6}
{"Functions Text":"This means that the minimum kinetic energy Emin to produce a detectable impact flash on the Moon is much higher than the kinetic energy of a portion of the meteoroids included in the computation of hourly rates on Earth. This means that the velocity and mass distribution of meteoroids must be somehow included in Eq. (11) to take into consideration for the computation of the probability parameter p only those meteoroids with a kinetic energy above the threshold kinetic energy given by Emin","Functions Label":2}
{"Functions Text":"Simulations of this type seem to indicate that although this process is effective in the case of (quasi-)parallel shocks where the magnetic field is aligned with the direction of motion, it becomes ineffective once the angle between the magnetic field and the shock exceeds approximately 50\u00b0","Functions Label":1}
{"Functions Text":"Star formation can be triggered by these interactions, within clouds that reach sufficient density (Figs. 9 and 10). However, there is evidence that star formation is possible only within dark-matter encapsulated HVCs such as the Smith Cloud","Functions Label":1}
{"Functions Text":"In contrast, higher localization accuracy would be obtained by networking of 3rd generation GW detectors","Functions Label":1}
{"Functions Text":"Over the last decade, large observational efforts have been devoted to map the molecular gas reservoir of galaxies (e.g.,","Functions Label":0}
{"Functions Text":"These studies are largely based on observations of carbon monoxide (CO) rotational emission lines, used as a tracer of cold molecular hydrogen H2 (the ground-state rotational transition in particular traces the total molecular gas best),","Functions Label":0}
{"Functions Text":"Along decades, results based on this indirect method have indicated Z near or slightly above the solar value in nuclear regions","Functions Label":5}
{"Functions Text":"in consonance with predictions of chemical evolution models","Functions Label":5}
{"Functions Text":"and with the use of strong-line methods","Functions Label":5}
{"Functions Text":"Benchmarks by Hochlaf and co-workers","Functions Label":5}
{"Functions Text":"showed that results obtained from this highly correlated approach are close to those deduced using standard coupled cluster techniques extrapolated to the complete basis set (CBS) limit, whereas a strong reduction in CPU time and disc occupancy are observed.","Functions Label":5}
{"Functions Text":"In panel b of Fig. 12, we also superimpose the distribution of [OIII]\/[OII] ratio for the GRB sample of","Functions Label":2}
{"Functions Text":"and GRB 081121 reported here.","Functions Label":2}
{"Functions Text":"For the majority of the GRBs, this ratio is about two, with seven cases at O32 > 4. GRB 021004 has a high value of O32 > 10 and is the strongest LAE of our golden sample (with fesc(Ly\u03b1) of 60%) in agreement with potential high fesc(LyC). Nevertheless, the Ly\u03b1 profile of GRB 021004 is a single peak with no residual flux at the Ly\u03b1 line center.","Functions Label":1}
{"Functions Text":"Additionally, CGM observations infer a significant amount of metals (e.g.","Functions Label":0}
{"Functions Text":"The intensity variations in the major and minor volatile species were found to be periodic, and were dependent on both the observing sub-spacecraft latitude and longitude","Functions Label":0}
{"Functions Text":"Given the reported high spin values for these bright AGNs","Functions Label":2}
{"Functions Text":"we expect the ISCO to sit at \u223c1.25Rg.","Functions Label":2}
{"Functions Text":"Thus, we can compare now the new value obtained for Ekin with the mechanical energy deposited in the ISM by the wind of the WR star, Ew = (0.7\u20132.2) \u00d7 1050 erg","Functions Label":1}
{"Functions Text":"The data were recorded in psrfits format and processed using PSRCHIVE tools","Functions Label":2}
{"Functions Text":"determined by ion storage ring experiments,","Functions Label":0}
{"Functions Text":"The expected B values in star forming regions range from ~100 \u03bcG, for low-mass objects","Functions Label":2}
{"Functions Text":", to ~1 mG, as measured in regions hosting high-mass young stars (e.g.,","Functions Label":2}
{"Functions Text":"Numerous mass spectrometric studies have investigated the production of H+MF via various ion\u2013molecule reactions and its fragmentation by metastable decay and collisions","Functions Label":0}
{"Functions Text":"The salmon-coloured points show recent results from other high-resolution spectrographs:","Functions Label":2}
{"Functions Text":"WASP-121b with ESPRESSO","Functions Label":2}
{"Functions Text":"Since mergers are strong drivers of morphological change, this implies that our high-mass galaxies are mostly elliptical, which is in good agreement with observational results for ellipticals and S0 galaxies (e.g.","Functions Label":5}
{"Functions Text":"For example, studies of young clusters embedded in moderate-mass MCs (\u223c104M\u2299) (e.g.","Functions Label":0}
{"Functions Text":"have shown that their age histograms contain a large majority of young (1\u20132 Myr) objects, but also a tail of older (up to several Myr) ones suggesting an accelerating star formation activity, sometimes followed by a subsequent decline","Functions Label":0}
{"Functions Text":"NGC 419, another young massive cluster with an age of 1.72\u2009Gyr and a mass of \u223c104\u2009M\u2299, are comparably massive with respect to other star clusters that show clear evidence of MPs","Functions Label":6}
{"Functions Text":"the possibility that they are tidal dwarf galaxies \u2013 galaxies formed by strong interactions with recycled material from massive host galaxies, high in metals, and intrinsically born with a lack of dark matter (see e.g.,","Functions Label":6}
{"Functions Text":"\u2013 is ruled out.","Functions Label":6}
{"Functions Text":"A CO spectroscopic redshift of 3.26 was first suggested by Z-spec","Functions Label":1}
{"Functions Text":"observations, then subsequently confirmed by observations by","Functions Label":1}
{"Functions Text":"the Zpectrometer instrument","Functions Label":1}
{"Functions Text":"on the Greenbank Telescope","Functions Label":1}
{"Functions Text":"The Mid-Infrared Spectrograph (MIRS) aboard the Infrared Telescope in Space (IRTS) has also obtained the 4.7\u201311.7$\\, {\\rm \\mu m}$ spectrum for the diffuse ISM towards l = 44\u00b020\u2032, b = \u22120\u00b020\u2032","Functions Label":2}
{"Functions Text":"The primary tracer for H2 in current use is the J = (1\u22120) ground-state rotational transition of 12CO at a wavelength of 3 mm. While this tracer has become widely adopted over the years (see, e.g.,","Functions Label":0}
{"Functions Text":"and has been often defended as a reliable large-scale tracer for molecules in the ISM, it also remains the primary such tracer in common use. There are several reasons to be concerned about this.","Functions Label":1}
{"Functions Text":"It is reasonable to connect the scatter to the stellar rotation rate diversity, considering the fact that there exist noticeable differences in rotation periods between stars of the same temperature in young open clusters (e.g.","Functions Label":2}
{"Functions Text":"Previous sub-arcsecond angular resolution N-band (\u223c8\u201313 \u03bcm) ground-based spectroscopic studies investigated the 11.3 \u03bcm PAH feature in the nuclear and circumnuclear regions of AGN (e.g.,","Functions Label":0}
{"Functions Text":"However, these works were unable to provide definitive details regarding the effect of the AGN on the PAH molecules due to limited wavelength coverage and sensitivity.","Functions Label":3}
{"Functions Text":"The pitch angle and the distance at a reference position of the three arms are taken from","Functions Label":2}
{"Functions Text":"for the Local arm","Functions Label":2}
{"Functions Text":"These authors used the positions of water masers derived from parallax measurements as part of the Bar and Spiral Structure Legacy (BeSSeL) survey to fit the parameters of the spiral arms.","Functions Label":0}
{"Functions Text":"We found good agreement between the position of the FQS clouds and the modelled position of the Local and the Perseus arms,","Functions Label":5}
{"Functions Text":"Therefore, we can neglect the planet imprint and use this band to measure the stellar pulsations, and most specifically to tune their current phases (see phase shifts in","Functions Label":2}
{"Functions Text":"It is interesting to note that the [Ba\/Fe] versus Rgc slope according to this Cepheid sample is also negative, as in our study. [Ba\/Fe] is the only n-capture element-to-iron ratio with a negative radial gradient in our sample of stars and in","Functions Label":5}
{"Functions Text":"Dynamical models and N-body simulations (see, e.g.,","Functions Label":0}
{"Functions Text":"and references therein) have shown that, depending on the initial conditions, a bound pair of clusters may either become unbound, because of significant mass-loss in the early phases of stellar evolution, or merge into a single and more massive cluster on a short time-scale (\u224860\u2009Myr) due to loss of angular momentum from escaping stars","Functions Label":0}
{"Functions Text":"Inspired by earlier studies from Taylor & Manchester (1977) and","Functions Label":0}
{"Functions Text":"Lorimer et al. (2006) applied the snapshot approach to the canonical3 pulsar population to determine best-fitting probability density functions in Galactocentric radius (R), luminosity (L), height with respect to the Galactic plane (z), and the period P for the currently observed population of pulsars.","Functions Label":0}
{"Functions Text":"For instance, we can use these model-independent measurements","Functions Label":0}
{"Functions Text":"to test natural constants such as the speed of light","Functions Label":0}
{"Functions Text":"Selecting SMGs from observations at longer wavelengths is thought to favor galaxies at higher redshifts (e.g.,","Functions Label":1}
{"Functions Text":"although it is difficult to compare the redshift distributions in an unbiased way","Functions Label":1}
{"Functions Text":"and account for intrinsic variations of galaxy far-IR spectral energy distributions (SEDs).","Functions Label":1}
{"Functions Text":"Possible mechanisms responsible for the energization of particles around RFs have been widely investigated based on both spacecraft observations and numerical simulations during the past decade. The strong convection electric field induced by the strong magnetic field gradient of RFs provides significant adiabatic acceleration of the ambient particles","Functions Label":0}
{"Functions Text":"(simply K in other works) is the conversion factor from the MWO HKP-2 H & K flux (numerator of Equation (1)) to physical flux","Functions Label":2}
{"Functions Text":"We assume a power-law energy distribution of radiating electrons with somewhat shallow index of b = \u22121.5 that can account for the relatively flat spectrum of the source","Functions Label":2}
{"Functions Text":"The present observational probes that allow us to have a peak in this epoch are the absorption spectra of high-redshift quasars","Functions Label":0}
{"Functions Text":"However, these studies do not explore lower metallicities, despite available evidence for the existence of a low-metallicity ISM in the past through the discovery of stars with metallicities as low as $10^{-4}\\, \\rm {Z_{\\odot }}$","Functions Label":1}
{"Functions Text":"as well as several others with $\\rm {[Fe\/H]} \\lt -5$","Functions Label":1}
{"Functions Text":"Recent relativistic (magneto-) hydrodynamics simulations","Functions Label":3}
{"Functions Text":"have illustrated the importance of the ambient medium in shaping the jet, thereby highlighting the importance of understanding the remnant structure and ejecta properties","Functions Label":0}
{"Functions Text":"It is, however, conceivable that the large grains in this source are not well aligned because the radiative torque mechanism does not operate efficiently on them: this could happen if the characteristic wavelength of the anisotropic component of the local radiation field were much smaller than the mid-plane grain sizes (e.g.","Functions Label":7}
{"Functions Text":"While there is almost unanimous agreement that AGNs of low to moderate luminosity (Lbol \u2272 1045 erg s\u22121) at z \u2248 0\u20133 lie on or below the main sequence (e.g.,","Functions Label":5}
{"Functions Text":", no consensus exists for AGNs with Lbol > 1045 erg s\u22121.","Functions Label":6}
{"Functions Text":"As the quantity and quality of data available continue to improve over the years, the model parameters derived have become more precise, numerically. Ironically, those numerically more precise results do not converge","Functions Label":3}
{"Functions Text":"table 2 of","Functions Label":3}
{"Functions Text":"The scatters in density law parameters, such as scale lengths, scale heights and local densities of these Galactic components, as reported in the literature, are rather large.","Functions Label":3}
{"Functions Text":"According to","Functions Label":2}
{"Functions Text":"the subhalos also retain their identity for quite some time after accreting a larger halo, so satellites in subhalos less massive than ~1012 M\u2299 do not immediately see the effect of the hot gas in the larger halo and accrete in cold mode.","Functions Label":2}
{"Functions Text":"Thus, consistent with the results of Yang et al. (2012) and B\u00e9thermin et al. (2013), satellite galaxies continue to accrete gas and convert it to stars over a rather long period,","Functions Label":5}
{"Functions Text":"N-body simulations, combined with either hydrodynamic simulations or analytic prescriptions for migration and eccentricity\/inclination damping of planetary growth, have also been used to examine the origins of such systems","Functions Label":0}
{"Functions Text":"It is still difficult to constrain the BH spin parameter from the modelling of the SED of M87 due to some degeneracy in model parameters (wind parameter, s, magnetic parameter ;","Functions Label":1}
{"Functions Text":"The open circle and square are the results from the Arecibo Ultra Deep Survey (AUDS)","Functions Label":2}
{"Functions Text":"Using a Bayesian approach","Functions Label":2}
{"Functions Text":"we computed 95% upper limits for all the nondetections.","Functions Label":2}
{"Functions Text":"The very fast dissolution of tidally filling models with low King model concentration was already extensively discussed in the literature (e.g.","Functions Label":0}
{"Functions Text":"In 2013 May, the Kepler main mission ended with the failure of a second reaction wheel; however, the first four years of Kepler data have led to a wealth of planetary discoveries with a total of 4706 announced planet candidates","Functions Label":0}
{"Functions Text":"However, a large fraction (${\\sim } 28{{\\ \\rm per\\ cent}}$) was found to be inconsistent with the theoretical limit of \u22122\/3 (\u2018line of death\u2019;","Functions Label":6}
{"Functions Text":"and only specific physical scenarios remain plausible (large emitting radii and Lorentz factors of the flow,","Functions Label":6}
{"Functions Text":"Although our sample is definitely too small to make any strong conclusion in terms of statistical incidence of obscured AGN in dual systems, we note that the fraction of CT AGN in our sample of dual AGN is 25\u201350 per cent, i.e. higher than the fraction of hard X-ray selected CT AGN in isolated systems in a similar luminosity interval (BAT: 27 \u00b1 4 per cent,","Functions Label":1}
{"Functions Text":"This method has since been used to successfully uncover highly obscured and even Compton-thick AGNs in several other works thus far","Functions Label":0}
{"Functions Text":"In the case of collimated relativistic jets, magnetic fields must play an important role","Functions Label":0}
{"Functions Text":"Optical coordinates, right ascension and declination (epoch 2000.0) for the identified counterpart from Zaritsky et al. (2002), or \u2013 when not available there \u2013 from","Functions Label":2}
{"Functions Text":"For about 80 yr since the discovery of the extremely hot corona around the late 1930s (Grotian 1939; Edlen 1945), people have worked hard on addressing this issue, and great advances have been made in observation and theoretical studies","Functions Label":0}
{"Functions Text":"Cepheids analysis from","Functions Label":2}
{"Functions Text":"green","Functions Label":2}
{"Functions Text":"The latter model has been invoked as a possible mechanism in the downstream of the CME shock","Functions Label":2}
{"Functions Text":"Since then, several authors","Functions Label":0}
{"Functions Text":"have established precise initial mass ranges for ECSNe to occur, although these mass ranges are highly sensitive to the adopted convection criteria, overshooting, and mass-loss prescriptions","Functions Label":0}
{"Functions Text":"Other emission lines, however, such as the far-infrared [C ii]\u03bbl58 \u00b5m line, are strikingly enhanced on global scales in dwarf galaxies (e.g.,","Functions Label":1}
{"Functions Text":"Subsequently, a number of works have","Functions Label":0}
{"Functions Text":"and to use their abundances to estimate the ages of stars, often using neutron capture s-process elements in combination with other elements with opposite behaviours, such as \u03b1 elements \u2013 that we indicate as chemical clocks \u2013 and thus maximising the dependence of the relationship with age (see, e.g.,","Functions Label":0}
{"Functions Text":"We assume that polarized BELs are scattered into the line of sight by material that is close to coplanar with the BLR (i.e. the torus). This prediction has been searched for in RQ-NLS1s, but many objects have not been detected in polarized light, and none of the detected show any significant broadening of the BELs (e.g.","Functions Label":1}
{"Functions Text":"Inclusion of mass-loss and\/or rotation would produce a similar increase in the Cepheid luminosity level at fixed mass (see","Functions Label":2}
{"Functions Text":"for details).","Functions Label":2}
{"Functions Text":"Doing so, we find EX \u2248 EU \u223c 2 \u00d7 1032\u2009erg for AD\u2009Leo","Functions Label":2}
{"Functions Text":"Evidence for offset dust continuum emission relative to the rest-UV has been identified in several high-redshift Lyman-break galaxies (LBGs;","Functions Label":1}
{"Functions Text":"In previous studies, geometrical models based on the assumption of different cone shapes were developed to obtain CME 3D parameters from single spacecraft observations","Functions Label":0}
{"Functions Text":"Analysis of the particle yields produced in relativistic A+A collisions within statistical (thermal) models, i.e., the Hadron Resonance Gas (HRG) model","Functions Label":0}
{"Functions Text":"shows the importance of the particle hard core repulsion.","Functions Label":0}
{"Functions Text":"The dimensionless accretion rate is estimated by $\\dot{\\mathscr {M}}=20.1\\, \\ell _{44}^{3\/2}M_7^{-2}$ from the Shakura\u2013Sunyaev disc model","Functions Label":2}
{"Functions Text":"where \u211344 is the 5100 \u00c5 luminosity in units of $10^{44}\\, {\\rm erg\\, s^{-1}}$ and $M_7=M_{\\bullet }\/10^7\\, \\mathrm{M}_{\\odot }$.","Functions Label":2}
{"Functions Text":"The sample of","Functions Label":2}
{"Functions Text":"showed spectral changes with observed power-law slope varying between 1.0 and 2.0 (see their Fig. 7). For a typical Galactic absorption of 3 \u00d7 1020 cm-2 the change from slope of 1.0 to 2.0 would alter our estimated fluxes by \u221214% (ROSAT), \u221213% (XMM-Newton), +7% (Swift-XRT), +76% (Suzaku), +25% (Einstein-IPC). The change is large for Suzaku observations since in this case we use the count rate between 2.0\u201310.0\u2009keV and extrapolate it to the soft band. All other satellites are sensitive in the soft band and hence the fluxes are less dependent upon the assumed spectral index.","Functions Label":2}
{"Functions Text":"They can also shed light on the origins of supermassive black holes and early cosmological reionization and chemical enrichment","Functions Label":3}
{"Functions Text":"A high R-value suggests a small viewing angle to the jet axis, while a low R-value indicates more of an edge-on view to the quasar","Functions Label":0}
{"Functions Text":"These findings by","Functions Label":1}
{"Functions Text":", along with the discrepancy between our calculated ratio of Ebp\/kBTc = 5.5 \u00b1 0.1 and the prediction of Ebp\/kBTc = 7, suggest that the model of Scudder & Olbert (1979) requires a minor update to either the theory or to the input parameters.","Functions Label":1}
{"Functions Text":"With such properties, TOI-849b represents one of the few planets populating the hot Neptune desert, a region on the radius-orbital distance plane characterised by a surprising deficit of Neptune-sized planets on very short orbits (e.g.","Functions Label":0}
{"Functions Text":"In Goswami et al. (2021), we present a detailed analysis and discussion on the classification criteria of CEMP stars, as well as the formation scenarios of CEMP stars put forward by different authors","Functions Label":0}
{"Functions Text":"Recently, we proposed an improved Amati correlation","Functions Label":0}
{"Functions Text":"by using the Gaussian copula, which is a powerful statistical tool capable of describing the dependence structures between multivariate random variables, and has been applied to various fields by the astronomical community","Functions Label":0}
{"Functions Text":"An interesting implication is that, if BHs settle into the disk, they interact dynamically and form BH\u2013BH binaries efficiently, and frequent dynamical interactions and gas effects drive the BHs to merger, producing gravitational waves (GWs) detectable by LIGO, VIRGO, and KAGRA","Functions Label":0}
{"Functions Text":"Deep Herschel\/SPIRE spectroscopy has also revealed a number of FSL detections, either in individual objects","Functions Label":0}
{"Functions Text":"If 26Al was introduced into the solar system at the earliest stage of the disk evolution (e.g.,","Functions Label":2}
{"Functions Text":"differences in Be\u2013B and Al\u2013Mg systematics between CH\u2013CB and CV CAIs imply that the injection of 26Al have occurred between the evolutionary stages class I and class II of the solar protoplanetary disk.","Functions Label":2}
{"Functions Text":"The inner jet","Functions Label":0}
{"Functions Text":"and displays strong and variable radio polarization (e.g.","Functions Label":0}
{"Functions Text":"A number of theoretical studies predicted that the accretion flow components of hot geometrically thick (RIAF-like) and cold geometrically thin can coexist in either horizontal or vertical stratification (e.g.,","Functions Label":0}
{"Functions Text":"Two-point statistics are central to many of the leading cosmological analyses of the large-scale structure searching for deviations from \u039bCDM","Functions Label":0}
{"Functions Text":"and a great deal of effort has gone into accurately modelling the non-linear matter power spectrum in modified gravity and dark energy cosmologies \u2013 a theoretical ingredient essential to extract the cosmological information locked in small scales (e.g.","Functions Label":0}
{"Functions Text":"Indeed, Mg ii is known as a good tracer of high column density H\u2009i\u2009gas in damped Lyman \u03b1 absorbers (e.g.","Functions Label":0}
{"Functions Text":"on the other hand explored two types of models, with ages being either uniformly distributed between 0 and 1000 Myr, or linearly distributed in log space between 1 and 1000 Myr.","Functions Label":6}
{"Functions Text":"These latter authors found that the uniform-age models efficiently explain the size and luminosity statistics of bright sources observed by LOFAR, while the log-uniform models were a better representation of the faint population.","Functions Label":1}
{"Functions Text":"Modelling by both Shabala et al. (2020) and","Functions Label":5}
{"Functions Text":"confirms the picture in which the remnant lobes fade quickly below the LOFAR detection limit.","Functions Label":5}
{"Functions Text":"This can be mitigated by using integral field spectroscopy (IFS) which is being increasingly used for extragalactic studies (e.g.","Functions Label":0}
{"Functions Text":"although there could still be projection effects with the IFS data.","Functions Label":0}
{"Functions Text":"Recently, it has been demonstrated that its thermal X-ray spectrum is dominated by the colliding-wind region in the close binary, with only a weak\/moderate contribution coming from the wind-wind interaction in the wide orbit","Functions Label":0}
{"Functions Text":"It is also well known that the radius R1.4 of canonical NSs is essentially determined by the pressure at densities around \u03c10 \u223c 2.5\u03c10","Functions Label":2}
{"Functions Text":"while the maximum mass of NSs is determined by the pressure at higher densities reached in the core.","Functions Label":2}
{"Functions Text":"Our findings of bulges and bars suggest a considerable on-going evolution in the local LSB galaxies and the bars might as well be playing a role in the bulge growth","Functions Label":1}
{"Functions Text":"A fraction of the stellar wind is captured and channelled along the strong magnetic field","Functions Label":0}
{"Functions Text":"of the neutron star on to the magnetic poles, producing regular X-ray pulsations caused by the spin period \u223c283\u2009s","Functions Label":0}
{"Functions Text":"of the neutron star.","Functions Label":0}
{"Functions Text":"Recent experiments for key nuclear reactions like 7Be(n,p)7Li and 7Be(d,p)24He allow for a reduction of the 7Li production by about 12%","Functions Label":6}
{"Functions Text":"compared to previous calculations.","Functions Label":6}
{"Functions Text":"We shall adopt here the EoS of the BSk21 model","Functions Label":2}
{"Functions Text":"as a representative example of contemporary EoS for the complete NS structure,","Functions Label":2}
{"Functions Text":"Our group is addressing this problem by combining a variety of complementary perspectives:","Functions Label":2}
{"Functions Text":"(iii) by characterizing the three-dimensional (3D) global velocity space through the analysis of the velocity dispersion profile and rotation curve from resolved star spectroscopy","Functions Label":2}
{"Functions Text":"A dust cloud composed by large grains ( \u223c 1\u2009\u03bcm) would suppress the scattered intensity even at 1 keV, while it would significantly attenuate X-rays at \u22640.5 keV (e.g.","Functions Label":2}
{"Functions Text":"Previously, we retrieved and cross-matched a large quantity of atomic data from several major atomic databases such as the","Functions Label":2}
{"Functions Text":"and providers within the Virtual Atomic and Molecular Data Centre (VAMDC;","Functions Label":2}
{"Functions Text":"in preparation for quality assessment work","Functions Label":2}
{"Functions Text":"A few examples are","Functions Label":0}
{"Functions Text":"and superluminal motion and high brightness temperature","Functions Label":0}
{"Functions Text":"They may also be aligned in the direction of","Functions Label":0}
{"Functions Text":"or the drift velocity of the grains relative to the ambient gas","Functions Label":0}
{"Functions Text":"In addition to the stellar mass, the spin-filament alignment was shown to depend on other internal properties of galaxies. Blue or rotation-supported galaxies were found to dominate the alignment signal at low stellar mass, while red or dispersion-dominated galaxies tend to show a preferential perpendicular alignment","Functions Label":0}
{"Functions Text":"Instead, the most successful theoretical models link the growth of stellar mass to the growth of the dark matter halos that galaxies inhabit, for example, via subhalo abundance matching (e.g.,","Functions Label":0}
{"Functions Text":"This Tmai is at the low end of the Tmai output by thermal evolution models for multi-Gyr-old sub-Neptunes (e.g.,","Functions Label":1}
{"Functions Text":"Based on weak sources in Chandra deep field images, the threshold for PB adopted based on a balance between reliability and completeness varies from 0.002 to 0.007","Functions Label":2}
{"Functions Text":"Alternatively, the scarcity of detected pulsars might be caused by a more complex scattering structure towards the GC","Functions Label":0}
{"Functions Text":"The upper panel of Figure 4 also shows a strong correlation between [Na\/Fe] and the \u03b4CN index, which is in good agreement with previous studies","Functions Label":5}
{"Functions Text":"Thus, in clustered DE scenarios, we should consider the contribution of perturbated DE components to the total mass of the haloes","Functions Label":2}
{"Functions Text":"We used total fluxes of 0.2 Jy and 0.55 Jy for the artificial sources; these values ensure that our simulated outflows are sufficiently faint to not violate the constraints given by the known recent brightness evolution of Sgr A* (0.2 Jy from the mean variability of \u224815% from June 2013 to February 2014 at 41 GHz, with 0.55 Jy corresponding to the strongest variation in the same period,","Functions Label":2}
{"Functions Text":"For this reason a subregion of this cloud has been the subject of many previous papers, dealing with different observational aspects of the star formation (SF), such as","Functions Label":0}
{"Functions Text":"and clustering","Functions Label":0}
{"Functions Text":"According to the pseudo-time-dependent gas-phase astrochemical model under dense cloud conditions (104 cm\u22123, 10 K, 10 mag) by","Functions Label":1}
{"Functions Text":"the conversion of atomic N into N2 takes an order of Myr, depending on assumed elemental abundances. In the gas-ice model of Daranlot et al. (2012), under the similar physical conditions, the conversion of atomic N to N2 takes ~5 \u00d7 105 yr, and it occurs after the significant fraction of nitrogen is frozen out.","Functions Label":1}
{"Functions Text":"In particular, it is known to often display a blue wing (e.g.","Functions Label":3}
{"Functions Text":"generally interpreted as a signature of outflows with dust preferentially hiding one cone behind the stellar disc. For that reason, some studies have excluded the [O\u2009iii] blue wing","Functions Label":3}
{"Functions Text":"Both Bernard-Salas et al. (2009) and","Functions Label":5}
{"Functions Text":"reported data from the high-resolution Spitzer-IRS spectra.","Functions Label":5}
{"Functions Text":"In this work, we aim to better understand how these considerations affect the observed SZE signals using high-resolution submillimeter and radio imaging of a representative sample of SZE-selected clusters.We present new observations at 345 GHz (19 2 resolution) with the Large APEX Bolometer Camera","Functions Label":2}
{"Functions Text":"on the Atacama Pathfinder EXperiment (APEX","Functions Label":2}
{"Functions Text":"telescope","Functions Label":2}
{"Functions Text":"Meanwhile, with the progress of observational studies, two groups of theoretical models, magnetic reconnection models and magnetohydrodynamic wave models, have traditionally attempted to explain coronal heating, but so far no models can address the key mystery perfectly","Functions Label":3}
{"Functions Text":"It has a contribution of at least 15 per\u2009cent in the clump at early stages of massive star formation, which is lower than that reported in previous studies","Functions Label":6}
{"Functions Text":"Interestingly,","Functions Label":0}
{"Functions Text":"was the first to suggest the existence of an observational signature for the transition between fully and partly convective structures for pre-main sequence stars and predicted that it would result in a HRD gap. This author explored signatures of this transition in young clusters and linked the growth of a radiative core to rapid change in effective temperature caused by changes in the dominant energy transport mechanism and ignition of hydrogen burning.","Functions Label":0}
{"Functions Text":"As for the experiment on ice by","Functions Label":1}
{"Functions Text":"it is well known that reaction barriers possibly present in gas-phase reactions are not significantly reduced when moving to ice-mediated reactions","Functions Label":1}
{"Functions Text":"We chose to compare to the","Functions Label":2}
{"Functions Text":"spectral models from WM-BASIC for OB-stars","Functions Label":2}
{"Functions Text":"However, considering that little or nothing is known about the LECR fluxes in the Cas A SNR and uncertainties in the generally small cross-sections for the relevant reactions to produce either ${}^{44}_{}\\mathrm{Ti}$\u2009 or excited ${}^{44}_{}\\mathrm{Ca}^{*}$","Functions Label":1}
{"Functions Text":"the validity of such an interpretation of the discrepant measurements of ${}^{44}_{}\\mathrm{Ti}$\u2009 fluxes at 68 and 78 keV and at 1.157 MeV by different instruments and by the same instrument (SPI) may be doubted.","Functions Label":1}
{"Functions Text":"These triggering processes were numerically studied by Karlick\u00fd & Jungwirth (1989) and","Functions Label":0}
{"Functions Text":"Additional evolutionary channels for SNIa include","Functions Label":0}
{"Functions Text":"the core-degenerate channel","Functions Label":0}
{"Functions Text":"We ignore the pressure term in equation (4), which leads to a set of equations that conserve energy","Functions Label":2}
{"Functions Text":"The peak column densities and total masses of both sources deduced from the 1.3 mm continuum emission are \u223c1 \u00d7 1024 cm\u22122, and \u223c2 \u00d7 102 M\u2299, respectively, with an assumption","Functions Label":2}
{"Functions Text":"and a uniform dust temperature of 20 K, which is typically adapted\/estimated for galactic high-mass star-forming dust clumps (e.g.,","Functions Label":2}
{"Functions Text":"Dispersions are thought to be driven at least partially by thermal velocities or supernovae","Functions Label":1}
{"Functions Text":"Early work highlighting the issue of the high-redshift offset in the [O iii]\u03bb5007\/H\u03b2 vs. [N ii]\u03bb6584\/H\u03b1 BPT diagram focused on these parameters (e.g.,","Functions Label":0}
{"Functions Text":"In fact, the jet\u2013wind interaction alone can already perturb the jet","Functions Label":0}
{"Functions Text":"other studies describe the formation of both molecules and dust clusters from the shocked gas by assuming a chemical kinetic approach under non-equilibrium conditions and the subsequent coalescence and coagulation of these clusters to form dust grains","Functions Label":0}
{"Functions Text":"The presence of the substructure has been confirmed by Chandra and XMM-Newton","Functions Label":0}
{"Functions Text":"as well as by more recent SZE measurements","Functions Label":0}
{"Functions Text":"Our flared vertical profiles for the thin and thick disks","Functions Label":5}
{"Functions Text":"and are consistent with the number simulations of the chemodynamical evolution in Galactic disks formed in the cosmological context","Functions Label":5}
{"Functions Text":"The upper atmospheres (above optically thick clouds) of giant exoplanets and those of smaller planets around M stars can be probed using spectroscopy during primary and\/or secondary transits","Functions Label":0}
{"Functions Text":"The laboratory data most widely used for comparison to observations are those provided by","Functions Label":2}
{"Functions Text":"The first reference gives IR spectra and band strengths of methanol ice at 10 K in the 2.5\u201320 \u03bcm range.","Functions Label":2}
{"Functions Text":"However, over the last few years a number of multifrequency compact source detection techniques have been proposed in the literature","Functions Label":0}
{"Functions Text":"A statistical study was performed by Richardson & Cane (2011) on more than 300 ICMEs, showing that 80% of them is associated with an FD, detected by the anticoincidence guard data on the International Monitoring Platform (IMP-8;","Functions Label":0}
{"Functions Text":"and that the minimum GCR intensities occur within the MC.","Functions Label":0}
{"Functions Text":"Indeed, the scientific debate about the emission profile of the jet and the subsequent gamma-ray production mechanism of GRB 170817A is still ongoing","Functions Label":3}
{"Functions Text":"For the refractory and main component elements in CC chondrites, we examine the elemental and isotopic compositions of Ti and Cr, respectively, because these are lithophile elements whose isotopic compositions have been measured precisely for a large number of chondrites and their components","Functions Label":3}
{"Functions Text":"GRB 170817A was followed by the discovery of the optical counterpart Swope Supernova Survey 17a [SSS17a (AT 2017gfo)] \u223c11 h later in the galaxy NGC 4993","Functions Label":0}
{"Functions Text":"and later confirmed by others teams","Functions Label":0}
{"Functions Text":"The model of Charbonnel & Lagarde (2010) of thermohaline instability induced mixing and the model by Eggleton et al. (2008) are both based on the ideas of","Functions Label":0}
{"Functions Text":"Cluster number counts from Sunyaev-Z\u2019eldovich surveys are routinely modelled in terms of the signal-to-noise ratio (S\/N) or the Compton parameter of the detections, which can be related to the cluster mass via scaling relations from X-ray, lensing, or velocities (e.g.","Functions Label":0}
{"Functions Text":"This result is consistent with previous research within a 1\u03c3 error","Functions Label":5}
{"Functions Text":"Here, it is worth noting that the 1\u03c3 errors of the \u03b3 best fit from previous research are both larger than 0.01.","Functions Label":6}
{"Functions Text":"For the collision term associated with neutrino emission, absorption, and scattering with leptons, nucleons, and nuclei handles, the basic neutrino reactions are adopted","Functions Label":2}
{"Functions Text":"In the optically thin limit, the emission is significantly polarized","Functions Label":0}
{"Functions Text":"an effect that has been observed in higher-luminosity AGN sources","Functions Label":5}
{"Functions Text":"It is also much better at driving winds, because the CRs do not suffer strong energy losses via Alfven wave heating","Functions Label":2}
{"Functions Text":"We repeated the plasma pressure calculation presented by","Functions Label":2}
{"Functions Text":"and Fuselier et al. (2012) for the new ENA energy spectrum.","Functions Label":2}
{"Functions Text":"Such evolutionary behavior is consistent with \u201cstrangulation\u201d wherein cold gas that could be used for star formation is depleted as satellites are accreted (e.g.,","Functions Label":5}
{"Functions Text":"The Pipe Nebula,","Functions Label":0}
{"Functions Text":"has played a workhorse role in a number of previous studies (e.g.","Functions Label":0}
{"Functions Text":"Many of these works have the common goal of determining how GMCs are organized in the stages that precede their collapse and the consequent conversion of gas into stars.","Functions Label":0}
{"Functions Text":"For instance, the TDCOSMO collaboration","Functions Label":0}
{"Functions Text":"has achieved \u223c2% in the inference of H0 from time-delay cosmography under the assumption that the radial-mass distribution of the lens can be described by a power-law mass profile or a composite of a dark-matter halo","Functions Label":0}
{"Functions Text":"and baryon matter.","Functions Label":0}
{"Functions Text":"As is often observed","Functions Label":5}
{"Functions Text":", we require multi-temperature components to achieve an adequate description of the observed coronal spectra.","Functions Label":5}
{"Functions Text":"May & Stevenson (2020) claimed that the differences between the retrieved phase offsets is the result of temporal binning which was not used by","Functions Label":1}
{"Functions Text":"and May & Stevenson (2020) but was used by Mendon\u00e7a et al. (2018), Morello et al. (2019), and this work.","Functions Label":1}
{"Functions Text":"Various observational techniques, such as measuring the Gunn\u2013Peterson optical depth from QSO spectra or the prevalence of Ly \u03b1 emission in high-redshift galaxies, have placed very tight constraints on the volume filling fraction of neutral hydrogen in the intergalactic medium (IGM) towards the end of reionization at z\u223c 6","Functions Label":0}
{"Functions Text":"More recently,","Functions Label":0}
{"Functions Text":"also investigated the gradients of n-capture element abundance-to-iron ratios with respect to Rgc for a sample of 435 Cepheids.","Functions Label":0}
{"Functions Text":"Except for two objects","Functions Label":0}
{"Functions Text":"in the local Universe no ionizing radiation has been detected directly","Functions Label":0}
{"Functions Text":"although some objects show indirect evidence of photon leakage","Functions Label":0}
{"Functions Text":"From the figure, it seems that there is not difference between the SM star and other stars in the remnant of SN 1006 in the aspect of proper motion, i.e. the proper motion of the SM star only slightly deviates from the median value of the proper motions of the stars at the direction of the SNR centre of SN 1006, and such a proper motion disfavours the SM star as the surviving companion of SN 1006","Functions Label":5}
{"Functions Text":"As an example, the analysis of the hyperfine structure of several N-bearing species, such as N-protonated isocyanic acid (H2NCO+,","Functions Label":0}
{"Functions Text":") which has been detected toward G+0693-0.027","Functions Label":0}
{"Functions Text":"was required for its conclusive line-by-line identification.","Functions Label":0}
{"Functions Text":"The observational constraints of rdt and rdt\/rBLR are discussed in estimating tcross for the double-peaked BEL CL-AGN NGC 3516, where rdt is a dust torus radius","Functions Label":2}
{"Functions Text":"In recent years, attention directed towards explosions of sub-MCh WDs triggered by double detonations (primarily related to a DD scenario) has led to promising results (e.g.","Functions Label":0}
{"Functions Text":"found that the deuteration (D\/H ratio) of HC(O)NH2 in IRAS 16293 B is similar to that of HNCO, in agreement with the hypothesis that both species are chemically related via grain-surface reactions.","Functions Label":0}
{"Functions Text":"Also, NGC 4490 has a giant H i envelope that probably originated from the star formation","Functions Label":0}
{"Functions Text":"Alternatively, one can compute the bolometric luminosity following","Functions Label":2}
{"Functions Text":"However, there is overwhelming observational evidence that magnetic fields in the ISM have well-defined directions, indicating that turbulence is sub, trans-Alfv\u00e9nic and hence turbulent properties are highly anisotropic","Functions Label":0}
{"Functions Text":"However, the question of whether galactic bars can significantly affect AGN activity is still under debate","Functions Label":0}
{"Functions Text":"N. E. Raouafi et al. (2015, in preparation) have argued that type II spicules have much more in common with so-called \u201cclassical\u201d spicules","Functions Label":5}
{"Functions Text":"than do type I spicules. In particular, type II and classical spicules are both commonly observed in quiet Sun and coronal hole regions, whereas type I spicules appear to be exclusively confined to active regions.","Functions Label":5}
{"Functions Text":"The factor 1.08 is the multiplicative shear calibration bias of the used KSB+ pipeline","Functions Label":2}
{"Functions Text":"to convert from measured to true ellipticity.","Functions Label":2}
{"Functions Text":"Thus, it is possible that disks were massive enough to form the cores of planets at younger ages. This idea has been suggested by","Functions Label":1}
{"Functions Text":"Williams (2012), and Najita & Kenyon (2014), among others. In this scenario, the vast majority of the material composing planets must already be in the form of planetesimals, for rocky planet formation, and of already-formed planetary cores. The latter condition is necessary as gas giant planets need to accrete gas from the gas-rich disk.","Functions Label":1}
{"Functions Text":"The bimodality has now been observed in some simulations","Functions Label":5}
{"Functions Text":"There is also an observed discrepancy between the radial extents of the gas and dust components of protoplanetary discs, with dust discs being significantly more compact","Functions Label":0}
{"Functions Text":"This process can end up as a SN Ia, a highly magnetized WD (MWD), or an accretion-induced collapse","Functions Label":0}
{"Functions Text":"The synchrotron peak usually moves to higher frequencies with increasing flux during outbursts","Functions Label":0}
{"Functions Text":"but no correlation between the break energy and the flux exists when a broken power law is adopted to fit the X-ray spectra","Functions Label":0}
{"Functions Text":"The reason for this discrepancy is not known, but it is likely related to the different redshift ranges probed by the two methods (much more local sources are considered in the second one), and\/or\u2014under the assumption of a strong correlation between radio luminosity and environmental density (e.g.,","Functions Label":1}
{"Functions Text":"but see further in this section for different points of view)","Functions Label":1}
{"Functions Text":"To avoid catastrophic suppression of the dynamo action (\u03b1-quenching), the magnetic helicity due to the small-scale magnetic field should be removed from the system","Functions Label":0}
{"Functions Text":"Mechanisms suggested to produce these small-scale magnetic helicity fluxes are:","Functions Label":0}
{"Functions Text":"and through diffusive flux","Functions Label":0}
{"Functions Text":"Top right: the r31 brightness temperature ratio of VLASPECS galaxies (green circles) is similar to that of","Functions Label":5}
{"Functions Text":"and z > 2 dusty star-forming galaxies (DSFGs; blue squares; compilation from Sharon et al. 2016; including data from","Functions Label":5}
{"Functions Text":"However, at the corresponding frequency of 138\u2009d\u22121, the TESS high-cadence data (sector 10) show no signs of such a signal, confirming previous negative reports","Functions Label":5}
{"Functions Text":"The current model of the CGM suggests the presence of a clumpy multiphase medium which extends beyond the virial radius of the host galaxy, with a declining radial density profile, containing a substantial amount of gas and metals (e.g.","Functions Label":0}
{"Functions Text":"Density Functional Theory (DFT) has been used rigorously to calculate the harmonic frequencies and intensities of vibrational modes of PAHs in various forms including size, composition and charge states","Functions Label":0}
{"Functions Text":"The latest Fermi Large Area Telescope (Fermi-LAT) survey data are now providing strong evidence towards an origin mostly due to integrated radiation from blazars and radio galaxies (e.g.","Functions Label":0}
{"Functions Text":"The unprecedented quality of the light curves combined with new curve-shifting algorithms","Functions Label":2}
{"Functions Text":"lead to time delays with typically \u223c3 per cent accuracy","Functions Label":2}
{"Functions Text":"The stream interface (S\u2032-F\u2032) is indicated by the vertical line in Fig. 2 and is characterized by a drop of the O7+\/O6+ abundance ratio measured with SWICS in the bulk solar wind","Functions Label":2}
{"Functions Text":"For grains surrounded by an ice mantle, the optical properties are derived with the core-mantle Mie theory using the BHCOAT routine given in","Functions Label":2}
{"Functions Text":"The more contentious issue is that of the phase curve\u2019s phase offset and nightside temperature.","Functions Label":6}
{"Functions Text":"initially reported only a 2\u03c3 upper limit on the nightside temperature of 650\u2009K, while all subsequent reanalyses (including ours) favour a significantly detectable nightside temperature of \u223c800\u2009K.","Functions Label":6}
{"Functions Text":"In this scenario, BHs form in situ in the vicinity of a GN and sink to the inner region due to mass segregation or they are delivered to these regions by infalling globular clusters","Functions Label":0}
{"Functions Text":"then get captured in the disc by hydrodynamic drag as they cross the disc (e.g.","Functions Label":0}
{"Functions Text":"Similar outflows have been reported for","Functions Label":5}
{"Functions Text":"and for one hot Neptunian planet, GJ 435 b","Functions Label":5}
{"Functions Text":"Observations of the Antennae galaxies report only one TDG candidate, at the tip of the southern tail","Functions Label":3}
{"Functions Text":"but the exact nature of this structure is still questioned","Functions Label":3}
{"Functions Text":"Our adopted classification scheme is based on physical properties of a young stellar object, such as envelope and disk masses (e.g.","Functions Label":2}
{"Functions Text":"rather than on observational signatures, such as submillimeter luminosities or effective temperatures","Functions Label":6}
{"Functions Text":"Thus, both survival and replenishment of galaxies should be expected over the time, and two important factors come into play: (i) the accretion rate of galaxies; and (ii) the orbital dependence of galaxy properties (e.g.","Functions Label":2}
{"Functions Text":"The model has been chosen on the basis of a \u03c72 test and, in every image, the best fit is provided by a Moffat function","Functions Label":2}
{"Functions Text":"Different models for galaxy formation and evolution often make very different assumptions and\/or predictions. Among them, semi-analytic galaxy formation models (SAMs; e.g.,","Functions Label":0}
{"Functions Text":"are two powerful tools to trace galaxy formation and evolution in cosmological volumes. SAMs are phenomenological models that use an approximate\/empirical formula to describe all baryonic processes relevant to galaxy formation, such as gas accretion, heating and cooling, star formation, feedback from stars and AGN, mergers, and stripping due to tides and ram pressure.","Functions Label":0}
{"Functions Text":"Nevertheless, a recent study of the dynamics of dwarf spheroidals orbiting around the Milky Way has shown some inconsistencies with previous results","Functions Label":6}
{"Functions Text":"The escape fraction is a key parameter in studies of the contribution of the observed galaxy population to reionization","Functions Label":0}
{"Functions Text":"semi-analytic modelling of reionization (e.g.","Functions Label":0}
{"Functions Text":"Since the errors of the LIGO-estimated rates are dominated by Poisson statistics","Functions Label":2}
{"Functions Text":"we approximate the PDF for the expected number of detections $\\mathcal {N}=\\mathcal {R}VT$ (from the surveyed space\u2013time volume VT) by $\\mathrm{d}P\/\\mathrm{d}\\mathcal {N}\\propto \\mathcal {N}^{k-1\/2}\\mathrm{e}^{-\\mathcal {N}}\/k!$, where k = 1 for each of the relevant cases ($\\mathcal {R}_{190814}$, $\\mathcal {R}_{170817}$, and $\\mathcal {R}_{190425}$), and the factor of $\\mathcal {N}^{-1\/2}$ is from Jeffrey\u2019s prior","Functions Label":2}
{"Functions Text":"The estimated spin-down energy is \u0116 = 1.36 \u00d7 1036 erg s-1 and the surface dipolar magnetic field is 7.4 \u00d7 1011 G","Functions Label":0}
{"Functions Text":"The initial perturbation can be compensated or uncompensated, which leads to different void growth scenarios","Functions Label":0}
{"Functions Text":"An accurate determination of the low-energy cutoff to non-thermal electron distributions is crucial for the calculation of power and consequently non-thermal energy in solar flares","Functions Label":3}
{"Functions Text":"Since AGB stars can become C rich and have been confirmed both theoretically and observationally as the main stellar site for the s-process (see, e.g.,","Functions Label":0}
{"Functions Text":"it is natural to interpret these post-AGB observations as the signature of the nucleosynthesis and mixing events that occurred during the preceeding AGB phase.","Functions Label":0}
{"Functions Text":"Previous studies suggested that the early disappearence of circumstellar discs could be related to environmental effects imposed by the presence of massive stars that produce strong UV radiation, stellar winds, and supernova explosions (see e.g.","Functions Label":0}
{"Functions Text":"However, we see no dependency of the spectral index on the position of the stars in our sample and any nearby OB star surrounding the Lupus clouds to support this scenario.","Functions Label":6}
{"Functions Text":"To avoid the redundancy and computational waste of representing the orbits of every single particle in the model, one can use a phase-space distribution function (DF) to represent each population of constituent particles (typically, various stellar populations and dark matter; see e.g.","Functions Label":2}
{"Functions Text":"While the composition of the target surface was different than in","Functions Label":1}
{"Functions Text":"and Higa et al. (1996) (fine granular material vs. solid ice), the similar behavior of the coefficient of restitution supports the fact that particle-surface collisions are very different from particle-particle collisions, and coefficients of restitution are only velocity dependent for collisions with particles with very different sizes (a much larger particle can be approximated as a target surface).","Functions Label":1}
{"Functions Text":"In particular, the \u201csubmillimeter-HCN diagram\u201d, first proposed in Izumi et al. (2013) and later expanded upon in","Functions Label":0}
{"Functions Text":"is a very notable example of the use of molecular line ratios as a probe of AGN-galaxies; this diagram makes use of two line ratios, HCN(4\u22123)\/HCO+(4\u22123) and HCN(4\u22123)\/CS(7\u22126), where all of the molecules involved are considered tracers of dense gas.","Functions Label":0}
{"Functions Text":"One possibility to solve this issue is that the potential Psyche asteroid family was created at an early time, e.g. within the first 500\u2009Myr of Solar system history","Functions Label":1}
{"Functions Text":"This would allow the family fragments to be ground down by collisional evolution and be unobservable today. The same models show that, even in this case, today there should be several surviving fragments having diameters around 20\u2009km and above the detection limit.","Functions Label":1}
{"Functions Text":"The CH and CH\/CB (hereafter: CH\u2013CB) chondrites and their components are characterized by enrichments in 15N (up to 1,100\u2030;","Functions Label":0}
{"Functions Text":"Once metallicity starts to increase, low- and intermediate-mass stars release carbon and massive stars start to eject more carbon than oxygen","Functions Label":0}
{"Functions Text":"Unlike LIGO\/Virgo, which can only detect merging BHBs in the final inspiral phase before merger, LISA will be able to detect eccentric stellar-mass BHBs for long timescales before they merge in the LIGO\/Virgo band (e.g.,","Functions Label":1}
{"Functions Text":"These have led to the discovery of metastable maser lines in 22 different regions","Functions Label":0}
{"Functions Text":"This is confirmed by the blind carbon monoxide (CO J = 1\u20130) survey of a subsample of the brightest 350 \u03bcm peakers (S350 \u2265 115 mJy), which has shown a strikingly similar redshift distribution as 850 \u03bcm selected SMGs (zCO = 2.5 \u00b1 0.8;","Functions Label":5}
{"Functions Text":"In order to check the effects of the morphological K-correction, we used publicly available HST\/ACS VF606W-band data over a 0.05 deg2 region in the COSMOS field from the CANDELS survey","Functions Label":2}
{"Functions Text":"For instance, a number of measurements have revealed that the stable isotopic compositions of all meteorites fall into two distinct families","Functions Label":0}
{"Functions Text":"Semiminor and semimajor axes of many 2FGL sources are derived with one order of magnitude higher uncertainties than those for Mrk 421 in the 2FGL catalogue","Functions Label":1}
{"Functions Text":"Perhaps a more likely possibility is that, even in this comparatively young source, the grains near the mid-plane, which dominate the total intensity, have already grown to sizes that exceed the maximum size $a_\\mathrm{max} = \\lambda \/2\\pi$ for producing polarized emission at wavelength \u03bb (e.g.","Functions Label":2}
{"Functions Text":"; for \u03bb = 1.25\u2009mm, amax = 0.2\u2009mm)","Functions Label":2}
{"Functions Text":"It has been shown that for mildly positive surface density gradients or negative entropy gradients, a positive corotation torque can eventually counteract the effect of a negative differential Lindblad torque, which may stall or even reverse migration","Functions Label":0}
{"Functions Text":"Continuum and methanol line maps from Effelsberg observations have also been obtained as part of the GLOSTAR survey","Functions Label":2}
{"Functions Text":"The bar, detected in the NIR by Quillen et al. (1997) and","Functions Label":0}
{"Functions Text":"shows a prominent boxy-shape morphology.","Functions Label":0}
{"Functions Text":"The inferred mass of the galaxy (baryons) in the best model (5.4\u2005\u00d7\u20051010 M\u2299) is marginally consistent with the estimated stellar mass derived from the velocity dispersion \u2013 stellar mass correlation","Functions Label":5}
{"Functions Text":"These new limits, in conjunction with the inconsistency of isotropic flux interpretations, leave no room for an astrophysical interpretation of AAEs in the context of the standard model for time windows as short as 103 s. However, it has been shown that these events can be explained using physics beyond the standard model, as many models suggest that AAEs lend support for axionic dark matter, sterile neutrinos, supersymmetry, or heavy dark matter","Functions Label":3}
{"Functions Text":"Many of these models,","Functions Label":3}
{"Functions Text":"can be constrained by this nonobservation at IceCube.","Functions Label":3}
{"Functions Text":"These simulations were tailored to the BHB system H1743\u2212332, where there is Chandra high-resolution data in both states giving detailed spectral information on the wind or its absence","Functions Label":2}
{"Functions Text":"The slopes solely inferred from the CARS data are consistent with those reported by Greene et al. (2012) and","Functions Label":5}
{"Functions Text":"and are therefore on the shallower side of previous estimates.","Functions Label":5}
{"Functions Text":"and Kitaura et al. (2012) proposed a Gibbs sampling scheme to jointly infer density and velocity fields and corresponding power-spectra.","Functions Label":0}
{"Functions Text":"However, these approaches assume matter density amplitudes to be log-normally distributed. The log-normal distribution reproduces one- and two-point statistics but fails to reproduce higher-order statistics associated with the filamentary dark matter distribution.","Functions Label":1}
{"Functions Text":"Hence, the main idea is to consider the object x as the sum of two components, namely x = xP + xE, where xP represents the point sources and xE the extended source. This approach was proposed for the first time in","Functions Label":2}
{"Functions Text":"assuming that the positions of the point sources are known.","Functions Label":2}
{"Functions Text":"Several ALMA blind surveys have been performed and allowed to detect and characterize the faint SMGs across cosmic times (e.g.,","Functions Label":0}
{"Functions Text":"One can see that the larger the initial amplitude, \u03c1IA, the stronger the decrease of the primary wave\u2019s amplitude, which is consistent with observations","Functions Label":5}
{"Functions Text":"The observed electron cigar distribution and the associated magnetic dip are a strong indication of the betatron cooling effect. This betatron-mediated cigar distribution has been suggested in previous studies","Functions Label":5}
{"Functions Text":"but never clearly observed. These observations, for the first time, show a direct link between the cigar distribution and betatron cooling.","Functions Label":5}
{"Functions Text":"Another model-independent method for distances to PNe are a cluster membership, as studied extensively by Majaess et al. (2007, 2014), and as discussed in","Functions Label":0}
{"Functions Text":"Similar deviations are observed in","Functions Label":5}
{"Functions Text":"outer parts of HSB spiral galaxies","Functions Label":5}
{"Functions Text":"A still slower rotating model","Functions Label":0}
{"Functions Text":"built large-scale, axisymmetric, cycling magnetic fields of somewhat lower amplitude which did not eliminate the star\u2019s differential rotation, reminiscent of the distributed \u03b1\u03a9-type dynamos prevalent in solar-like contexts.","Functions Label":0}
{"Functions Text":"kinetic instabilities such as the Buneman and modified two-stream instability (e.g.,","Functions Label":0}
{"Functions Text":"Lastly, post-AGB stellar evolution models, computed with updated physics in a reduced mass range","Functions Label":6}
{"Functions Text":"show a strong disagreement with the previous grids.","Functions Label":6}
{"Functions Text":"Starting from our completeness limit at 22 \u03bcm, after conservatively dereddening it by AV = 20, we assumed a spectral index \u03b3 = \u22122 (see Table 3 for definition) to compute the MIR luminosity from Eq. (6) of","Functions Label":2}
{"Functions Text":"From here on we present all the basic equations in the irreducible basis (see","Functions Label":2}
{"Functions Text":"for details).","Functions Label":2}
{"Functions Text":"The optical\/near-IR photometry was then complemented with the 24\u2009\u03bcm catalog","Functions Label":2}
{"Functions Text":", built as summarized in Section 2.1 from the Multi-Band Imaging Photometer for Spitzer (MIPS) images","Functions Label":2}
{"Functions Text":"Such a distance would make PSR\u2009J2043+2740 a viable target for deep optical observations, never carried out until now, and might be compatible with the debated association","Functions Label":3}
{"Functions Text":"Computing the exact pressure and temperature broadened Voigt profile for each of these lines is computationally extremely demanding. There are several approximate methods for computing Voigt profiles available in the literature (e.g.","Functions Label":0}
{"Functions Text":"Among the latter, Joudaki et al. (2018) recently performed a combined analysis of cosmic shear tomography, galaxy\u2013galaxy lensing tomography, and redshift space multipole power spectra using data from KiDS-450 (\u223c450\u2009deg2 of cosmic shear data from the KiDS survey) and two overlapping spectroscopic surveys, the 2-degree Field Lensing Survey4 (2dFLenS;","Functions Label":0}
{"Functions Text":"Previous studies have classified light bridges based on their morphological properties. Light bridges separating two umbral regions are called strong light bridges (e.g.,","Functions Label":0}
{"Functions Text":"Their brightness is similar to that of the penumbra, and they typically appear between two regions with the same polarity. Faint light bridges (e.g.,","Functions Label":0}
{"Functions Text":"are elongated bright structures that penetrate the umbra. They are composed of rows of bright grains with sizes comparable to umbral dots.","Functions Label":0}
{"Functions Text":"Following the method applied by","Functions Label":2}
{"Functions Text":"in their Eq. (2), we plot the relation between the LTE kinetic temperature, TLTE, and the para-H2CO (3\u20132) line ratio in Fig. 5.","Functions Label":2}
{"Functions Text":"The bulk SW shows a fractionation of elemental abundances correlating with FIP, as previously observed by spacecraft (e.g.,","Functions Label":5}
{"Functions Text":"However, the better accuracy and element coverage of Genesis data compared to in situ measurements allows further insights into this FIP-related fractionation.","Functions Label":1}
{"Functions Text":"Their numerical simulations were performed using the classical version of the Mercury code","Functions Label":3}
{"Functions Text":"which does not include general relativity (GR) effects and tidal interaction with the central star. They studied how the initial number of planets, the spatial separation between them, and the location of the inner planet influence the efficiencies of high-eccentricity mechanisms. As a result, they found that the Kozai\u2013Lidov mechanism plays the most important role in HJ production. The restriction made in the previous study, regarding not including the contribution of GR and realistic initial mass configurations (unequal masses), makes us wonder about the implications of these contributions on the efficiency of each high-eccentricity mechanism in the activation of the HJ production process.","Functions Label":3}
{"Functions Text":"Better agreement with observations can be obtained if freeze-out of O atoms onto dust grains is taken into account in gas-grain chemical models","Functions Label":3}
{"Functions Text":", with consequence surface production of H2O and O2, which may trap a significant fraction of oxygen, leaving only some atomic O and CO in the gas phase.","Functions Label":3}
{"Functions Text":"To create a single mock light curve, pseudo-random numbers are generated using the Fast Mersenne Twister SFMT19937 generator seeded with hardware-generated random numbers (generated using Intel RDRAND instruction) to ensure that the random number sequences are free of artificial correlations","Functions Label":2}
{"Functions Text":"induced by poor random seed choices.","Functions Label":2}
{"Functions Text":"The submm photometry of HATLAS12-00 at 890\u2009\u03bcm acquired with the Submillimeter Array (SMA) as part of this programme","Functions Label":5}
{"Functions Text":"is fully consistent with the 870\u2009\u03bcm and 850\u2009\u03bcm fluxes derived for this source from the LABOCA and SCUBA2 data to be presented here.","Functions Label":5}
{"Functions Text":"Historically, systematic studies of galactic outflows in nearby and high-z galaxies have focused on the ionized gas","Functions Label":0}
{"Functions Text":"and the atomic phase \u2013 based on the Na D or Mg II lines in absorption (e.g.","Functions Label":0}
{"Functions Text":"Relics trace ICM shock waves with relatively low (M\u2004 \u20043) Mach numbers","Functions Label":0}
{"Functions Text":"This assumption is inconsistent with our current understanding of the structure of MCs, which are known to be far from spherically symmetric, and instead consist of an intricate and inhomogeneous network of filaments and clumps within them (e.g.","Functions Label":6}
{"Functions Text":"In recent years, large-area optical surveys have detected candidate TDEs emitting at temperatures of a few \u00d7104 K","Functions Label":0}
{"Functions Text":"However, even with these degrees of freedom, the models still often fail to explain the abundances of certain individual species at the order-of-magnitude level (see, e.g.,","Functions Label":6}
{"Functions Text":", although they undoubtedly explain many of the observed abundance ratios.","Functions Label":5}
{"Functions Text":"A variety of other studies have reached the same conclusions, placing the combination of RP and photoionization of gas by massive stars as the dominant mechanism for disruption of molecular clouds and internal regulation of the SF process","Functions Label":0}
{"Functions Text":"as well as the best model using a Hernquist component for the stars and an NFW halo for the dark matter with and without adiabatic contraction, also from","Functions Label":2}
{"Functions Text":"More recent numerical and analytic models have continued in this vein (e.g.","Functions Label":0}
{"Functions Text":"rather than address the question of whether CRs represent a significant contribution to the support of the neutral material that dominates the total mass budget and occupies at least $\\sim 50{{\\ \\rm per\\ cent}}$ of the volume","Functions Label":0}
{"Functions Text":"near the mid-plane.","Functions Label":0}
{"Functions Text":"Previously, it has been argued that stars and BHs crossing the disk on low-inclination orbits get captured by Chandrasekhar dynamical friction into the disk","Functions Label":0}
{"Functions Text":"It was shown by","Functions Label":0}
{"Functions Text":"that this ridge structure is governed by the degree of oscillation modes and resembles the predictions made by Ando & Osaki (1975).","Functions Label":0}
{"Functions Text":"found that the number density of massive quiescent and elliptical galaxies with Re 2.5\u2009kpc decreases by about 30% from z~1 to z~0.2 and that their U\u2212V colours are consistent with passive evolution. They concluded that the driving mechanism for the average size-growth of the whole population is the appearance at later epochs of larger quiescent galaxies.","Functions Label":0}
{"Functions Text":"This is not typical for embedded clusters, which have typical half mass radii of \u223c0.8 pc","Functions Label":6}
{"Functions Text":", and therefore would have less frequent interactions between cluster stars and a particular binary.","Functions Label":6}
{"Functions Text":"Previous works have confirmed that H-atmosphere models accurately describe the spectra of qLMXBs, with radii in the range 10\u201315 km, as expected for NSs, either from single sources (e.g.","Functions Label":0}
{"Functions Text":"Alternatively, BBHs can form dynamically in","Functions Label":0}
{"Functions Text":"multiples (e.g.","Functions Label":0}
{"Functions Text":"Since in the experiment by","Functions Label":1}
{"Functions Text":"the ice was irradiated by VUV photons at the Lyman alpha wavelength, and we now know that methanimine can be efficiently ionized by those photons, we can also argue that ionization of several methanimine molecules can instead trigger the process in cold interstellar ices.","Functions Label":1}
{"Functions Text":"While most systems with exo-Kuiper belts do not have known planetary mass companions, in a few of these it has been possible to directly image one, thus enabling the study of planet\u2013disc interactions in more detail. There are well-known examples such as","Functions Label":0}
{"Functions Text":"and Fomalhaut having a narrow and eccentric planetesimal belt","Functions Label":0}
{"Functions Text":"Moreover, in recent years evidence has grown supporting the statement that GCs are generally composed of two or three chemically distinct populations. These subpopulations are separated by a few tens to hundreds of Myr in age and show vastly varying abundances of light elements such as C, N, O, Na, Mg, and Al (see, e.g.,","Functions Label":0}
{"Functions Text":"NGC 5813 itself has been assumed to be dynamically old","Functions Label":0}
{"Functions Text":"with no evidence of a recent major merger in its history, as indicated by the lack of any significant disturbances to its dusty circumnuclear disc","Functions Label":0}
{"Functions Text":"These values are in the range of those observed towards the molecular clouds in the Galactic centre but lower than in Orion KL","Functions Label":1}
{"Functions Text":"To come to a robust conclusion, independent H0 probes with accuracy better than $2{{\\ \\rm per\\ cent}}$ are crucial","Functions Label":3}
{"Functions Text":"The underlying cause of the split tracks (see","Functions Label":0}
{"Functions Text":"for a clustering analysis into the statistical robustness of this split) for BHXBs is not known","Functions Label":0}
{"Functions Text":"The retrograde x4 (stable) orbit family is also elongated perpendicular to the bar at small radii, but becomes rounder as it extends to larger radii (for detailed description of orbit families and how they are identified see","Functions Label":0}
{"Functions Text":"In the frame of reference rotating with the bar, all of these families are characterized by a 1:2 resonance between the tangential oscillation frequency (\u03a9\u03d5) and the radial or epicyclic frequency (\u03a9R).","Functions Label":0}
{"Functions Text":"The approximate rate of RETs (\u226510\u22126 Mpc\u22123\u2009yr\u22121","Functions Label":2}
{"Functions Text":"Such cores can be created within the CDM paradigm by a variety of baryonic processes (e.g.","Functions Label":0}
{"Functions Text":"However, on the other hand, understanding of the formation mechanism of massive stars is still elusive","Functions Label":0}
{"Functions Text":"Price et al. (2010) and","Functions Label":2}
{"Functions Text":"investigated the sizes of particles smaller than 10 \u03bcm that impacted the aluminum foils of the Stardust probe. The distribution peaks at about 175 nm, but if we assume that the particles areagglomerates of smaller subunits, as indicated by their common polymineralic nature, then the subunit size distribution would peak at sizes below 100 nm","Functions Label":2}
{"Functions Text":"while the models with higher He core masses are compatible with the typical kicks of young pulsars","Functions Label":1}
{"Functions Text":"A more realistic shock process, on the other hand, is most likely accompanied by radiative cooling to some degree in which the post-shock plasma temperature may stay comparatively as cool as that of the upstream one, as in the isothermal shocks (e.g.,","Functions Label":6}
{"Functions Text":"It has been pointed out that the widely used approximation for the vertical component of gravity, GMz\/R3, is only valid for the thin disk with H\/R \u226a 1, and a more accurate expression of vertical gravity should be adopted for a slim disk","Functions Label":1}
{"Functions Text":"Because they are detected in a wide variety of interstellar sources \u2013 in hot cores","Functions Label":3}
{"Functions Text":"it is of prime importance to understand well how these precursor molecules form.","Functions Label":3}
{"Functions Text":"The points mark detections from previous studies in the literature. References:","Functions Label":2}
{"Functions Text":"All relevant numerical routines were extracted from the\u202fLLMODELS stellar model atmosphere code","Functions Label":2}
{"Functions Text":"Nevertheless, the \u2018combined\u2019 bar fraction in Fig. 6 is not constant over (g \u2212r) colour and agrees well with","Functions Label":5}
{"Functions Text":"for redder colours [(g \u2212r) colour > 0.5]","Functions Label":5}
{"Functions Text":"The flux variability of the source rules out an X-ray supernova remnant and confirms that it is powered by accretion onto a compact object","Functions Label":1}
{"Functions Text":"As for the main isotopolog","Functions Label":2}
{"Functions Text":"we employed the RAM36 (rho-axis-method for 3- and 6-fold barriers) code that uses the RAM approach for the molecules with the C3v top attached to a molecular frame of Cs or C2v symmetry and having 3- or 6-fold barriers to internal rotation, respectively","Functions Label":2}
{"Functions Text":"Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S\u2009ii]\/H\u2009\u03b1 > 0.4\u20130.5","Functions Label":0}
{"Functions Text":"the stellar radius and Teff","Functions Label":0}
{"Functions Text":"In some galaxies, the depletion time in the centres appear shorter","Functions Label":0}
{"Functions Text":"In 2018, a new technique combining a Terahertz radiometer (41\u201349) GHz and a vacuum chamber was developed to observe the generation of cold plasma and UV photochemistry in the gas phase under low pressure as described by","Functions Label":0}
{"Functions Text":"However, in the context of the experiment described here, it is important to note that the spectrometer developments were not coupled to a system where the gas-phase molecules originated from the solid state.","Functions Label":6}
{"Functions Text":"Pebble accretion is a mechanism able to speed up significantly the giant planet formation process (i.e.,","Functions Label":0}
{"Functions Text":"A whole host of ions, atoms, and molecules have been detected through a variety of, often complementary, techniques, such as differential spectrophotometry using low-to-mid resolution spectroscopy (e.g.","Functions Label":0}
{"Functions Text":"Historically, models reproducing the evolution of stellar populations and dust emission have been developed separately,","Functions Label":0}
{"Functions Text":"and a thorough comprehension of dust grains physics on the other","Functions Label":0}
{"Functions Text":"Velocity dispersions in dwarf galaxies can be on the order of the rotational velocity, \u223c10\u201315 km s\u22121 (e.g.,","Functions Label":1}
{"Functions Text":"Orbiting SMBHBs produce a stochastic GW background (GWB","Functions Label":0}
{"Functions Text":"On the numerical side, van Wassenhove et al. (2010) consider different scenarios for formation of a black hole in Milky Way satellites and place the likelihood of one of them having a black hole around the size found here to be below 1%, but this result also depends on the initial seed mass (see also","Functions Label":1}
{"Functions Text":"In particular, an instrumental line (Cu K\u03b1) is known to affect pn at a rest-frame energy of ~8 keV","Functions Label":2}
{"Functions Text":"Despite our efforts to carefully estimate the background, that line might interfere with the Ni-K line in several observations, making a proper modelling of the Ni-K line impossible, and hence, boosting the Ni absolute abundance in pn.","Functions Label":2}
{"Functions Text":"Since then, these two methods have been widely used to explore the cosmic anisotropy","Functions Label":0}
{"Functions Text":"by investigating observational data of, for instance, the Union2.1 sample","Functions Label":0}
{"Functions Text":"Significant progress has been made in recent times through detailed full-quantum scattering calculations, based on quantum chemical data, for the cases of simple atoms such as Li, Na, Mg and Ca","Functions Label":0}
{"Functions Text":"The blue bump appears mainly due to the presence of late-type WN (WNL) and early-type WC (WCE) stars","Functions Label":0}
{"Functions Text":"The M-type sample consists of the non-Mira stars from the General Catalog of Variable Stars (GCVS;","Functions Label":2}
{"Functions Text":"with quality flag 3 in the IRAS 12, 25, and 60 \u03bcm bands and 60 \u03bcm flux \u22733 Jy","Functions Label":2}
{"Functions Text":"This model features a self-consistent treatment of the thermal, Compton scattering and the reflection component: ${\\tt {\\rm kerrbb2}}$ describes the thermal component and supplies the seed photons for ${\\tt{\\rm simplr}}$ (a modified version of ${\\tt{\\rm simpl}}$,","Functions Label":2}
{"Functions Text":"to generate the Compton component;","Functions Label":2}
{"Functions Text":"while the post-shock temperature in the hot halo near Rv may only be \u223c0.5Tv","Functions Label":2}
{"Functions Text":", P18).","Functions Label":2}
{"Functions Text":"It is worth noting that the original samples from","Functions Label":1}
{"Functions Text":"and Bernard-Salas et al. (2009) have spectra solely covering the central region of the galaxies.","Functions Label":1}
{"Functions Text":"The center-to-limb variations ofintensity I(\u03bcij) and polarization P(\u03bcij) were found through trilinear interpolation using the look-up tables from Kostogryz & Berdyugina (2015) and","Functions Label":2}
{"Functions Text":", according to the selected wavelength, surface gravity, and temperature of a star.","Functions Label":2}
{"Functions Text":"The Kamioka Gravitational Wave Detector","Functions Label":0}
{"Functions Text":"will be a 3-km-long underground interferometer in Japan capable of detecting the gravitational radiation emanating from collisions involving black holes with masses up to 200\u2009M\u2299","Functions Label":0}
{"Functions Text":"We then attempted to unify the data for each filter to a consistent zero point by using ensemble photometry","Functions Label":2}
{"Functions Text":"This essentially uses all measured stars on the frame to determine magnitude offsets resulting from differences in exposure time, airmass, atmospheric transparency, and the like. Our implementation iteratively fits for position-dependent corrections that result from variations from point-spread function across the frame.","Functions Label":0}
{"Functions Text":"Aa is itself composed of two spectroscopic components (Aa1+Aa2) in an eclipsing orbit with a5.7325 d period, while Ab is two magnitudes fainter than the two Aa components and located 0.\u2032\u2032 267 away in 1993 and moving away from the primary","Functions Label":0}
{"Functions Text":"We also plot the SFR in the outer regions of spiral galaxies","Functions Label":2}
{"Functions Text":"square symbols).","Functions Label":2}
{"Functions Text":"This unprecedented relation is likely the result of the observed link found between SF indicators such as radio, far-infrared, optical or line luminosities, and galaxy mass","Functions Label":2}
{"Functions Text":"Such shadows reveal that angular distortions are common in inner disks. This is consistent with the existence of a class of self-shadowed disks in which the inner disk scale height is higher than that of the outer disk, leading to a general shadowing and related cooling of the outer disk","Functions Label":5}
{"Functions Text":"The mass accretion and loss rates for Class 0\/I low-mass protostars span the range of 10\u22126\u201310\u22128 M\u2299 yr\u22121, and the derived jet efficiencies (ratio between mass ejection and accretion rates) range between \u223c1 per\u2009cent and 10 per\u2009cent (e.g.","Functions Label":0}
{"Functions Text":"These measurements are within the range predicted by the magnetohydrodynamic jet launching models","Functions Label":5}
{"Functions Text":"On larger scales or for measurements invoking substantial temporal and\/or spatial averaging, the distributions become gyrotropic but can still remain anisotropic, since isotropization may be slow. The corresponding RH should take into account this anisotropy","Functions Label":0}
{"Functions Text":"For example, shown in Figure 1 are the values of symmetry energy at 2\u03c10, that is, Esym(2\u03c10), from","Functions Label":2}
{"Functions Text":"(6)","Functions Label":2}
{"Functions Text":"analyses of NS radii, tidal deformability, and maximum mass within an extended Skyrme Hartree\u2013Fock approach (eSHF)","Functions Label":2}
{"Functions Text":"Despite the rather different assumptions and methods used in analyzing the different types of laboratory and observational data, it is very interesting to see that they all together are consistent with a fiducial value of Esym(2\u03c10) = 47 MeV within the still relatively large error bars of the individual analyses.","Functions Label":5}
{"Functions Text":"A second, fast path involves a downward transition in the mass\u2013size plane, at approximately constant redshift","Functions Label":0}
{"Functions Text":"This process requires a substantial \u201ccompaction\u201d of the formally extended star-forming galaxies.","Functions Label":0}
{"Functions Text":"In LTE, a linear dependence of the core\/wing ratio is expected (e.g.,","Functions Label":1}
{"Functions Text":"but such dependence is probably less obvious for the Mg ii h and k line, whose cores form in NLTE conditions.","Functions Label":1}
{"Functions Text":"Weaker solar cycles and advanced imaging and modeling capabilities have raised the profile of pseudostreamers and their boundaries as contributors to the outflows within this slow wind layer","Functions Label":3}
{"Functions Text":"Radio observations were provided by","Functions Label":2}
{"Functions Text":"and the High Energy Telescope","Functions Label":2}
{"Functions Text":"Plin represents the real-space, linear matter power spectrum for which we use the CLASS Boltzmann solver","Functions Label":2}
{"Functions Text":"When random pairing is used (i.e., binary companions are randomly chosen from a given IMF), we find similar mass segregation results to those for star clusters containing only single stars. However, random pairing is ruled out observationally, and there is also a lack of theoretical backing for a random pairing function","Functions Label":1}
{"Functions Text":"It has a (energy-dependent) angular size of \u223c0.1\u00b0 and its distance has been estimated to be \u22482.2\u2009kpc, corresponding to a physical size of \u22483.8\u2009pc","Functions Label":0}
{"Functions Text":"At large galactocentric radii (>10 kpc) this includes, among others,","Functions Label":0}
{"Functions Text":"and streams of stars kicked up from the disk that undergo phase mixing, sometimes referred to as \u201cfeathers\u201d (e.g.,","Functions Label":0}
{"Functions Text":"with a sample of 322 giants, including 10 planet-hosts, did not find any metallicity offset.","Functions Label":1}
{"Functions Text":"Bars in spiral galaxies may drive gas inflows, which enhance central star formation (bar-driven evolution;","Functions Label":0}
{"Functions Text":"found that CIR boundaries can be well defined when the total pressure exceeds 50 pPa (indicated by the horizontal dashed line in Fig. 2), which is slightly higher than that in the background solar wind, which typically is 20\u221230 pPa, according to Jian et al. (2006).","Functions Label":2}
{"Functions Text":"Within the classical MOND framework, the Newtonian gravitational acceleration gN is replaced in the spherically symmetric case by $g=\\sqrt{g_{\\rm {N}} a_0}$ when the gravitational acceleration is far smaller than the critical acceleration a0 = 1.2 \u00d7 10\u221210 m s\u22122","Functions Label":0}
{"Functions Text":"Different types of software, such as lenstronomy","Functions Label":0}
{"Functions Text":"can handle the inference of lensing quantities from mass maps using fast Fourier transform convolution.","Functions Label":0}
{"Functions Text":"As mentioned in Sect. 5.7, the 13CO\/C18O abundance ratio increases in regions of enhanced UV field","Functions Label":2}
{"Functions Text":"This category is similar to the \u2018uncertain\u2019 (UNC) class introduced in","Functions Label":5}
{"Functions Text":"that, based on the results of the 3DBarolo fits, contains sources they are unable to classify because of the low S\/N and\/or spectral resolution, or contrasting evidence in their classification criteria.","Functions Label":5}
{"Functions Text":"An additional goal of high-resolution observations for L1451-mm and the remaining youngest candidates should be to investigate the temperature and density profiles of the envelope at scales from few au to 100 au. This is because simulations show that the temperature remains lower than \u223c30 K even at several tens of au up to 100 au from the centre","Functions Label":7}
{"Functions Text":"The quality and breadth of these experiments are limited by the availability of computational resources and the fidelity of models for galaxy physics such as","Functions Label":3}
{"Functions Text":"It has only recently become widespread to model the formation of galaxies ab initio","Functions Label":3}
{"Functions Text":"and the realism continues to improve","Functions Label":3}
{"Functions Text":"It was the first source identified as a hot corino","Functions Label":0}
{"Functions Text":"based on the detection of Complex Organic Molecules (COMs) in the source, which was later supported by follow-up studies","Functions Label":0}
{"Functions Text":"In the case of pre-ELMVs,","Functions Label":0}
{"Functions Text":"and nonradial p- and g-mode pulsations","Functions Label":0}
{"Functions Text":"revealed that the excitation is probably due to the \u03ba\u2005\u2212\u2005\u03b3 mechanism, acting mainly in the zone of the second partial ionization of He, with a weaker contribution from the region of the first partial ionization of He and the partial ionization of H.","Functions Label":0}
{"Functions Text":"Surprisingly, we observe that this data reduction change was only applied to the Balmer \u03b2, \u03b3, and \u03b4 lines but not applied to the Balmer \u03b1 line. For the latter one, the original iterative spline interpolation scheme has been used all along. As a result, an absorption-like feature at the location of Balmer \u03b1 is found in SDSS data releases 9 up to now, i.e. the latest data release 14","Functions Label":1}
{"Functions Text":"It is more similar to the extremely low values of [14N\/15N] found in primitive solar system material, like cometary CN and HCN","Functions Label":5}
{"Functions Text":"More importantly, we showed that, as long as the archives are consistent with each other, for example, they are centred at the same wavelength and employing the same bandwidth for the observations, the method can be used to derive accurate information on the evolution of plage areas without the need of any adjustments in the processing of the various archives","Functions Label":0}
{"Functions Text":"Paper II, hereafter).","Functions Label":0}
{"Functions Text":"The energetic plasma in the vicinity of RFs plays a key role in connecting the magnetotail with the inner magnetosphere because they carry a large amount of energy and can be injected into the inner magnetosphere to affect the ring current and radiation belt","Functions Label":3}
{"Functions Text":"The most well-known stellar stream in this region is the Monoceros Ring (e.g.","Functions Label":0}
{"Functions Text":"while the baryon content is revealed by emission lines ranging from H and He lines in the optical through to highly ionized Fe lines in the X-rays","Functions Label":0}
{"Functions Text":"These values are consistent with the current observed SFR in the Milky Way","Functions Label":5}
{"Functions Text":"The tidal disruption probability of NSBH mergers and the brightness of NSBH EM signals are determined by the BH mass, BH spin, NS mass, and NS equation of state (EoS; e.g.","Functions Label":2}
{"Functions Text":"This UV-soft SED is regarded as more realistic for radio-quiet quasars than the other available SEDs provided by Cloudy (see the detailed discussion in Section 4.2 of","Functions Label":2}
{"Functions Text":"Usually, we see a decay in magnetic field strength as solar-type stars evolve, as their activity decreases along with their rotation","Functions Label":1}
{"Functions Text":"However, this subgiant star seems to have a relatively strong large-scale magnetic field compared to the Sun. The exact process through which this star would reach this stage in its evolution with such a magnetic field is yet unknown.","Functions Label":1}
{"Functions Text":"Theoretical works","Functions Label":2}
{"Functions Text":"showed that, in order to have a significant feedback impact in the environment surrounding an AGN, it is required a minimum ratio between the mechanical power of the outflow and the bolometric luminosity of ${\\sim}0.5{{\\ \\rm per\\ cent}}$.","Functions Label":2}
{"Functions Text":"Instead, the lower limits are below the minimum value required to generate at least a weak feedback. Considering only the values derived from the lower limits on the distance, i.e. the situation in which the X-ray winds are cospatial, we would be in a scenario in which the source loses much luminosity due to advection inside the disc, resulting in a much lower efficiency for wind production as most of the radiation remains trapped inside the disc.","Functions Label":2}
{"Functions Text":"For a sanity check, we estimate the bulge mass of NGC 3504 using our H-band MGE model and adapting the effective radius of the bulge derived from the bulge-disk-bar decomposition model","Functions Label":2}
{"Functions Text":"However, previous results show that fast CME would decelerate during their propagation in interplanetary space (e.g.,","Functions Label":1}
{"Functions Text":"Moreover, several molecules were detected and resolved toward NGC 1068 with interferometers in the past few years","Functions Label":0}
{"Functions Text":"The F\u03ba-test is preferred when the magnitude difference between the object and comparison stars is large","Functions Label":1}
{"Functions Text":"derived values of 0.15\u20130.25","Functions Label":2}
{"Functions Text":"The corresponding range is depicted in Fig. 6 by the horizontal bar shaded in blue. As thevolume filling factor is known, the laboratory measurements can be used to determine the most likely material of the surface.","Functions Label":2}
{"Functions Text":"are at the levels of >4\u03c3 for the analysis of","Functions Label":1}
{"Functions Text":"Multiple feedback mechanisms influence disc evolution. In sufficiently dense environments, star\u2013disc encounters can truncate the disc and induce increased accretion rates","Functions Label":0}
{"Functions Text":"Accordingly, numerous studies were focused on peak fluxes of SEPs and corresponding acceleration and transport processes (e.g.,","Functions Label":0}
{"Functions Text":"A process that constrains the outcoming radiation field to narrower angles may leave some room for the accretion process to continue in some directions. This seems to be the case for the outflows driven by young stars from a very broad mass range, as previous reported by several authors","Functions Label":1}
{"Functions Text":"VLA observations of the NH3 inversion lines (1,\u20091) and (2,\u20092) seen in absorption (1\\hbox{$\\farcs$}.\u030b1 beamsize) revealed radial infall on scales larger than 5000 AU toward the W51e2 core","Functions Label":0}
{"Functions Text":"The RXTE observed another outburst in 2002 and re-established its cyclotron resonance feature corresponding to a centroid energy at 30.7 \u00b1 1.8 keV (as established earlier by Ginga), which did not show a significant dependence on X-ray luminosity, although the continuum became harder with increasing source luminosity","Functions Label":1}
{"Functions Text":"QSO flux measurements that reach to z \u223c 7.5","Functions Label":0}
{"Functions Text":"the absorbed doses used in our fixed energy experiments change from ~ 2 to ~ 15 MGy, whichis quite similar to the absorbed doses in","Functions Label":5}
{"Functions Text":"In the linear perturbation theory limit of the MHD equations, \u03b4B2 includes contributions from shear Alfv\u00e9n, fast and slow magnetosonic compressive eigenmodes (e.g.","Functions Label":2}
{"Functions Text":"We do detect starburst-like behaviors in galaxies on the main sequence","Functions Label":1}
{"Functions Text":"likely linked to the existence of transitional objects","Functions Label":1}
{"Functions Text":"to limit the references to recent works based on submillimeter observations","Functions Label":1}
{"Functions Text":"However, implementation of these models is complex and a large library is needed to model all galaxies properties. Instead, numerous studies have used simple analytical forms to model galaxies SFH (e.g.,","Functions Label":0}
{"Functions Text":"This limit is referred to as the quasi-static approximation to MHD","Functions Label":0}
{"Functions Text":"although recent numerical studies on its turbulent properties and anisotropy have been done as well","Functions Label":0}
{"Functions Text":"Reconstruction techniques are divided into two classes, although this distinction is by no means unique or even consistent in some cases. Parametric techniques (e.g.","Functions Label":0}
{"Functions Text":"assume a parametric form of the underlying mass density distribution for the lens and typically make the assumption that light traces mass in the positioning of these parametric forms.","Functions Label":0}
{"Functions Text":"In particular, the Magnetospheric Multiscale (MMS) mission has contributed greatly to the kinetic physics of magnetopause reconnection","Functions Label":0}
{"Functions Text":"see fig. 1 of","Functions Label":0}
{"Functions Text":"With the remarkable progress in scientific computing, their rotating magnetosphere has captured designers of numerical methods that integrate FFE and magnetohydrodynamics (MHD) with ever-improving accuracy (e.g.","Functions Label":0}
{"Functions Text":"Presently, although we still know little about rotation velocities of massive stars and their variation with environment, observations seem to favor fast rotators at low Z (e.g.","Functions Label":0}
{"Functions Text":"The possible change of macroscopic magnetic moment of pulsars at the moment of a glitch occurring was discussed by Link and Epstein","Functions Label":0}
{"Functions Text":"We use the same normalization","Functions Label":2}
{"Functions Text":"where time, radius and velocity are normalized to the outer radius a, the resistive diffusion time \u03c4R = a2\/\u03bc0\u03b7, and the Alfv\u00e9n velocity $V_{\\rm A} = B_0\/\\sqrt{\\mu _0 \\rho _0}$, respectively.","Functions Label":2}
{"Functions Text":"As of today, many more mass ejection channels have been discussed:","Functions Label":0}
{"Functions Text":"as MHD-driven winds","Functions Label":0}
{"Functions Text":"Unfortunately, the previous work does not cover all the phase angles of the images we investigated, but the spectral slope variation between 35\u201354\u00b0 (Fig. 3 of","Functions Label":1}
{"Functions Text":"is small so that we can make this comparison. However, if we follow the linear trend of the phase reddening, for the image taken in 70.45\u00b0 phase angle (image #4), the spectral slopes would vary from 15%\/100 nm to 18%\/100 nm in the observations we used.","Functions Label":1}
{"Functions Text":"Most of the known metal-poor stars have been found in dedicated surveys, such as objective prism surveys (the HK survey and Hamburg-ESO survey","Functions Label":0}
{"Functions Text":"These motivated an effort to measure the neutron star radius using the burst continuum spectrum, where the normalization of the burst blackbody is expected to be proportional to the square of the stellar radius (e.g.,","Functions Label":0}
{"Functions Text":"A contact binary could result from","Functions Label":1}
{"Functions Text":"(ii) the disruption of a monolithic object due to excessive spin-up resulting from non-gravitational forces or YORP5 effect followed by a reaccretion","Functions Label":1}
{"Functions Text":"If the pairs are produced via TeV\u2013eV collisions (i.e., via the second path) outside the gap outer boundary, they have outward ultrarelativistic momenta to easily \u201cclimb up the hill\u201d of the potential k0","Functions Label":1}
{"Functions Text":"see also Figure 2 of HP16) and propagate to large distances without turning back.","Functions Label":1}
{"Functions Text":"Considering that the relation between the gas temperature and the para-H2CO line ratio may vary at different spatial densities (see Fig. 2 in","Functions Label":2}
{"Functions Text":"we modeled it at spatial densities 104, 105, and 106 cm\u22123 in Fig. 5.","Functions Label":2}
{"Functions Text":"Moreover, the Te problem can also be originated due to the use of an unappropriate calculation of the ionization correction factor (ICF) for oxygen in AGNs","Functions Label":1}
{"Functions Text":"The models for galaxy formation include physical processes such as gas heating by a spatially uniform and time-dependent UV background, primordial and metal-line gas cooling, a subgrid model for star formation, and the unresolved structure of the interstellar medium","Functions Label":2}
{"Functions Text":"The blue squares are data from the GAMA galaxy survey","Functions Label":2}
{"Functions Text":"We probed four orientations for the simulated outflows","Functions Label":2}
{"Functions Text":"the jet direction claimed by","Functions Label":2}
{"Functions Text":"For a few very nearby (100 Mpc) quiescent galaxies, including our Galaxy, SMBH masses can be measured through the stellar or gaseous dynamics method (e.g.","Functions Label":0}
{"Functions Text":"Because it is difficult to determine the cut-off energy from our data, we fix it at 300 keV, which is a typical value measured in nearby AGNs","Functions Label":2}
{"Functions Text":"For example, the enhanced close binary fraction of metal-poor solar-type stars substantially strengthens the conclusion that the shaping of PN morphologies is the result of binary interactions","Functions Label":5}
{"Functions Text":"When the magnetic field lines are parallel it is not easy to have reconnection","Functions Label":2}
{"Functions Text":"Hereafter, we adopt natural units c = \u210f = 1. have been reported (see, e.g.,","Functions Label":2}
{"Functions Text":"There remains much debate in the literature on the origin of such axisymmetric substructure in protoplanetary disks including","Functions Label":3}
{"Functions Text":"and toroidal dust traps created by hydrodynamic or magnetohydrodynamic effects (see, e.g.,","Functions Label":3}
{"Functions Text":"The existence of an early ocean is supported by","Functions Label":0}
{"Functions Text":"and from records of the oxygen isotope composition of seawater","Functions Label":0}
{"Functions Text":"However,","Functions Label":0}
{"Functions Text":"also saw highly structured material most probably originating from a prominence in 63% of CMEs associated with eruptive prominences at the limb observed in visible light using the broadband filter (\u03bb\u03bb 5000\u22125350\u2009\u00c5).","Functions Label":0}
{"Functions Text":"Although such observations are called as white light in literature, it would be better to consider them as observations in visible light, because naturally integral intensities in the visible spectral range are observed including both continuum and absorption lines, while white light is just a continuum caused by Thomson scattering on free electrons without the lines.","Functions Label":1}
{"Functions Text":"This cluster has about solar metallicity ([Fe\/H] in the range \u22120.04 to +0.03, e.g.","Functions Label":3}
{"Functions Text":"Nevertheless, it still faces numerous challenges on galaxy scales. Among these, the most important ones are","Functions Label":0}
{"Functions Text":"or the unexpected diversity of rotation curve shapes at a given mass scale","Functions Label":0}
{"Functions Text":"While the PHIBSS project estimated molecular gas masses by measuring the CO(3\u20132) line emission","Functions Label":1}
{"Functions Text":"Scoville et al. (2016, 2017) used the flux on the Rayleigh\u2013Jeans tail of the dust continuum emission to estimate the total gas masses.","Functions Label":1}
{"Functions Text":"Complementing these observations, the spectroscopic confirmation","Functions Label":0}
{"Functions Text":"of over a dozen sources has seen impressive advances with ground-based spectroscopy (e.g., probing the rest-frame UV and FIR with Keck\/MOSFIRE, VLT\/X-Shooter, and ALMA), particularly for the brightest and rarest objects.","Functions Label":0}
{"Functions Text":"This is quite a difficult measurement to do in observations as light profile fitting is required, which can be robustly done in very disc- and bulge-dominated galaxies, but when both components contribute similarly, the measurement is less robust","Functions Label":3}
{"Functions Text":"Set II: we now focus on the observational constraints on the model parameters after the inclusion of the local measurement of H0 by","Functions Label":2}
{"Functions Text":"with the previous data sets (CMB, Pantheon, and CC) in order to see how the parameters could be improved with the inclusion of this data point.","Functions Label":2}
{"Functions Text":"When the relative fraction of RC stars is taken into account (27%; see Section 4), the difference in [Na\/Fe] between the genuine RC stars would correspond to \u0394[Na\/Fe] \u223c 0.20 dex, which is comparable to that expected from our chemical evolution model for the bulge stars (\u0394[Na\/Fe] = 0.2 \u223c 0.3 dex;","Functions Label":5}
{"Functions Text":"As an example, it has been known for several decades that the Galactic disc contains large-scale non-axisymmetric features, including","Functions Label":0}
{"Functions Text":"a warp","Functions Label":0}
{"Functions Text":"In low radio states, it has also displayed evidence of a high-ionization X-ray-absorbing wind","Functions Label":0}
{"Functions Text":"estimated with NEXAFS spectroscopy (at the C K-edge) that X-ray irradiation at 150 eV of pure methanol ice at 20 K leads to a survival rate of 50% for methanol after an absorbed dose of 1.1 MGy.","Functions Label":2}
{"Functions Text":"However, the complexity of such simulations obscures the physical mechanisms through which these processes affect the dark matter distribution. These mechanisms normally invoke \u2018heating\u2019 of the cold central density cusp through an irreversible process, such as dynamical friction from infalling clumps","Functions Label":0}
{"Functions Text":"In the jet model, such a p can also reasonably account for the very late flux decline of","Functions Label":2}
{"Functions Text":"While this parameter space is inhabited by Uranus and Neptune in the Solar system, which should thus readily supply objects to the Oort Cloud (even accounting for the possibility that these planets may have started closer to the Sun;","Functions Label":1}
{"Functions Text":"it could be that Oort Clouds are relatively rare.","Functions Label":1}
{"Functions Text":"The first possible scenario is that all FRBs are generated from magnetars, the population of non-repeating FRBs are from magnetars born in the delay formation channels","Functions Label":0}
{"Functions Text":"or white dwarf\u2212white dwarf mergers","Functions Label":0}
{"Functions Text":"This result strengthens the notion that metallicity may not play an important role in deciding theresulting SN type, in agreement with other works based on SN environments","Functions Label":5}
{"Functions Text":"Absorption band shifts of CO ice in the UV and IR ranges only occurred at deposition temperatures above 20\u2009K","Functions Label":0}
{"Functions Text":"suggesting that CO ice grown at lower temperatures is amorphous below 20\u2009K in our experiments, and therefore, the decreasing photodesorption yield is not related to a transition from amorphous to crystalline ice, instead it might be associated to a different degree of molecular disorder in CO ice samples, depending on their deposition temperature.","Functions Label":1}
{"Functions Text":"One is evaluated from the best-fit model, and one weights all models allowed by the parametric grid, with the best-fit model having the heaviest weight","Functions Label":2}
{"Functions Text":"In the seminal work of BPS","Functions Label":0}
{"Functions Text":"the nuclear masses for the outer crust were provided by an early semi-empirical mass table.","Functions Label":0}
{"Functions Text":"The corresponding EoS is seen to display a similar pattern with the BCPM, FRDM, and BSk21 results in Fig. 2.","Functions Label":5}
{"Functions Text":"These soft residuals are known to be a common feature in the spectra of ULXs and bright X-ray binaries","Functions Label":5}
{"Functions Text":"and found in other ULXs to be a combination of emission and absorption features related to powerful outflowing winds (including in NGC 6946 ULX-3;","Functions Label":5}
{"Functions Text":"Modelling of DLAs observations suggests that DLAs resemble rotating disc galaxies with circular velocities typically of the order of $100\\!-\\!200\\, {\\rm km\\, s}^{-1}$","Functions Label":0}
{"Functions Text":"Findings by","Functions Label":6}
{"Functions Text":", on the other hand, show that the (nh\u2005+\u2005ns)\/nc ratio remains roughly constant with heliocentric distance in the slow wind, suggesting a lack of interchange between the thermal and suprathermal populations.","Functions Label":6}
{"Functions Text":"These three protostars are all embedded in dense cores with masses \u22730.5 M\u2299","Functions Label":3}
{"Functions Text":"Therefore, they are excellent targets by which to study the gas motions on a 100 au scale at an early evolutionary stage.","Functions Label":3}
{"Functions Text":"In observed spectra, recurrent frequency spacings that may correspond to the large separation or half its value have been found in some stars","Functions Label":0}
{"Functions Text":"Comparisons of the two methods show quite good agreement and reasonable agreement with the full quantum calculations is found, particularly for the most important processes with the largest rates","Functions Label":5}
{"Functions Text":"However, our result is consistent with other NLFFF results","Functions Label":5}
{"Functions Text":"The composite SED was reddened according to the new family of optical and near-infrared extinction laws for O-type stars provided by Ma\u00edz Apell\u00e1niz et al. (2014), which constitute an improvement of the widely used extinction laws by","Functions Label":2}
{"Functions Text":"For instance, thioformic acid (HC(O)SH) was very recently detected in G+0.693\u20130.027. Its trans-isomer has an abundance of ~1 \u00d7 10\u201310","Functions Label":0}
{"Functions Text":"Studies showed that the majority of the optically visible Galactic post-AGB stars could be classified based on their spectral energy distributions (SEDs) into two groups: shell-sources and disc-sources","Functions Label":0}
{"Functions Text":"Studies suggest that this valley likely marks the transition from the smaller rocky planets: \u2018super-Earths\u2019, to planets with significant H\/He envelopes typically containing a few per cent of the planet\u2019s total mass: \u2018sub-Neptunes\u2019 (e.g.","Functions Label":0}
{"Functions Text":"Spacecraft observations show that wave potential structures of Gaussian form are common in space and astrophysical plasmas","Functions Label":2}
{"Functions Text":"We assume this potential well to have Gaussian form","Functions Label":2}
{"Functions Text":"Super-Earths can be found with either high-precision RV observations or space-based transit searches. Such high-precision RV surveys include those being undertaken currently with HARPS (e.g.,","Functions Label":0}
{"Functions Text":"The signature of flare QPPs can be detected in flare light curves across a broad band of the electromagnetic spectrum, i.e., radio\/microwave emissions","Functions Label":0}
{"Functions Text":"For cometary nuclei, the primary cause for spin-up is torques caused by outgassing, therefore it is possible that 8P\/Tuttle formed as a monolithic body and became a contact binary after its injection into the inner Solar System as a result of excessive spin-up resulting from non-gravitational forces. This scenario has been proposed for comet 67P\/Churyumov-Gerasimenko by","Functions Label":1}
{"Functions Text":"Such transition might well imply an imminent increase of the SFR, driving the object in the realm of starbursts","Functions Label":1}
{"Functions Text":"or its cessation, bringing the system back onto or even below the main sequence","Functions Label":1}
{"Functions Text":"with the CO properties potentially able to distinguish between these two scenarios.","Functions Label":7}
{"Functions Text":"The complex dielectric functions of the samples obtained by heating bayerite and boehmite to various temperatures","Functions Label":2}
{"Functions Text":"were derived by modeling the reflectance spectra of pellets obtained by pressing powders of these materials under great pressure","Functions Label":2}
{"Functions Text":"The avoidance of its going into CE evolution is \u2013 as we will argue \u2013 a consequence of the donor star having a radiative envelope","Functions Label":2}
{"Functions Text":"In such a case, when the emission beam is confined by dipolar open field lines, we would expect a P\u2212 1 \/ 2 dependence, which has indeed been observed when correcting for geometrical effects by transforming the pulse width into a beam radius measurement (see","Functions Label":1}
{"Functions Text":"This effect has been considered in numerical models of GCR modulation to study the long-term modulation mechanism (e.g.,","Functions Label":0}
{"Functions Text":"Over the past decades, much effort has been devoted toward constructing such global NLTE, steady-state model atmospheres of hot stars with winds; several numerical computer codes meanwhile exist on the market, for example","Functions Label":0}
{"Functions Text":"POWR","Functions Label":0}
{"Functions Text":"This is not an ideal approach: the momentum imparted on the SMBH from the swallowed gas particle may artificially dislodge it from its position, particularly without instantaneous repositioning (as also discussed by","Functions Label":1}
{"Functions Text":"However, even in ellipticals, large differences prevail. Recent observations of elliptical galaxies with Spitzer and Herschel","Functions Label":0}
{"Functions Text":"have revealed that the far-infrared (FIR) luminosity LFIR from these galaxies can vary by \u223c100 among galaxies with similar optical luminosity.","Functions Label":0}
{"Functions Text":"Some of these bursts are still not well understood. This is a case of the slowly positively drifting bursts (SPDBs). They appear in groups or as single bursts, with a duration of an individual burst from 1 to several seconds and their frequency drift is lower than about 100 MHz s\u22121","Functions Label":0}
{"Functions Text":"Such a distribution is believed to be related to the mass of the hydrogen envelope maintained by the progenitor stars, as evidenced by the results that SNe having larger envelope masses produce light curves with shallower plateau slopes and longer plateau durations","Functions Label":3}
{"Functions Text":"Several explanations about their origin have been put forth. Among these theories, interchange reconnection is the most focused upon","Functions Label":0}
{"Functions Text":"In this scenario, switchbacks are generated in the solar corona, and form at the reconnection sites between open and closed magnetic fluxes.","Functions Label":0}
{"Functions Text":"However, more recent studies","Functions Label":1}
{"Functions Text":"have revealed small non-mass-dependent variations in Fe isotopes.","Functions Label":1}
{"Functions Text":"This relation has been further extended to high redshifts, using deep near-infrared (IR) spectroscopy facilitated by large ground-based and space-based telescopes","Functions Label":0}
{"Functions Text":"The early X-ray afterglows are usually dominated by erratic X-ray flares and the tail emission of prompt gamma-rays are due to the arrival time delay of photons in the high latitude of the radiating fireball","Functions Label":0}
{"Functions Text":"Toward this goal, conventionally, new summary statistics that can only be measured with imaging have been proposed. These include","Functions Label":0}
{"Functions Text":"bispectrum","Functions Label":0}
{"Functions Text":"The [C\u2009ii]158\u2009\u03bcm line is typically the brightest in star-forming galaxies, arising from ionized, and even neutral gas where it is the main coolant","Functions Label":0}
{"Functions Text":"In addition, an intermediate-mass black hole (IMBH) in a cluster core will act as a strong central energy source able to delay, or even prevent, core collapse (e.g.","Functions Label":0}
{"Functions Text":"Moreover, it was found that the highest dust temperature at which H2 can be formed efficiently is less than 17\u2009K","Functions Label":0}
{"Functions Text":"and through diffusive flux","Functions Label":0}
{"Functions Text":"Recently, magnetic fields have been unambiguously detected via Zeeman signatures in a large sample of single G-K giants observed with the spectropolatimeters TBL\/Narval and CFHT\/ESPaDOnS","Functions Label":0}
{"Functions Text":"Gravitational lensing allows for constraints to be placed on the dark matter substructure content of external galaxies, as orbiting sub-haloes will result in anomalies in strong gravitational lenses","Functions Label":3}
{"Functions Text":"Whilst this higher total disc mass is still consistent with the dust mass measurements of protoplanetary discs","Functions Label":1}
{"Functions Text":"high debris disc masses, i.e. those in the range of $100\\!-\\!1000\\, M_{\\oplus }$, become problematic since these would require a very high efficiency of primordial dust being incorporated into these larger planetesimals (an example of the so-called \u2018disc mass problem\u2019, see","Functions Label":1}
{"Functions Text":"The (CH2OH)2\/CH2OHCHO abundance ratio of ~0.3\u20130.5 previously derived in IRAS 16293 by","Functions Label":6}
{"Functions Text":"was revised.","Functions Label":6}
{"Functions Text":"Some studies find weak statistical links among AGN activity and the presence of bars (e.g.,","Functions Label":0}
{"Functions Text":"An exponential rise\/decay model can appropriately fit the blazar light curve, which generally consists of superpositions of a steady background flux density and a number of flare components caused by events in the jet or the accretion disc\/corona region (e.g.","Functions Label":2}
{"Functions Text":"BALQSOs are classified into three sub-classes based on the ionization state of the absorbing gas: (a) high-ionization BALQSOs (HiBALs) consist of absorption from high-ionization lines such as C iv, Si iv, and N v","Functions Label":0}
{"Functions Text":"The sample used in this paper is primarily drawn from Sloan Lens ACS Survey (SLACS)","Functions Label":2}
{"Functions Text":"The combined sample includes 91 lenses from SLACS","Functions Label":2}
{"Functions Text":"Using Ks-band (2.15 \u03bcm) direct imaging andH-band (1.65 \u03bcm) polarimetric imaging with the High-Contrast Instrument with Adaptive Optics (HiCIAO) at the Subaru Telescope,","Functions Label":0}
{"Functions Text":"detected two spiral arms and polarized light down to 0.\u2032\u2032 1 (15 au) from the star.","Functions Label":0}
{"Functions Text":"Second, the mass distributions of single and binary sdB stars are indistinguishable (","Functions Label":3}
{"Functions Text":", Table 3 in particular).","Functions Label":3}
{"Functions Text":"The choice of SED is very important in the BLR modeling, as different lines respond to the continuum variations on different time scales","Functions Label":3}
{"Functions Text":"Previous sub-arcsecond angular resolution N-band (\u223c8\u201313 \u03bcm) ground-based spectroscopic studies investigated the 11.3 \u03bcm PAH feature in the nuclear and circumnuclear regions of AGN (e.g.,","Functions Label":0}
{"Functions Text":"However, these works were unable to provide definitive details regarding the effect of the AGN on the PAH molecules due to limited wavelength coverage and sensitivity.","Functions Label":3}
{"Functions Text":"we estimated several dynamical properties of the clusters in the point source sample and compared them with the extent-selected sample presented in","Functions Label":2}
{"Functions Text":"Between the end of inflation at t = te \u223c 10\u221233\u2009s; (e.g.","Functions Label":0}
{"Functions Text":"and t = teq = 2.37 \u00d7 1012 s, the Universe was radiation-dominated since at the latter instant a radiation-matter equality is reached (Table 1).","Functions Label":0}
{"Functions Text":"Furthermore, discoveries of atmospheric chemical species allow us to better understand various thermodynamical processes and chemistry, winds in the upper atmosphere","Functions Label":0}
{"Functions Text":"The observations of NGC 1333 IRAS4A and IRAS16293 are presented in Girart et al. (2006) and","Functions Label":0}
{"Functions Text":"respectively.","Functions Label":0}
{"Functions Text":"Together, these properties lead to the result that an ANN can be trained to provide accurate and practical solutions to Newton\u2019s laws of motion, resulting in major improvements in computational economy","Functions Label":3}
{"Functions Text":"relative to modern technologies.","Functions Label":3}
{"Functions Text":"There are various observations of flux ropes in the","Functions Label":0}
{"Functions Text":"and solar wind (e.g.,","Functions Label":0}
{"Functions Text":"At 8.7 GHz we find a PA of 25\u00b0 \u00b1 5\u00b0 at about 5 mas from the core, consistent with the archival VLBA monitoring results at 15 GHz, showing a persistent jet orientation at a PA of about 30\u00b0 in the epochs from 1995 to 2013 at angular scales \u223c5 mas","Functions Label":1}
{"Functions Text":"Magnetic field fluctuations have been characterized with great detail at magnetohydrodynamic and kinetic scales, for example, through spectral and high-order moments analysis","Functions Label":0}
{"Functions Text":"Besides the GRB 170817A\/AT 2017gfo event, searches for possible kilonova emission have already been carried out in the afterglows of many SGRBs since 2013","Functions Label":0}
{"Functions Text":"The large scale outflow is observed in CO emission at millimeter wavelengths, with both the red and blue lobes being about 100\u2033 in extent","Functions Label":0}
{"Functions Text":"In this very region, the analysis of heliospheric imaging (HI;","Functions Label":0}
{"Functions Text":"has described a transition from striated images that appear to be highly collimated due to a structured magnetic field and lower plasma beta to higher altitude images that appeared to be more disordered and isotropic, a condition described as \u201cflocculation.\u201d","Functions Label":0}
{"Functions Text":"Such a massive secondary black hole would require the Milky Way to have experienced a major merger relatively recently, which is excluded by observations (see","Functions Label":0}
{"Functions Text":"Those cavities have been suggested to exist at \u223cpc scales at least for XTE J1550\u2013564 and H1743\u2013322","Functions Label":2}
{"Functions Text":"Compared with other short GRBs, the luminosity of GRB 170817A was extremely weak, thus suggesting that the jet was off-axis to the line of sight","Functions Label":1}
{"Functions Text":"There are a variety of theoretical works related to the damping of the coronal loop oscillations based on the theory of resonant absorption of MHD waves (e.g.,","Functions Label":0}
{"Functions Text":"Alternatively, small dense structures can be temporary density fluctuations frequently created and destroyed by supersonic turbulence (e.g.,","Functions Label":0}
{"Functions Text":"We note that some of our data fits the observational findings of","Functions Label":5}
{"Functions Text":"represented by diamonds over-plotted on the power spectra","Functions Label":2}
{"Functions Text":"The agreement of the theory with the observational data indicates that the results can be used to determine the background structure of the solar atmosphere and confirms that wave generation by the solar granulation in the partially ionized plasma dominates the behavior of the waves.","Functions Label":1}
{"Functions Text":"In the absence of QED vacuum polarization effects, this would produce a drastic depolarization of the radiation collected at infinity","Functions Label":0}
{"Functions Text":"see also","Functions Label":0}
{"Functions Text":"This could stem from the fact that the galaxies studied by Holt et al. (2011),","Functions Label":1}
{"Functions Text":"are local luminous or ultra-luminous infrared galaxies (U\/LIRGs), and those of Villar Mart\u00edn et al. (2014, 2015) are highly obscured Seyfert 2, thus sampling sources that are more gas and dust rich compared to our sample.","Functions Label":1}
{"Functions Text":"We do detect starburst-like behaviors in galaxies on the main sequence","Functions Label":1}
{"Functions Text":"likely linked to the existence of transitional objects","Functions Label":1}
{"Functions Text":"Eventually Philippov & Spitkovsky (2014) computed the first two-dimensional axisymmetric pulsar magnetosphere for an aligned rotator by permanently injecting particle supposed to be released from the surface, avoiding to end to an electrosphere configuration","Functions Label":0}
{"Functions Text":"This chemical scheme was implemented in a chemical model by","Functions Label":0}
{"Functions Text":"to explain the abundance of cyanoallene in TMC-1.","Functions Label":0}
{"Functions Text":"The soft X-ray region of the reflection spectrum is also the most sensitive to modelling assumptions such as vertical disc structure","Functions Label":1}
{"Functions Text":"The in situ formation of the compact blobs is further supported by their metallicity. In fact, while the disc properties are consistent with the stellar mass\u2013metallicity relation of z \u223c 2 star-forming galaxies (e.g.","Functions Label":5}
{"Functions Text":"compact blobs instead show metallicities inconsistent with the mass\u2013metallicity relation (Fig. 7, bottom right panel).","Functions Label":6}
{"Functions Text":"However, the mean length for QS network jets is smaller (3.53 Mm;","Functions Label":1}
{"Functions Text":"Because of the potential diffuse nature of the excited states, their wavefunctions were calculated using a large basis set composed by the aug-cc-pVQZ quality, which is augmented by 3s and 2p diffuse Gaussian-type orbitals (GTOs;","Functions Label":2}
{"Functions Text":"Figure 5 shows the comparison between our EWs measurements and the line strengths measured by","Functions Label":1}
{"Functions Text":"(in both cases the sum of the two strongest lines) for the five calibration clusters.","Functions Label":1}
{"Functions Text":"The observed scatter is consistent with the internal errors of the EW measurements,","Functions Label":5}
{"Functions Text":"Note that any changes in the nearly flat potential will eventually lead to certain features in the spectrum. Local glitches in the potential including rapid change of its amplitude, or the break in its first or second derivatives","Functions Label":3}
{"Functions Text":"all lead to local and non-local oscillations in the spectrum.","Functions Label":3}
{"Functions Text":"Locally, less than 5% of the galaxy population has a star formation rate (SFR) that is significantly higher than the empirical main sequence for star-forming galaxies, i.e., the tight correlation (\u223c0.3 dex) between the SFR and stellar mass, M\u22c6","Functions Label":0}
{"Functions Text":"In a shearing disc, if the cells adapt in a truly Lagrangian manner, then they are inevitably deformed into a highly sheared\/irregular shape","Functions Label":1}
{"Functions Text":"Several strong processes have been proposed and observed, such as harassment (e.g.","Functions Label":0}
{"Functions Text":"Both giant HII regions are projected on the contour of a giant bubble-shaped structure, outlined in the distribution of HI and CO emission as first noted by","Functions Label":0}
{"Functions Text":"noted the presence of O and early B stars in the area and proposed that they were part of a massive star population responsible for having caused the bubble, but a review of their properties shows them to be generally too bright to be at the distance of the bubble and the giant HII regions, and instead are more likely members of a foreground population.","Functions Label":1}
{"Functions Text":"If the cirrus ISM component heated by the more general galactic UV radiation field contributes to LIR, then the","Functions Label":1}
{"Functions Text":"relationship overestimates the SFR.","Functions Label":1}
{"Functions Text":"We then remove the cosmic rays using the LACosmic algorithm","Functions Label":2}
{"Functions Text":"However, sensitivity and resolution limitations severely reduce the effectiveness of the past and present generations of radio and X-ray searches for SNRs in galaxies beyond the Small and Large Magellanic Clouds (MCs)","Functions Label":0}
{"Functions Text":"These slopes essentially provide information on the relative amount of structure as a function of spatial scale and can be compared with theoretical models of turbulence (mainly numerical simulations) to characterize turbulence cascade (e.g.,","Functions Label":0}
{"Functions Text":"Two orange peaks represent the cool lines of O\u202fI 1354.60 \u00c5 and C\u202fI 1354.84 \u00c5","Functions Label":2}
{"Functions Text":"which are far away from the flaring line of Fe\u202fXXI 1354.08 \u00c5.","Functions Label":2}
{"Functions Text":"A CO spectroscopic redshift of 3.26 was first suggested by Z-spec","Functions Label":5}
{"Functions Text":"observations, then subsequently confirmed by observations","Functions Label":5}
{"Functions Text":"and the Zpectrometer instrument","Functions Label":5}
{"Functions Text":"on the Greenbank Telescope","Functions Label":5}
{"Functions Text":"The most stringent and precise constraints on the self-interaction cross-section have been put on the scales of galaxy clusters (e.g.","Functions Label":1}
{"Functions Text":"where observations require that $\\sigma _T\/m_chi \\lesssim 1\\, {\\rm cm^2g^{-1}}$.","Functions Label":1}
{"Functions Text":"This form of joint analysis is already being explored within the framework of WMAP","Functions Label":0}
{"Functions Text":"and LiteBIRD","Functions Label":0}
{"Functions Text":"in combination with Planck Low Frequency Instrument data","Functions Label":0}
{"Functions Text":"Moreover, in recent years evidence has grown supporting the statement that GCs are generally composed of two or three chemically distinct populations. These subpopulations are separated by a few tens to hundreds of Myr in age and show vastly varying abundances of light elements such as C, N, O, Na, Mg, and Al (see, e.g.,","Functions Label":0}
{"Functions Text":"Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S\u2009ii]\/H\u2009\u03b1 > 0.4\u20130.5","Functions Label":0}
{"Functions Text":"We adopt a four-level AR classification scheme based on the maximum GOES-level flare an AR ever yields","Functions Label":2}
{"Functions Text":"Al i lines at 6696 and 6698 are used for deriving the Al abundance and these lines have negligible contributions from NLTE effects","Functions Label":2}
{"Functions Text":"As pointed out in","Functions Label":5}
{"Functions Text":"we found clear evidences of pulsation phase variability with a maximum change of 2 \u00d7 10-3 c\/d. In other words, as an example after one year time a phase-constant model would appear to have the correct shape with respect to the pulsation pattern of the star, but shifted several minutes in time.","Functions Label":5}
{"Functions Text":"The dust radiative transfer and photosionisation code mocassin","Functions Label":2}
{"Functions Text":"was used produce the temperature parametrization. The atomic data base of the mocassin code included opacity data from Verner et al. (1993) and Verner & Yakovlev (1995), energy levels, collision strengths and transition probabilities from Version 5.2 of the CHIANTI data base (Landi et al. 2006, and references therein) and hydrogen and helium free\u2013bound continuous emission data of Ercolano & Storey (2006).","Functions Label":2}
{"Functions Text":"For BH-LMXBs","Functions Label":0}
{"Functions Text":"and the X-ray spectrum can be well described by a multicolour blackbody spectrum (e.g.","Functions Label":0}
{"Functions Text":"Equilibrium tides become then effective (e.g.,","Functions Label":2}
{"Functions Text":"and references therein) and the tidal evolution may occur on a longer timescale.","Functions Label":2}
{"Functions Text":"For instance, for the Lyman \u03b1 radiation \u03c7\u03bdr = 0.042 for optimum efficiency \u03c7o = 0.1","Functions Label":2}
{"Functions Text":"In particular, there are currently five main competing models.","Functions Label":0}
{"Functions Text":"(2) Empty Asteroid Belt: embryos and planetesimals in the protoplanetary disk formed concentrated within a narrow belt at \u223c0.7\u20131 au","Functions Label":0}
{"Functions Text":"In what is called the \u201cfrozen-screen\u201d hypothesis","Functions Label":0}
{"Functions Text":"these pockets, or turbulent eddies, are assumed to be fixed in the atmospheric layer that advects over an interferometric array","Functions Label":0}
{"Functions Text":"The dark and light shaded areas in Fig. 10 correspond to the 1\u03c3 and 2\u03c3 constraints on the redshift of reionization from the cosmic microwave background measurements of the Planck mission","Functions Label":2}
{"Functions Text":"with a reionization midpoint zre\u2004=\u20047.67\u2005\u00b1\u20050.73.","Functions Label":2}
{"Functions Text":"Previous sub-arcsecond angular resolution N-band (\u223c8\u201313 \u03bcm) ground-based spectroscopic studies investigated the 11.3 \u03bcm PAH feature in the nuclear and circumnuclear regions of AGN","Functions Label":0}
{"Functions Text":"However, these works were unable to provide definitive details regarding the effect of the AGN on the PAH molecules due to limited wavelength coverage and sensitivity.","Functions Label":3}
{"Functions Text":"In particular, the asymmetric Ly\u03b1 line profile has enabled redshift confirmations of large samples of sources at both 2\u2004\u2004z\u2004\u20046 (e.g.,","Functions Label":0}
{"Functions Text":"The faster solar wind tends to be more imbalanced with greater wave energy flux antisunward than sunward","Functions Label":0}
{"Functions Text":"In addition, another classification scheme uses a scatter plot of flux and duration fitted with two-dimensional Gaussian functions","Functions Label":1}
{"Functions Text":"Since NS He-atmosphere models have harder spectra than H-atmosphere models, using the incorrect composition for the observed thermal emission can result in biases of the inferred radii","Functions Label":2}
{"Functions Text":"The main sequence is a relationship between SFR and stellar mass followed by the majority of star-forming galaxies, apart from some outliers located above the average SFR at given stellar mass","Functions Label":0}
{"Functions Text":"As a result, direct imaging studies cannot decisively determine whether the clumps are different in nature from star-forming regions in our local universe or if the larger apparent size is merely an artifact of insufficient resolution","Functions Label":0}
{"Functions Text":"Prior to complete gas removal, moderate values of ram pressure have also been shown to increase the star formation rate in galaxies both observed","Functions Label":0}
{"Functions Text":"and simulated","Functions Label":0}
{"Functions Text":"However, close encounters with the planets proved not to be enough for creation of the current population of binary systems","Functions Label":0}
{"Functions Text":"Choosing values of these parameters that are consistent with simulations (e.g. those of","Functions Label":2}
{"Functions Text":"Magnetic reconnection rapidly converts magnetic energy to particle energy, causing emission flare in multiple wave bands and even triggering coronal mass ejections","Functions Label":0}
{"Functions Text":"So, the mean length for QS network jets from the present work is in good agreement with","Functions Label":5}
{"Functions Text":"We note that a hotter disk during maximum was predicted by a simpler study in the past","Functions Label":5}
{"Functions Text":"The most evident effect driven by galaxy encounters is probably the triggering of new episodes of star formation, which can occur both in the pre-merger regime between first pericentre and coalescence (e.g.","Functions Label":0}
{"Functions Text":"In Fig. 10, we show the relation between the size and star formation rate of clumps, including samples across different redshifts","Functions Label":2}
{"Functions Text":"Our sample","Functions Label":5}
{"Functions Text":"despite being at z \u223c 2\u20136, have sizes comparable to local H\u2009ii regions and GCs","Functions Label":5}
{"Functions Text":"but they have SFRs \u223c300 times higher.","Functions Label":6}
{"Functions Text":"However, a study of non-convex shape models for fast two to four hour rotators in","Functions Label":5}
{"Functions Text":"indicated that such asteroids have rather minimal levels of global-scale concavities, and the ~ 2.7 h rotation period of Cuyo implies that its shape could be similar.","Functions Label":5}
{"Functions Text":"An alternative explanation that we propose here goes back to the nature of the optically thick 12CO emission and to the approximately linear relation between 12CO luminosity and virial mass found for GMCs (see e.g.","Functions Label":2}
{"Functions Text":"for a more recent compilation","Functions Label":2}
{"Functions Text":"Similar signatures were also reported in observations (e.g.,","Functions Label":5}
{"Functions Text":"For reference, the dark red crosses also show the equivalent satellite\/central red galaxy wg + correlations from KiDS\u00d7GAMA here (c.f.","Functions Label":2}
{"Functions Text":"fig. 7, red points\/band).","Functions Label":2}
{"Functions Text":"On large scales at least, our illustristng red sample is consistent with their measurements.","Functions Label":5}
{"Functions Text":"There are a few interesting features here to note, however.","Functions Label":1}
{"Functions Text":"Although the general trends match the real data,","Functions Label":5}
{"Functions Text":"with ss and to a lesser extent cs exhibiting strong scale-dependent IAs in this regime, the magnitude is somewhat higher in our sample.","Functions Label":6}
{"Functions Text":"This is particularly interesting, given that our sample characteristics are similar (\u2329L\u232a\/L0 = 0.91 and 0.34 for our red and blue samples, respectively, compared with their \u223c0.99 and 0.50).","Functions Label":1}
{"Functions Text":"It is now well established that the weak lensing of distant galaxies by foreground mass provides a relatively clear window on to the large-scale structure of the Universe. This is true whether that foreground mass is in the form","Functions Label":0}
{"Functions Text":"or the continuous large-scale matter distribution (cosmic shear;","Functions Label":0}
{"Functions Text":"The [C\u2009ii] deficit persists when including high-z galaxies (e.g.","Functions Label":3}
{"Functions Text":"This problem is also known as the Cosmological Lithium problem","Functions Label":0}
{"Functions Text":"Over that time they have been assigned different terms, such as","Functions Label":0}
{"Functions Text":"coronal waves (e.g.,","Functions Label":0}
{"Functions Text":"For comparison, we show published observations in the same redshift range from the literature in the right panel of Figure 5","Functions Label":2}
{"Functions Text":"We estimated using the","Functions Label":2}
{"Functions Text":"IMF the expected range for the observed M\/OB number ratio.","Functions Label":2}
{"Functions Text":"Minkowski functionals, which are also closely related to the crossing statistics","Functions Label":0}
{"Functions Text":"and have been utilized for cosmological random fields","Functions Label":0}
{"Functions Text":"This phase motion has been seen in magnetospheric data of Alfv\u00e9n waves","Functions Label":2}
{"Functions Text":"and the simulations of coronal oscillations by","Functions Label":2}
{"Functions Text":"These studies note that the direction of motion is related to the spatial variation of \u03c9c.","Functions Label":2}
{"Functions Text":"Energetic electrons are unstable to Langmuir waves, thus they are converted into radio emission at the local plasma frequency and its harmonic (see","Functions Label":0}
{"Functions Text":"have shown that the effects of a merger are visible for approximately 0.25 Gyr after the merger event while the pre-merger stage is much longer. However, we chose to have the pre and post merger period approximately equal as tests conducted with longer pre-merger times showed no improvement, see discussion in Sect. 4.2.","Functions Label":1}
{"Functions Text":"Fourthly, with the NIST data base","Functions Label":2}
{"Functions Text":"which is considered as the most critically analysed data base.","Functions Label":2}
{"Functions Text":"Comparison with observed energies","Functions Label":5}
{"Functions Text":"and with the NIST values shows that the present ab initio values are not fully converged to experimental values.","Functions Label":5}
{"Functions Text":"The hybrid source XTE J1701\u2013462 occupies a special place among NS LMXBs and is considered to be a remarkable source, as it displays all the characteristics exhibited by both Z and atoll sources","Functions Label":3}
{"Functions Text":"As for the planet\u2019s phase offset,","Functions Label":1}
{"Functions Text":"and May & Stevenson (2020) favour a larger phase offset (21 \u00b1 2\u2009\u00b0E) than Mendon\u00e7a et al. (2018) and Morello et al. (2019) (12 \u00b1 3\u2009\u00b0E and 11 \u00b1 2\u2009\u00b0E).","Functions Label":1}
{"Functions Text":"There are at least three reasons why radiative feedback is an essential ingredient of the galaxy formation process.","Functions Label":0}
{"Functions Text":"Thirdly, it is difficult to explain the large gas turbulence values observed in star-forming regions without including the momentum input by radiation","Functions Label":0}
{"Functions Text":"Furthermore, most of these HFF clusters are in a state of collision, enhancing their value for assessing the collisionality of dark matter (DM), a basic assumption of the standard particle interpretation of DM","Functions Label":3}
{"Functions Text":"The features observed in most CL AGNs, e.g., the complex multiband spectral variabilities, and strong changes seen in the infrared or low level of polarization, strongly argue against the scattering (or obscuration) scenario (e.g.,","Functions Label":1}
{"Functions Text":"noted that heating bayerite at 500\u00b0C eliminates the XRD pattern of bayerite, and they note that at 700\u00b0C, the infrared reflectance spectrum of the boehmite sample no longer shows OH\u2212 stretching bands.","Functions Label":1}
{"Functions Text":"As can be seen in this table, the WHISPER survey allowed the detection of some organic molecules in the Horsehead nebula, such as formaldehyde (H2CO) and methanol (CH3OH), which constitute key species in the likely synthesis of more complex organic molecules such as some prebiotic molecules","Functions Label":2}
{"Functions Text":"In these objects, the total number of OB associations is significantly larger than the number of HII regions under formation and of OB stars reaching the final stage of their evolution, thus their total H\u03b1 luminosity is fairly constant with time. This might not be the case in strongly perturbed systems or in dwarf galaxies, where the total star formation activity can be dominated by individual giant HII regions","Functions Label":1}
{"Functions Text":"Early attempts of low-resolution three-dimensional numerical simulations on overshooting were made by","Functions Label":0}
{"Functions Text":"(downward overshooting)","Functions Label":0}
{"Functions Text":"also showed that the MMF can be generalized for the case where the SED of the sources is not known.","Functions Label":0}
{"Functions Text":"This generalization outperforms the single-frequency MF in terms of S\/N and can be used to infer the spectral index of synchrotron-dominated radio sources, as shown in Lanz et al. (2013).","Functions Label":1}
{"Functions Text":"The detrending performances of pixel-ICA method have been compared with division by a polynomial function of the centroid, in this paper PCD method, and PLD method","Functions Label":1}
{"Functions Text":"This result is inline with the number density estimate of the order of \u223c10\u221210 Mpc\u22123 by","Functions Label":5}
{"Functions Text":"Our preliminary analysis shows that the self-gravitating response is a linear superposition of two terms: (i) a continuum of modes given in Equation (12), dressed by self-gravity, that undergo phase mixing and give rise to the phase spiral; and (ii) a discrete set of modes called point modes or normal modes (see","Functions Label":2}
{"Functions Text":"that follow a dispersion relation.","Functions Label":2}
{"Functions Text":"One warm and compact component at 200 K and a size of 0.35\u2033 (that of the continuum compact emission obtained by ALMA Band 7 observations,","Functions Label":2}
{"Functions Text":"this mass is significantly diminished via stellar winds already during core hydrogen (H) burning","Functions Label":0}
{"Functions Text":"The Low Frequency Array","Functions Label":0}
{"Functions Text":"has opened up new ways of studying galaxies in the radio, and a number of studies have used LOFAR\u2019s capabilities to investigate this relationship between star formation and radio luminosity in the low-frequency regime \u2013 for example","Functions Label":0}
{"Functions Text":"Read et al. (2018), Smith et al. (2021), and Wang et al. (2019a).","Functions Label":0}
{"Functions Text":"The chemical contamination of barium stars is believed to be due to accretion of chemically enriched material from an evolved binary companion, likely through wind","Functions Label":0}
{"Functions Text":"Then a separation of the HC top from that of the prominence was observed during the eruption initiated by the ideal kink instability","Functions Label":6}
{"Functions Text":"Therefore, this observation offered further important support for the idea that an HC is an MFR","Functions Label":5}
{"Functions Text":"The overall excesses within 805 and 1186 h of HESS exposures","Functions Label":2}
{"Functions Text":"Most of the radiative models for Sgr A*, which are based on post-processing GRMHD simulations, assume that electrons have a thermal, relativistic (Maxwell\u2013J\u00fcttner) distribution function, and that the proton-to-electron temperature ratio is constant across the simulation domain","Functions Label":0}
{"Functions Text":"There are indeed indications that the buildup of the ice in cold environments results in the formation of pores as shown b","Functions Label":0}
{"Functions Text":"and simulations","Functions Label":0}
{"Functions Text":"These two studies, based on Monte Carlo simulations, suggest a significant level of porosity at the surface\/subsurface, in particular in cold and dense environments.","Functions Label":0}
{"Functions Text":"This geometric advantage is shared with the related analysis technique of spherical Fourier-Bessel (SFB) decomposition","Functions Label":5}
{"Functions Text":"which, in addtion to spherical harmonic decomposition, involves a further Fourier-Bessel transform and data-compression along the line-of-sight.","Functions Label":0}
{"Functions Text":"However, SFB does not share another important feature of SHT, which is its ability to capture redshift-dependent change over cosmological time in deep surveys.","Functions Label":6}
{"Functions Text":"While Sn can also be formed from pure H2S ice by photo processing","Functions Label":1}
{"Functions Text":"the fact that S3 is clearly related to dust and is not found in the normal nucleus ice, where H2S is quite abundant, indicates that S3 is a product of radiolysis of the ammonium salt.","Functions Label":1}
{"Functions Text":"However, for heavily accreting massive YSOs the onset of the H\u202fII region could be delayed via stellar bloating","Functions Label":0}
{"Functions Text":"where the effective temperature of the star is much cooler than it would be considering a main sequence star of the same luminosity. In these models, a halt or considerable reduction in accretion (\u226a10\u22123 M\u2299 yr\u22121), or growth beyond ~30\u221240 M\u2299, will result in the YSO contracting to a \u201cmain-sequence\u201d configuration, heating significantly, and being able to create an H\u202fII region.","Functions Label":0}
{"Functions Text":"When we change the magnitude of two tides, the final location of the planets can be adjusted","Functions Label":2}
{"Functions Text":"Concerning the other far-IR PACS band (100 \u03bcm) and the mid-IR 24-\u03bcm band, we use the association available in the DR1 release and based on the maximum likelihood technique","Functions Label":2}
{"Functions Text":"The time for GJ 1148 b to reach asymptotic rotation is inversely proportional to the initial Prot, as long as the initial Prot is much less than 27.5 d, and it depends on the other parameters of GJ 1148 b according to Eq. (3) of","Functions Label":2}
{"Functions Text":"At higher Eddington ratios of Lbol\/LEdd \u2273 10\u22122, single-epoch X-ray and UV observations of large samples of AGN have previously revealed a hardening of \u03b1OX as Lbol\/LEdd drops from \u223c1 to \u223c10\u22122 (e.g.,","Functions Label":0}
{"Functions Text":"We note that we can discount variations in the seed photon population as the driver for changes in the power spectrum, as the UV emission from the disc is established to be considerably less variable than the corona in NLS1s","Functions Label":2}
{"Functions Text":"We find here that about two free-fall times (as defined for cylindrical systems, see","Functions Label":2}
{"Functions Text":"are sufficient to reach core deuteration fractions of \u22730.1.","Functions Label":2}
{"Functions Text":"Within conventional leptonic scenarios, this component is produced when the synchrotron-emitting electrons inverse Compton up scatter the photons of internal (synchrotron self-Compton, SSC;","Functions Label":1}
{"Functions Text":"Adding on AGN feedback would significantly impact on the distribution, kinematics and physical status of the gas, specifically for the close environment of the black hole","Functions Label":7}
{"Functions Text":"In last few decades, the understanding of CMEs improved significantly because of space and ground-based observational data with the help of various modelling efforts. The studies are focused on the morphological and kinematic evolution of CMEs in the heliosphere, e.g.","Functions Label":0}
{"Functions Text":"The growth of dust grains through accretion in the ISM has been proposed as a solution (e.g.","Functions Label":3}
{"Functions Text":"Other studies suggest that the presence of preeruptive MFRs is not necessary and MFRs could be built up in the corona via magnetic reconnection processes associated with flares","Functions Label":3}
{"Functions Text":"For instance, it is well known that adding a tiny amount of heavy elements and dust grains alters the EOS of a collapsing cloud (e.g.","Functions Label":0}
{"Functions Text":"High-ionization UV lines have been detected in the spectra of z\u2004\u2273\u20042 galaxies through","Functions Label":0}
{"Functions Text":"spectral stacking","Functions Label":0}
{"Functions Text":"The EWs of He\u202fII, O\u202fIII]\u03bb1666, and C\u202fIII] from these works are larger than those measured in the average spectra of our LAEs, with the exception of","Functions Label":5}
{"Functions Text":"some of the stacks from","Functions Label":5}
{"Functions Text":"The EWs from","Functions Label":6}
{"Functions Text":"are computed from average spectra of a z\u2004\u2248\u20043 LAE population whose median UV luminosity is about two orders of magnitude brighter than ours.","Functions Label":6}
{"Functions Text":"From Figure 2 in Rincon et al. (2017), we further notice that the vortical component of the photospheric surface velocity field has a structure reminiscent of 2D Euler turbulence, which admits a vortex point representation","Functions Label":2}
{"Functions Text":"also on the sphere","Functions Label":2}
{"Functions Text":"An alternative route to explain the presence of methanol in the gas phase is the reactive\/chemical desorption that has been theoretically proposed by Garrod et al. (2007) and","Functions Label":0}
{"Functions Text":"and experimentally studied by Dulieu et al. (2013) and Minissale et al. (2016).","Functions Label":0}
{"Functions Text":"On the other hand, c-C3H2 is mainly formed in the gas phase","Functions Label":0}
{"Functions Text":"and is expected to preferentially trace dense and chemically young gas, that is, gas where C atoms have not yet been mainly locked into CO.","Functions Label":0}
{"Functions Text":"This gas rich in C atoms is expected in the outer envelope of an externally illuminated dense core","Functions Label":0}
{"Functions Text":"However, towards L1544, c-C3H2 only appears to trace one side of the core, the one closer to the sharp N(H2) edge and away from the CH3OH peak. This indicates that photo-chemistry is not uniformly active around L1544, most likely because the distribution of the envelope material (belonging to the filament within which L1544 is embedded) is not uniform, as is clearly shown by the Herschel map in Fig. 1.","Functions Label":6}
{"Functions Text":"To date our knowledge of GRGs (see e.g.","Functions Label":0}
{"Functions Text":"is limited by their sparse numbers and by the difficulty of detecting them over large areas of the sky. Low-frequency radio observations have an enhanced capacity to detect the extended old electron population in these objects (see e.g. the recent Low Frequency Array \u2013 LOFAR \u2013 observation of the GRG UGC095551), but high-frequency radio observations are less efficient in this task due to the steep-spectra of giant radio lobes.","Functions Label":0}
{"Functions Text":"In this context these sources will be ideal targets for the next coming deep, wide-field surveys like, e.g. the ATLAS survey of the Australia Telescope Network Facility (ATNF","Functions Label":7}
{"Functions Text":"or the Square Kilometre Array (SKA) deep surveys that will have the potential to study their population evolution up to high redshifts and thus clarifying their role on the feedback for the evolution of non-thermal processes in large-scale structures.","Functions Label":7}
{"Functions Text":"Within a 500 arcsec radius centred on NGC 346, we find an atomic gas mass of 2.7\u00d7106 M\u2299 using the Parkes+ATCA H\u2009i map","Functions Label":2}
{"Functions Text":"Analysis of Chandra observations revealed a hole or bubble within the ICM, cospatial with the eastern lobe of the jet","Functions Label":0}
{"Functions Text":"By using the RADEX2 dense cloud models developed by","Functions Label":2}
{"Functions Text":"to reproduce the HCN(3\u20132)\/(1\u20130) line luminosity ratios in the outflow of Mrk 231, we can attempt to find a combination of XHCN, XCN, Tkin, and nH2 solutions that can also fit the CN\/HCN and CN spin doublet line ratios (Table 2)","Functions Label":2}
{"Functions Text":"The HB pattern is generally observed in the subcritical regime and the DB pattern is observed in the supercritical regime","Functions Label":0}
{"Functions Text":"Previous 12CO observations either reported no detection of outflow emission toward this source","Functions Label":1}
{"Functions Text":"or only weak compact blueshifted emission towards east of the continuum source","Functions Label":1}
{"Functions Text":"The [OII]\u03bb3737 emission traces on-going star formation","Functions Label":0}
{"Functions Text":"but it also depends on the metallicity and can be a poor tracer for dusty galaxies (e.g.","Functions Label":0}
{"Functions Text":"Moreover, other studies have compared AGN selected from various wavebands and find that their host galaxies tend to have different properties","Functions Label":3}
{"Functions Text":"and star-formation rates (SFR;","Functions Label":3}
{"Functions Text":"The model atmosphere used in this work was interpolated from the line-blanketed, local thermodynamic equilibrium (LTE) ATLAS9-ODFNEW grid","Functions Label":2}
{"Functions Text":"Besides these necessary conditions for the applicability of the FP equation, also other simplifying assumption for a better tractability of the FP equation are being made, such as (1) the magnetic fluctuations are homogeneous in space, (2) the electromagnetic fields are quasi-static, (3) the interaction has a finite decorrelation time, etc. (see more details in the books","Functions Label":0}
{"Functions Text":"Unfortunately, in astrophysical and laboratory plasmas, most of the above assumptions are not valid, yet the FP equation is used extensively, without a proof of its validity.","Functions Label":0}
{"Functions Text":"Aside from the observational implications, the planet\u2019s physical and chemical state can be altered by stellar activity as well due to, for example, coronal mass ejections (CMEs) and stellar particle events (SPEs)","Functions Label":0}
{"Functions Text":"As a further comparison, data from the SOHO\/EPHIN spacecraft (red square marker) between 40 MeV and 53 MeV are also presented","Functions Label":2}
{"Functions Text":"The agreement appears to be good in all the three examined periods, considering both statistical and systematic uncertainties.","Functions Label":5}
{"Functions Text":"Covering these spatial scales in \u2264108 yr requires a diffusion coefficient of D \u2265 9 \u00d7 1028 cm2 s\u22121, which is slightly higher than observed in spiral galaxies","Functions Label":6}
{"Functions Text":"If the spatial velocity of a star in an SNR is very different from the others in the SNR, the star is very possible to be the surviving companion in the remnant","Functions Label":2}
{"Functions Text":"Mechanisms involving the addition of hydrocarbons, such as acetylene onto aromatic rings as well as the attachment of other aromatic rings, or hydrocarbon pyrolysis, have been proposed to characterize the growth process of PAHs","Functions Label":0}
{"Functions Text":"Current cosmological hydrodynamic simulations of galaxy formation employ a variety of subgrid models (e.g.","Functions Label":0}
{"Functions Text":"that artificially launch galactic winds,","Functions Label":0}
{"Functions Text":"These three spatial features nearby to the Sun appear to form part of the global spiral structure in the Galaxy. Contrary, the objects of older population with larger random velocities, for instance, main-sequence A\u2013K stars or the oldest Cepheids and open clusters, do not currently follow the exact location of those arms (e.g.","Functions Label":1}
{"Functions Text":"fig. 8 therein","Functions Label":1}
{"Functions Text":"The above equation should reduce to the jet Lorentz factor profile used in","Functions Label":5}
{"Functions Text":"when \u03b6 = 1.","Functions Label":5}
{"Functions Text":"The core stable within 200 \u03bcas constrained by the VERA can be explained by Lorentz factors within a factor of two variation for the slower ejecta, i.e., 8 \u2264 \u0393s \u2264 17, by assuming","Functions Label":0}
{"Functions Text":"\u0393f\/\u0393s \u2264 1.01","Functions Label":0}
{"Functions Text":"This scenario is in agreement with arguments by other authors that the 26Al-free CAIs formed prior to injection and homogenization of 26Al in the early solar system","Functions Label":5}
{"Functions Text":"When planets become massive enough, they can carve gap","Functions Label":0}
{"Functions Text":"and disturb the dynamics of the gas","Functions Label":0}
{"Functions Text":"Galaxies formed in these halos because of the cooling of","Functions Label":0}
{"Functions Text":"or molecular hydrogen","Functions Label":0}
{"Functions Text":"This allows us to use the microlensing magnifications to estimate the source size, and such work has shown that in general the accretion disks are larger than would be expected from either thin disk modeling or total flux arguments","Functions Label":0}
{"Functions Text":"The bright end of the UpSco population has been examined in X-rays","Functions Label":0}
{"Functions Text":"A full description of the GLOSTAR continuum data calibration and imaging is given in","Functions Label":2}
{"Functions Text":"More precisely, it takes 3\u20134 orbits for MRI to develop and \u223c10 orbits to saturate","Functions Label":2}
{"Functions Text":"presented scaling relations between the azimuthal separation of the primary and secondary arms and the planet-to-star mass ratio for a single companion on a circular orbit with a mass between Neptune mass and 16 MJ around a 1 M\u2299 star. They predicted with 30% accuracy that a single putative planet responsible for both spiral features of SAO 206462 would have a mass of ~6 MJ.","Functions Label":0}
{"Functions Text":"The most likely candidates for this task, given their reasonable agreement with observations and numerical simulations of cosmic-ray diffusion coefficients, are the quasilinear theory (QLT) of Jokipii (1966), the weakly nonlinear theory (WNLT) of Shalchi et al. (2004b), and the nonlinear guiding center theory (NLGC; or one of its variants; see, e.g.,","Functions Label":0}
{"Functions Text":"Our analysis was rather easy, starting from a prediction based on","Functions Label":2}
{"Functions Text":"parameters.","Functions Label":2}
{"Functions Text":"Other examples of AGN with at least two variable phases of the X-ray winds are","Functions Label":0}
{"Functions Text":"and PG 1114+445","Functions Label":0}
{"Functions Text":"We showed that the ambipolar diffusion module in Bifrost can cope with the passage of the solutions through the current sheets, with the level of accuracy increasing the higher the spatial resolution and in spite of the intrinsic singularity in them. Vice versa, the tests show that these functions can probe the capabilities of ambipolar diffusion modules to a larger extent than the simple ZKBP solution that has been used thus far (e.g.","Functions Label":1}
{"Functions Text":"The results were obtained implementing a Bayesian scheme that uses the spectroscopic constraints and frequency ratios as the parameters in the fit","Functions Label":2}
{"Functions Text":", the latter being almost insensitive to the surface effects in solar-like oscillators","Functions Label":2}
{"Functions Text":"studied the mechanism for the flare trigger by shock waves. They used a 2D magnetohydrodynamic model with the MHD shock wave propagating towards the current sheet. A portion of the shock wave passed through the sheet, and the rest was reflected. Nothing occurred at the very beginning of the wave-current sheet interaction. However, after some time, specific plasma flows around the current sheet were formed, which led to the start of magnetic reconnection.","Functions Label":0}
{"Functions Text":"This shows that for reconnection to be triggered, the enhanced electrical resistivity as well as the plasma flows are important.","Functions Label":3}
{"Functions Text":"The release of gravitational binding energy via accretion of matter onto these BHs is expected to have a profound impact on the evolution of their host galaxies (e.g.,","Functions Label":3}
{"Functions Text":"Figure 1 shows the view obtained from polarimetric observations: the left panel shows the Q\u03a6 image in the J band obtained by","Functions Label":2}
{"Functions Text":"using SPHERE on a linear scale, and the two rings are clearly visible.","Functions Label":2}
{"Functions Text":"We also used some observational data obtained within several other programmes","Functions Label":2}
{"Functions Text":"The nuclear reaction rates are those from the NACRE project","Functions Label":2}
{"Functions Text":", supplemented by the updated reaction rate from","Functions Label":2}
{"Functions Text":"Ccf is a factor that removes the color term from S and is a function of Johnson","Functions Label":2}
{"Functions Text":"Intrinsic L\u03bd(1400)\/L\u03bd(900) ratios obtained from different stellar population models: the BC03, assuming different initial mass functions (Salpeter, Salp, and Chabrier, Chab), star-formation histories (constant, cSFR, exponentially declining with \u03c4 = 0.1Gyr, exponentially rising with \u03c4 = \u22120.1Gyr), metallicties (Z\u2299 and 0.02 \u00d7 Z\u2299), and stellar-population ages;","Functions Label":2}
{"Functions Text":"As described in","Functions Label":2}
{"Functions Text":"BC03 provides the spectral energy distribution of stars obtained from a comprehensive library of theoretical model atmospheres (KBFA in the table).","Functions Label":2}
{"Functions Text":"The library consists of Kurucz (1996) spectra for O-K stars, Bessell et al. (1991) and Fluks et al. (1994) spectra for M giants, and Allard & Hauschildt (1995) spectra for M dwarfs.","Functions Label":0}
{"Functions Text":"The SFR_2b model is the one that best reproduces the observed A(Li) distribution while recovering the presently observed SFR and the thin-disk stellar and HI mass","Functions Label":1}
{"Functions Text":"There are at least three possible types of outflows around young stellar objects: (1) a disc wind launched from the accretion disc (e.g.","Functions Label":0}
{"Functions Text":"The net radiolysis is the combined effect of the direct primary excitations and ionisations, the core of the energy deposition by the ion, and the so-called delta rays (energetic secondary electrons) travelling at much larger distances from the core; that is, several hundreds of nanometres at the considered energies in this work","Functions Label":2}
{"Functions Text":"Experimental measurements by e.g. instantaneous laser tomography have given values ranging from D = 2.1\u22122.4 in a variety of flow geometries, with a preferred value of D = 2.35","Functions Label":2}
{"Functions Text":"If a single SMBH model with a BLR d of 95 light days is true (see","Functions Label":1}
{"Functions Text":"a differential signal would be 0.9\u00b0.","Functions Label":1}
{"Functions Text":"Instead, it is most likely that these values correspond to ram pressure, in which case they imply mass, momentum, and energy flux across Eulerian cloud boundaries, or a displacement of Lagrangian boundaries","Functions Label":2}
{"Functions Text":"The radiation of SNRs in different wavelength ranges is under the influence of biases as they cover different aspects of the ISM environment and SNR age and evolution","Functions Label":0}
{"Functions Text":"However, recent experiments indicate that this product channel occurs in only 19 percent of collisions, with 81 percent of collisions forming CH + S","Functions Label":1}
{"Functions Text":"Even so, significant progress has been made in the last decade, though the problem is usually made tractable by introducing at least one of the following simplifying assumptions: abandoning general relativity in favor of a pseudo-Newtonian description of the gravitational potential while performing realistic, multi-angle group radiation transport","Functions Label":0}
{"Functions Text":"The value R \u2248 5 mm has been constrained by several data collected at comet 67P, by laboratory experiments of dust accretion in conditions expected to occur in the solar protoplanetary disc and by observations of other protoplanetary discs","Functions Label":2}
{"Functions Text":"The astrophysical disk transition region is at least equally complicated since it is not only the base of the disk corona, but also the origin of purported disk winds and outflows (e.g.,","Functions Label":3}
{"Functions Text":"However, there is indication of non-negligible poloidal fields as well as toroidal fields\u2014resulting in helical magnetic fields\u2014in the jet environment of other distant AGNs, which results in transverse RM gradients with no sign changes (e.g.,","Functions Label":0}
{"Functions Text":"Open clusters have been used to test the scaling relations for giants","Functions Label":0}
{"Functions Text":"RASCAS deploys a general two-step methodology (e.g.","Functions Label":2}
{"Functions Text":"On the other hand, high values of temperature, surface density, and velocity dispersion in a turbulent ISM of starbursts and merging systems will shift \u03b1CO towards lower values","Functions Label":1}
{"Functions Text":"To our rescue, eBOSS also targets all SDSS point sources that are within 1 arcsec of a radio detection in the FIRST point source catalogue","Functions Label":2}
{"Functions Text":"Recent proper motion data confirm that most of the classical MW satellites do indeed have a common orbital plane","Functions Label":0}
{"Functions Text":"aligned with the plane normal defined by the satellite positions alone","Functions Label":0}
{"Functions Text":"Among these large-scale structures, the underdensities of the universe, i.e. cosmic voids, have been shown to have great potential for constraining dark energy and testing theories of gravity via several measurements. These measurements include: distance measurement via the Alcock\u2013Paczy\u0144ski test","Functions Label":3}
{"Functions Text":"There are further analytical approaches described in the literature","Functions Label":0}
{"Functions Text":", although these models predicted a change in the spin state of the nucleus without taking into consideration the exact 3D shape model and its variation induced by mass loss.","Functions Label":6}
{"Functions Text":"However, since the identification of the Ly\u2009\u03b1 forest in hydrodynamic simulations","Functions Label":0}
{"Functions Text":"it was realized that in the context of cosmological models for structure formation, the Ly\u2009\u03b1 forest is due to a fluctuating, continuous IGM (e.g.","Functions Label":0}
{"Functions Text":"Alternatively, the origination of giant pulses is proposed from the coherent instability of plasma near the magnetic equator of light cylinder","Functions Label":0}
{"Functions Text":"Magnetospheric accretion (MA) shock modelling was carried out for each star by adding (blackbody) accretion contributions to the photospheric (Kurucz) spectra (see e.g. the reviews in","Functions Label":2}
{"Functions Text":"Therefore, on the basis of the oscillation of coronal loops, especially their oscillation characteristics in frequency, phase and attenuation coefficient, solar physicists can further understand the relationships between the coronal magnetic field, flares and CME","Functions Label":3}
{"Functions Text":"and obtain corresponding physical parameters associated with oscillating coronal loops","Functions Label":3}
{"Functions Text":"lists the orbital parameters (orientation and separation) of WDS 02499+0856 and gave \u03b8 = 194\u00b0, \u03c1 = 5.66\u2009arcsec and magnitude difference \u0394V = 0.07\u2009mag (the magnitude difference can be as large as \u0394V = 0.36\u2009mag, due to photometric variability of the eclipsing binary)","Functions Label":0}
{"Functions Text":"Complementary to the study of the overall metallicity distribution, the abundance ratios of several other elements, such as \u03b1-elements, iron peak, odd-z, and neutron capture, can provide deep insight into the variety of nucleosynthesis processes, with their production sites and time-scales (e.g.","Functions Label":0}
{"Functions Text":"The thermal state and kinematics of the progenitor hot plasma halo drive the formation and evolution of all the condensed structures, which inherit some of the parent properties. Part of the inner condensed gas eventually accretes onto the central supermassive black hole (SMBH), igniting the feedback response and efficiently self-regulating the entire atmosphere over several gigayears (e.g.,","Functions Label":0}
{"Functions Text":"Furthermore, given the demonstrated sensitivity of computed low-energy galactic electron intensities to various turbulence quantities (see","Functions Label":2}
{"Functions Text":", it may be possible to draw conclusions from Jovian electrons to better understand the behaviour of those quantities in regions of the heliosphere where spacecraft observations of this character do not exist","Functions Label":2}
{"Functions Text":"As motivation, we note that a variety of observations in the solar wind","Functions Label":3}
{"Functions Text":"have suggested that fluctuations near the end of the magnetohydrodynamic (MHD) inertial cascade range, and approaching the kinetic plasma range, may consist primarily of kinetic Alfv\u00e9n waves (KAWs).","Functions Label":3}
{"Functions Text":"Events that took place in the far past are expected to have induced a thickening of the early Galactic disc,","Functions Label":0}
{"Functions Text":"and second by agitating the gaseous disc from which new stars are born, generating early stellar populations with higher initial velocity dispersions than those currently being formed","Functions Label":0}
{"Functions Text":"There have not been many simultaneous multi-wavelength studies of flaring stars","Functions Label":3}
{"Functions Text":"There is a particular dearth of simultaneous data in the EUV which is critical for studies of exoplanetary upper atmospheres, but where measurements are difficult due to ISM absorption. More observations are needed, but if young, magnetically active stars display broadband continuum enhancements during flares, similar to AU Mic, this would mean that large altitude ranges in planetary atmospheres are affected.","Functions Label":3}
{"Functions Text":"Although hampered by the short duration of the quenching process, the search for galaxies in this critical phase of evolution has been carried on by several authors in the past decades. Galaxies characterized by both a tidally disturbed morphology and intermediate colours (e.g","Functions Label":0}
{"Functions Text":"have been considered as valid 'recent time' quenching candidates.","Functions Label":0}
{"Functions Text":"There are a number of such ground-based experiments, including","Functions Label":0}
{"Functions Text":"the Shaped Antenna measurement of the background RAdio Spectrum (SARAS;","Functions Label":0}
{"Functions Text":"The reliability of the used method is also underlined by the good qualitative agreement between the Density Functional Theory (DFT) and MP2-F12 calculations as found in previous works","Functions Label":5}
{"Functions Text":"Theoretical models by Granato et al. (2004) suggest that forming clusters will go through a phase in which multiple members will undergo near-simultaneous massive bursts of star formation. The spectral energy distribution of these objects would be dominated by the far-IR, as is the case for local massive starbursts (e.g.","Functions Label":0}
{"Functions Text":"While the K2 optical data set detected a 3.3 day periodic 1% photometric modulation, it is not present in the Spitzer observations","Functions Label":6}
{"Functions Text":"Other possible alternative mechanisms leading to the acceleration of HVSs are the encounter between a single star and a massive black hole binary in the GC (e.g.","Functions Label":1}
{"Functions Text":"Conversions to magnitude are based on the standard zero-points in the Vega system as described in the ACS Data Handbook","Functions Label":2}
{"Functions Text":"At high accretion rate, the inner region of a standard \u03b1-disc","Functions Label":2}
{"Functions Text":"Recent works suggest that the deformation of the magnetic field lines is determined by the parameter \u03b4 (the ratio of the gravity to the magnetic pressure)","Functions Label":0}
{"Functions Text":"Bayesian reconstruction methods have become increasingly popular in cosmology and have been applied in a range of different applications such as","Functions Label":0}
{"Functions Text":"weak lensing","Functions Label":0}
{"Functions Text":"After 1500 A.D., the GNP moved to Canada. This caused the geomagnetic field latitude of China to decrease considerably. Meanwhile, the field intensity decreased to its minimum value in the last 2000 yr. Under these conditions, it would have been very rare to observe the aurora in most places in China after the 16th century, just like the present case","Functions Label":0}
{"Functions Text":"In what are sometimes called \u2018semi-empirical\u2019 methods [also called subhalo abundance matching (SHAM) or halo occupation distribution (HOD) models; see Wechsler & Tinker 2018], galaxy properties are mapped on to the properties of dark matter haloes such that a set of observational quantities is reproduced","Functions Label":0}
{"Functions Text":"In the case of midplane spiral structures, their origin may be linked to the presence of a companion\u2014stellar, fly-by, or planetary","Functions Label":0}
{"Functions Text":"However, it differs from Eq. (2) in","Functions Label":6}
{"Functions Text":"The accretion of gas and the dynamical evolution of BSBHs are likely to be coupled","Functions Label":0}
{"Functions Text":"such that the occurrence rate of BSBHs depends on the initial conditions and gaseous environments at earlier phases","Functions Label":0}
{"Functions Text":"For comparison, we also show the integral number count","Functions Label":2}
{"Functions Text":"and from the high-resolution ALMA follow-up of LESS","Functions Label":2}
{"Functions Text":"The dust distribution away from the midplane is better captured by hydrodynamical simulations than by simple prescriptions relying on a parameterization of the turbulence strength (see, e.g.,","Functions Label":0}
{"Functions Text":"since it depends on the particular source of turbulence.","Functions Label":0}
{"Functions Text":"These pads provide the digital readout of the detector up to 22 particles m\u22122, allowing the count of the air shower charged particles without any significant saturation up to primary cosmic-ray energies of about 200 TeV","Functions Label":0}
{"Functions Text":"Analysis of the stellar clusters in the complex reveals them to have ages of 1.5 Myr for Danks 1 and 3 Myr for Danks 2,with the former possibly being triggered by the latter","Functions Label":0}
{"Functions Text":"In order to fulfil equation (2) during the whole inbound orbit, cometary activity is driven by at least the five ices listed in Table 2, reporting the nucleus and gas coma parameters computed by means of the activity model","Functions Label":2}
{"Functions Text":"using GALEX data from","Functions Label":2}
{"Functions Text":"we find log\u2009FFUV\/FJ = \u22122.49, log\u2009FNUV\/FJ = \u22122.11","Functions Label":2}
{"Functions Text":"Analytical fits of these neutron-star EoSs have been constructed in order to facilitate their inclusion in astrophysical simulations","Functions Label":0}
{"Functions Text":"whereas in","Functions Label":5}
{"Functions Text":"and Mennella et al. (1998) and in the present study this correction was not applied","Functions Label":5}
{"Functions Text":"The majority of observed SPDBs are connected to solar flares","Functions Label":0}
{"Functions Text":"On the other hand, the annual variation in the IMF polarity in the band of 256\u2013512 days, which is referred to the Rosenberg\u2013Coleman effect","Functions Label":2}
{"Functions Text":"The authors indicated that such a result should be attributed to a more stable and flat heliospheric current sheet that only appears in the ascending phase of solar cycles and strong disturbance of the heliospheric current sheet that is present in the declining phase and minimum time of solar cycles, and the Rosenberg\u2013Coleman effect had been confirmed by the IMF Bx component during 1964\u20132002.","Functions Label":1}
{"Functions Text":"Such a model is used to study","Functions Label":0}
{"Functions Text":"flows of accreting matter in neutron stars","Functions Label":0}
{"Functions Text":"This can be done either in the EoS parameterizing methods","Functions Label":5}
{"Functions Text":"or the nonparametric approach","Functions Label":5}
{"Functions Text":"and the results are well consistent with each other.","Functions Label":5}
{"Functions Text":"Moreover, in DR processes, the H ejection is in general favoured more than H2 ejection","Functions Label":1}
{"Functions Text":"Currently, there are two possible scenarios on the origin of S0 galaxies.","Functions Label":0}
{"Functions Text":"The other is that S0 galaxies are intrinsically different from spiral galaxies since their formation","Functions Label":0}
{"Functions Text":"In this respect, GRGs have a crucial role in the acceleration of cosmic rays over large cosmic scales (e.g.","Functions Label":3}
{"Functions Text":"Gap-type emission models offer a promising alternative and different realizations have been proposed in the literature (e.g.,","Functions Label":3}
{"Functions Text":"The correlated angular momenta result into correlated inclination angles of neighbouring galaxies and thus ultimately into correlated ellipticities","Functions Label":2}
{"Functions Text":"We address this issue by calculating local number density of galaxies using kth nearest neighbour method","Functions Label":2}
{"Functions Text":"It is supported by correlated optical\/\u03b3-ray flares in FSRQs (e.g.,","Functions Label":5}
{"Functions Text":"Thus, for planets in the Solar System, it was shown both in the observations","Functions Label":1}
{"Functions Text":"that the presence of a weak magnetic field can intensify atmospheric escape.","Functions Label":1}
{"Functions Text":"Numerous investigations of tidal activity on extrasolar planets have been conducted, with a range of topics","Functions Label":0}
{"Functions Text":"issues of spin dynamics","Functions Label":0}
{"Functions Text":"The inner few arcseconds is a complex mix of","Functions Label":0}
{"Functions Text":"polarized, broad optical emission lines due to scattering by dust","Functions Label":0}
{"Functions Text":"It has been suggested","Functions Label":0}
{"Functions Text":"that the enthalpy fluxes associated with both evaporating and condensing plasma are at all times in approximate balance with the excess or deficit of the heat flux relative to the transition region radiation loss rate.","Functions Label":0}
{"Functions Text":"Some of these fragments have been recovered","Functions Label":0}
{"Functions Text":"and 2016\u20132017","Functions Label":0}
{"Functions Text":"For the purposes of this study, we adopt the composition of type I CAIs as the representative value of refractory objects because they are seemingly the most abundant type and lack the characteristic elemental depletions of other CAI groups (e.g.,","Functions Label":2}
{"Functions Text":"Hence, we think that the radio jet is transferring its energy and momentum to the ambient medium through an extended shock front, which creates turbulence in a dense clumpy ISM. Such a great impact of the radio jet has been observationally shown in many cases (e.g.","Functions Label":5}
{"Functions Text":"We also plot the results of previous blank-field surveys","Functions Label":2}
{"Functions Text":"This model has been previously used for the modelling of planetesimal formation in PPDs","Functions Label":0}
{"Functions Text":"The size distribution is probably shallower","Functions Label":1}
{"Functions Text":"All our low-mass galaxies are characterized by moderate Ly\u2009\u03b1 luminosities in a narrow range between 1042.19 and 1042.74\u2009erg\u2009s\u22121 (Fig. 6a), that are slightly below the values for confirmed LyC leakers (blue filled circles) by Izotov et al. (2016a,b, 2018a,b) and high-redshift galaxies (grey open circles) by Ouchi et al. (2008), Hashimoto et al. (2017), Jiang et al. (2018), Matthee et al. (2017), Matthee et al. (2018), Sobral et al. (2018), but are \u223c1 order of magnitude higher than those for GPs (black asterisks;","Functions Label":1}
{"Functions Text":"While the fluorescent signal powered by the diffuse metagalactic UV background","Functions Label":0}
{"Functions Text":"with an expected surface brightness (SB) of $\\rm SB_{Ly\\alpha }\\sim 10^{-20} \\,erg \\,s^{-1} \\,cm^{-2} \\,arcsec^{-2}$","Functions Label":0}
{"Functions Text":"is still out of reach for current optical instrumentation (but see","Functions Label":0}
{"Functions Text":"Ly\u2009\u03b1 fluorescence is predicted to be boosted up into the detectable regime in the vicinity of bright ionizing sources, as luminous quasars","Functions Label":0}
{"Functions Text":"In literature studies, CO line ratios do appear enhanced in low-metallicity regions or galaxies (e.g.,","Functions Label":0}
{"Functions Text":"The NFW profile has been shown to provide an overall good agreement with observations and simulations over a broad range of scales in GR","Functions Label":5}
{"Functions Text":"While some phenomena exist in the early Universe, such as quasars or radio galaxies, which are so powerful and intrinsically bright that they have been able to serve as beacons to early searches near the epoch of H I reionization (z ~ 5.5\u201310,","Functions Label":0}
{"Functions Text":"the bulk of the galaxy population residing in the early Universe does not contain such phenomena","Functions Label":0}
{"Functions Text":"Common definitions include","Functions Label":2}
{"Functions Text":"or the $\\rm [O\\, III]$ flux weighted radius","Functions Label":2}
{"Functions Text":"As evolved stars ascend the RGB, C and N abundances may be changed by first dredge-up","Functions Label":0}
{"Functions Text":"and extra mixing","Functions Label":0}
{"Functions Text":"The discovery of this correlation has led to an increased interest on the abundances of other elements in planet hosts(e.g.","Functions Label":3}
{"Functions Text":"However, these studies do not explore lower metallicities, despite available evidence for the existence of a low-metallicity ISM in the past through the discovery of stars","Functions Label":3}
{"Functions Text":"as well as several others with $\\rm {[Fe\/H]} \\lt -5$","Functions Label":3}
{"Functions Text":"while BL Lacs are powered by an advection-dominated, low radiative efficiency accretion flow","Functions Label":0}
{"Functions Text":"Given the rh = 20 au distance of our measurements (and the expected large size of 2014 UN271), we adopted a beaming factor \u03b7 = 1.175 \u00b1 0.42, based on measurements of 85 Centaurs and TNOs","Functions Label":2}
{"Functions Text":"At very large densities, though, owing to the increased dust absorption coefficient, the gas becomes opaque to its own radiation. This is sometimes referred to as the opacity limit","Functions Label":0}
{"Functions Text":"At this point, the fragmentation is halted, setting a scale below which no fragments form.","Functions Label":0}
{"Functions Text":"On scales up to a few Mpc from the nearest galaxy cluster, possibly along filaments, only a few diffuse synchrotron sources have been reported","Functions Label":0}
{"Functions Text":"The inertial range, which is dominated by magnetohydrodynamic (MHD) turbulence, follows the cascade models with spectral indices \u03b1i from around 3\/2 to 5\/3","Functions Label":0}
{"Functions Text":"The expanding box uses these comoving coordinates, approximating the spherical coordinates by the Cartesian ones","Functions Label":2}
{"Functions Text":"To assess the star formation contribution to the H\u03b1 flux, we consider lines from the most extreme AGN photoionisation models of Groves et al. (2004), to the location of solar metallicity star-forming galaxies (see also","Functions Label":2}
{"Functions Text":"In addition, the theoretical definition of cores also depends on whether the star-formation scenario is quasi-static or dynamic. In the former scenario, cores are gas condensations sufficiently dense to be on the verge of gravitational collapse, and they convert the core gas into stars","Functions Label":0}
{"Functions Text":"A commonly used tactic to increase the efficiency and improve the stability of these simulations is to artificially increase the luminosity (or nuclear energy for convective cores or burning shells) and to modify the thermal diffusivity of the reference stellar model. This tactic is common and has been used, for example, in","Functions Label":0}
{"Functions Text":"This approach is used to increase the Mach number of the convective flow, reducing the disparity between advective and acoustic timescales, improving the efficiency of time-explicit codes limited by the Courant\u2013Friedrich\u2013Levy constraint. It is also used to provide numerical stability or to accelerate the thermal relaxation. But no examination of its potentially far-reaching impact has been conducted.","Functions Label":0}
{"Functions Text":"The beam fluxes used had values of 3 \u00d7 109, 1 \u00d7 1010, and 3 \u00d7 1010 erg cm\u22122 s\u22121, while the low-energy cutoff EC covered the parameter space where flare values are usually found (20\u2013120 keV;","Functions Label":2}
{"Functions Text":"Galaxies satisfying all three of these criteria are rare; in principle the Milky Way GC databases could be used, but cluster-to-cluster foreground reddenings differ strongly, the published SDSS indices","Functions Label":1}
{"Functions Text":"show considerable scatter versus metallicity, and the variety of studies from which the UBVRI indices were derived are completely different from the SDSS survey, so that aperture-size mismatches are significant.","Functions Label":1}
{"Functions Text":"However, such a dynamical system is linearly unstable to parametric instabilities and large-amplitude Alfv\u00e9n waves are known to decay into compressible and secondary Alfv\u00e9nic modes through three- or four-wave resonances that lead to a variety of parametric instabilities, depending on the plasma beta and dispersive effects, such is the case of parametric decay","Functions Label":0}
{"Functions Text":"Recent works on laboratory measurements of cohesion between crystalline water-ice particles at vacuum conditions provided encouraging results that dust particles composed of water ice might be much more cohesive than previously believed","Functions Label":0}
{"Functions Text":"This equation and the condition $F_i-q^\\prime _if\\ne 0$ furnish the generalized NBH equations","Functions Label":2}
{"Functions Text":"In the avoidance scheme, smooth-spectrum foregrounds should, in the ideal case, occupy a wedge\u2013shaped region of the two\u2013dimensional power spectrum space (where the wavenumber k can be decomposed into k\u22a5 and $k_\\Vert$ that are the transverse and line-of-sight wave numbers, respectively) whereas the remaining area \u2013 the so-called EoR window \u2013 is dominated by the 21 cm emission","Functions Label":0}
{"Functions Text":"Maybe we do not need to intentionally take to heart such the classical dichotomy, because waves and reconnections may interact with each other","Functions Label":3}
{"Functions Text":"The cluster merger induced relatively strong shocks, which travelled through the ICM, accelerated particles to produce relics towards the north and south of the cluster","Functions Label":0}
{"Functions Text":"On kpc scales and in the discs of nearby star-forming galaxies, \u03c4dep is approximately constant around 1\u20132 Gyr","Functions Label":0}
{"Functions Text":"Several other works","Functions Label":0}
{"Functions Text":"applied a Gaussian process, principal component analysis (PCA), and deep learning neural networks to radiative transfer models of SNe.","Functions Label":0}
{"Functions Text":"A good agreement between observations and theoretical predictions for the Galaxy is obtained by models that are based on the assumption that the disc formed via the infalling of gas","Functions Label":0}
{"Functions Text":"Following this, higher level calculations on the electronic structure, rotational constants, and harmonic vibrational frequencies of each isomer were performed using CCSD(T) together with the Dunning basis sets aug-cc-pV(X+d)Z (X = T, Q, 5)","Functions Label":2}
{"Functions Text":"Our investigation is based on a magnetospheric model that synthesizes the corotating magnetosphere model and the vacuum model","Functions Label":2}
{"Functions Text":", in which multiple quasi-stable magnetospheric states are described by the parameter y such that the charge filling fraction of a state corresponds to a y value and a change in the charge filling fraction corresponds to a change of state which is signified by a change in y.","Functions Label":2}
{"Functions Text":"In some cases, the stellar system resulting from the merger event may show significant internal rotation (in fact, for many years this has been the preferred dynamical route to form rotating star clusters; see","Functions Label":0}
{"Functions Text":"Mechanisms suggested to produce these small-scale magnetic helicity fluxes are: advection of magnetic fields by an outflow from the disk through the galactic fountain or wind","Functions Label":0}
{"Functions Text":"For example, in Mrk 501 the shift in both peaks strongly implies the same particle distribution for the overall emission, while for OJ 287 the shift of only the high-energy peak can be reproduced by either inverse Compton scattering of the broad-line region photon field","Functions Label":1}
{"Functions Text":"Secondly, although a fraction of LBV stars are isolated (e.g.","Functions Label":1}
{"Functions Text":"For internal consistency, all EWs in this work have been adjusted to the measurement scale of","Functions Label":2}
{"Functions Text":"by using this relation.","Functions Label":2}
{"Functions Text":"The shock is then revived by adding an energy injection following the parameterized method of","Functions Label":2}
{"Functions Text":"In particular, the CN index distribution shows the largest spread. Note that a bimodality or a large spread in CN distribution is generally observed in most GCs","Functions Label":5}
{"Functions Text":"A similar feature has also been observed","Functions Label":5}
{"Functions Text":"CB 3 and CB 246","Functions Label":5}
{"Functions Text":"As the SN explosions start occurring within the cavity formed by the stellar wind bubbles, super-bubbles are created (e.g.","Functions Label":0}
{"Functions Text":"), which may eventually reach kiloparsec sizes.","Functions Label":0}
{"Functions Text":"In particular, it was noted that \u201cthe Simpson et al. (2017) stars do not define a red giant branch in the theoretical plane, suggesting that their parameters are not correct\u201d (Fig. 1 of","Functions Label":1}
{"Functions Text":"In the non-rotating case, the GW emission from the post-bounce phase has been studied using self-consistent 3D simulations by many groups","Functions Label":0}
{"Functions Text":"High temperatures in the accretion disc can induce exothermic nucleosynthesis too","Functions Label":0}
{"Functions Text":"All these processes taken together in an advective disc will produce very hot jet base.","Functions Label":0}
{"Functions Text":"Magneto-Rossby waves are basic mechanism in variability of various objects in plasma astrophysics. Magneto-Rossby waves determine the large-scale dynamics of the Sun and stars","Functions Label":0}
{"Functions Text":"The original function proposed by","Functions Label":6}
{"Functions Text":"(Eq. (6) with q = 0.62, see left column) does provide a good approximation of the observed distributions, when assuming the original \u0398med \u2212 S relation described by Eq. (7), only at flux densities S150 MHz\u227310 mJy (see long-dashed lines). This is perhaps not surprising considering that this relation was calibrated at 1.4 GHz down to a few mJy fluxes. At the lowest flux densities (S150 MHz\u22721 mJy) we need to assume a steepening of the parameter m (see Eq. (8)), to get a good match with observations (dotted line in the top left panel).","Functions Label":6}
{"Functions Text":"Similarly, the peak bolometric luminosity of SN 2012au (\u223c\u2009[6.56 \u00b1 0.70] \u00d7 1042 erg s\u22121) is higher than the mean peak luminosities of SNe Ib and Ic, but still lower than those of SNe Ic-BL","Functions Label":1}
{"Functions Text":"Putting aside large-scale eruptions so as to focus on the quasi-steady input of energy into the corona, it is possible to distinguish three broad magnetic configurations of the solar atmosphere for modelling purposes.","Functions Label":0}
{"Functions Text":"active or enhanced regions","Functions Label":0}
{"Functions Text":"CH3C3N itself may form the protonated species, C4H3NH+, through reactions with the HCNH+ and C2H5+ ions producing HCN and C2H4, respectively","Functions Label":1}
{"Functions Text":"Proton plasma properties provide an alternative to determine the solar wind type","Functions Label":0}
{"Functions Text":"A clear advantage of this approach is that the required observables are available from more spacecraft.","Functions Label":0}
{"Functions Text":"However, if the kink-unstable filament is heated during magnetic reconnection, it is often observed in the AIA 1600 \u212b channels (e.g.,","Functions Label":2}
{"Functions Text":"By comparison, the total background at 850\u2009\u03bcm inferred from COBE-FIRAS is 3.1\u20134.4 \u00d7 104\u2009mJy\u2009deg\u22122","Functions Label":1}
{"Functions Text":"Summing these separate surface brightness densities together, we find that the LBGs with L1700 > 1029 erg s\u22121 Hz\u22121 in our z \u223c 3, 4, and 5 samples comprise around 6\u20138 per cent of the submm background at 850\u2009\u03bcm (where the range of values simply reflects the uncertainty in the COBE-FIRAS result).","Functions Label":1}
{"Functions Text":"In this study, we use the Stratospheric","Functions Label":2}
{"Functions Text":"chemistry schemes.","Functions Label":2}
{"Functions Text":"Compared with simulations by","Functions Label":5}
{"Functions Text":"the diffuse form observed for the ICL is consistent with the scenario where this component formed by stripped material from the outskirts of a galaxy in a close passage with the cD","Functions Label":5}
{"Functions Text":"Although this may suggest better X-ray detection prospects for external galaxy bubbles than our results would imply, we note that these Galactic observations may include a very significant thermal bremsstrahlung contribution from all the gas in the Milky Way halo, which likely extends to a radius of \u223c250\u2009kpc","Functions Label":1}
{"Functions Text":"the Galactic bulge, and gas heated by the shocks associated with the bubble","Functions Label":1}
{"Functions Text":"none of which is included in our model (and could evolve as the bubble ages).","Functions Label":1}
{"Functions Text":"The penultimate point has been widely discussed (e.g.,","Functions Label":0}
{"Functions Text":"involving the role of the flare material and the interacting CMEs on seed particles.","Functions Label":0}
{"Functions Text":"In such a case, to accelerate particles up to an energy Ec via a diffusive mechanism, the mean-free path \u03bbc \u223c rg(\u03b3c, B)2\/s in the shock downstream region, where B is a small-scale field, has to be smaller than Larmor radius in Bjd","Functions Label":2}
{"Functions Text":"These astrophysical observations are furthermore theoretically explained by deep crustal heating due to pycnonuclear reactions","Functions Label":1}
{"Functions Text":"In particular, theoretical studies have shown that the MBH\u2013halo occupation fraction can be low in dwarf galaxies","Functions Label":0}
{"Functions Text":"and even in systems hosting MBHs, their growth is strongly suppressed because of the typically low gas densities in the host (compared to more massive disc galaxies) and the strong impact of supernova explosions, both at low and high redshift","Functions Label":0}
{"Functions Text":"These nebulae, whose first examples were detected in H\u03b1","Functions Label":0}
{"Functions Text":"more recently have been discovered and observed in X-rays and sometimes in radio","Functions Label":0}
{"Functions Text":"However, numerical results (e.g.","Functions Label":1}
{"Functions Text":"show some bending of the jets towards the tail. This bending in numerical models (for slow incompressible ISM flows) is connected with the numerical dissipation inherent in the numerical schemes. Numerical viscosity may cause the boundary layer breakage on the surface of the astropause, which consequently causes the pressure asymmetry that deflects the astropause. This may be the explanation for the fact that the tube of the astropause is always deflected to the tail in the numerical models. The above-described numerical effects have nothing to do with physical dissipation phenomena responsible for the bending of real astrospheres.","Functions Label":1}
{"Functions Text":"The physical dissipation mechanisms (e.g. magnetic reconnection, finite resistivity, Hall effects) should be explored as a possible cause of the astropause bending in the models with slow subsonic ISM flow.","Functions Label":7}
{"Functions Text":"In addition,","Functions Label":1}
{"Functions Text":"claim that previous estimates of the evolution in the RS GLF","Functions Label":1}
{"Functions Text":"were also due to SB effects.","Functions Label":1}
{"Functions Text":"Moreover, the disk formation process has been revealed to be much more complicated for binary and multiple cases,","Functions Label":0}
{"Functions Text":"and in numerical simulations (e.g.,","Functions Label":0}
{"Functions Text":"We test the results in Stanimirovi\u0107 et al. (2014) and","Functions Label":6}
{"Functions Text":"which differ by several factors.","Functions Label":6}
{"Functions Text":"Meanwhile, a similar power-law index of energy distribution for non-repeating FRBs is also found","Functions Label":5}
{"Functions Text":"The results presented here are based on the assumptions that the CBPs do not interact with the material ejected from their binary star. However, numerical studies have indicated that this material is neither lost isotropically from the binary during the CE phase, nor does it all become unbound. Instead, 1\u201310% of the ejecta may fall back into a CB disk according to Kashi & Soker (2011), and Passy et al. (2012) suggest that \u223c80% of the ejected material may remain gravitationally bound to the binary (also see","Functions Label":1}
{"Functions Text":"In recent years, a deficit of star-forming galaxies in the infalling region of clusters has been reported (e.g.","Functions Label":0}
{"Functions Text":"In the local universe, relationships between strong emission line ratios and metallicity can be calibrated to \u00e2\u0080\u009cdirect\u00e2\u0080\u009d electron temperature-determined metallicities from","Functions Label":0}
{"Functions Text":"or photoionization models of star-forming regions","Functions Label":0}
{"Functions Text":"We utilized a sample of ALMA-identified SMGs in the UKIDSS-UDS field, which has been studied in detail with proper SED fittings","Functions Label":2}
{"Functions Text":"Similarly to our observations, the sample of","Functions Label":5}
{"Functions Text":"was drawn from a flux-limited sample produced by the SCUBA-2 Cosmology Legacy Survey","Functions Label":5}
{"Functions Text":"Many authors have studied the global and local reconnection rates and timescales of solar reconnection during solar flares based on analysis of the ribbon motions in the chromosphere","Functions Label":0}
{"Functions Text":"Moreover, if we consider the inverse covariance of the time domain noise as the weights, the GLS estimate is also a minimum variance and a maximum likelihood solution to the problem. However, computation of the solution in such a case may require","Functions Label":1}
{"Functions Text":"or an application of some iterative procedure","Functions Label":1}
{"Functions Text":"These latte typically involve several matrix-vector multiplications at each iteration step.","Functions Label":1}
{"Functions Text":"Moreover, precisely determined DIB profiles","Functions Label":2}
{"Functions Text":"showing a specific substructure pattern each, should facilitate their carrier's identification.","Functions Label":2}
{"Functions Text":"For the radio-loud magnetars, given their large variability, we have chosen the brightest radio pulses reported in the literature (data collected from","Functions Label":2}
{"Functions Text":"detected PAHs on subarcsec scales in about half of their sample of 29 nearby Seyfert galaxies.","Functions Label":0}
{"Functions Text":"They argued that the high column densities in the torus around the AGN would provide shielding that enables PAHs to survive, and the implied central star formation rate density was much higher than in the circum-nuclear region.","Functions Label":1}
{"Functions Text":"A similar conclusion about PAH survival was reached by Esparza-Arredondo et al. (2018) for their sample of 19 AGNs, based on the lack of relation between the X-ray luminosity and a central PAH deficit \u2013 while PAHs were detected in most AGNs, the equivalent width was lower in the centre.","Functions Label":5}
{"Functions Text":"Knots in SS433\u2019s jet can be resolved at radio frequencies using very long baseline interferometry (VLBI) and indicate the presence of highly relativistic electrons","Functions Label":0}
{"Functions Text":", while the baryon content is revealed by emission lines ranging from H and He lines in the optical through to highly ionized Fe lines in the X-rays","Functions Label":0}
{"Functions Text":"Further monitoring, predominantly at frequencies between 0.6 and 15\u2009GHz, has since taken place (e.g.","Functions Label":0}
{"Functions Text":"Multilevel FIR transition lines have now been widely surveyed in local galaxies, originally by ISO (e.g.","Functions Label":0}
{"Functions Text":"Here different line features appear, more or less visible depending on the BH spin and radial distance, such as the clear iron absorption edge that occurs at around \u223c6\u20137 keV (see e.g.","Functions Label":2}
{"Functions Text":"The Galactic sample of post-AGB stars have been found to be a very diverse group of objects","Functions Label":0}
{"Functions Text":"In contrast, a sub-population of backsplash cluster galaxies would be expected to peak significantly at $|\\Delta \\mathrm{V}|\/\\sigma _{r_{200}}\\sim 0$ for values at or beyond our definition of the virial radius, with their fraction reaching zero at some upper limit (e.g.","Functions Label":2}
{"Functions Text":"At the wavelength around 4.6 \u03bcm for Perseus 1 and 3, RNO 91, and AFGL 7009S, there is a hint for another ice component overlapping with the CO absorption feature at 4.67 \u03bcm. Many near-infrared observations have revealed the same feature on the blue wing part of the CO absorption feature","Functions Label":1}
{"Functions Text":"which was suggested as an absorption feature of XCN ice.","Functions Label":1}
{"Functions Text":"Despite the observational evidence, and to keep alive the inherited model,","Functions Label":1}
{"Functions Text":"proposed to decrease the theoretical 60Fe abundance in molecular clouds by assuming that stars more massive than 30 M\u2299 do not explode as SNe. These stars would not contribute to the 60Fe inventory, bringing the theoretical ISM 60Fe\/26Al ratio closer to that of the solar system. Because stars more massive than 30 M\u2299 contribute to less than 50% of the 60Fe production2, this proposition cannot resolve the two orders of magnitude discrepancy between the model and observations.","Functions Label":1}
{"Functions Text":"The orbital phase is calculated using the TEMPO2 package","Functions Label":2}
{"Functions Text":"Although a cavity of 55 astronomical units (au) in radius has been inferred from dust millimeter emission","Functions Label":1}
{"Functions Text":"infrared polarized intensity observations have found no clear evidence for a cavity in scattered light","Functions Label":1}
{"Functions Text":"For the other lines in the 10\u2005\u2212\u200536\u2006\u03bcm interval,","Functions Label":1}
{"Functions Text":"did not report a detection, and we used the data presented in Bernard-Salas et al. (2009) for a total of 15 objects.","Functions Label":1}
{"Functions Text":"These compact remnants","Functions Label":0}
{"Functions Text":"can inject strong energy inputs in the primeval universe (e.g.,","Functions Label":0}
{"Functions Text":"Five clusters from the sample of","Functions Label":2}
{"Functions Text":"covering a wide metallicity range were re-reduced and analysed with our code to ensure that our EWs measurements are on the same scale as the template clusters used to define the metallicity calibration.","Functions Label":2}
{"Functions Text":"These processes have been studied both by investigating normal modes of the inhomogeneous structure","Functions Label":0}
{"Functions Text":"One striking problem is the ${\\rm ^{14}N}\/{\\rm ^{15}N}$ isotopic ratio of nitrogen in comets. Its average value, 144 \u00b1 3","Functions Label":3}
{"Functions Text":", is three times lower than the bulk ratio of 441 \u00b1 6 in the protosun as inferred from solar wind measurements","Functions Label":3}
{"Functions Text":"The reasons for these different ratios remain elusive, casting doubts on our understanding of the origin of the composition of comets and more generally of the origin of nitrogen in the Solar system.","Functions Label":3}
{"Functions Text":"Over the entire mission, the deceleration of the solar wind using the mean speed of the particles is much more limited than the deceleration shown by the norm of the bulk velocity","Functions Label":1}
{"Functions Text":": there is more kinetic energy in the solar wind than the bulk velocity vector would let us think.","Functions Label":1}
{"Functions Text":"At small scales (a few tens of kpc), there is substantial evidence from observations and simulations for a decrement of metallicity and an enhancement of star-formation activity in galaxy close pairs, merging, and interacting systems compared to isolated, field galaxies, mostly attributed to the interaction-induced inflow of metal-poor gas from the periphery of interacting galaxies to the center, diluting their metal content, and increasing their gas fuel for star-formation","Functions Label":1}
{"Functions Text":"The quasar-level AGN activity","Functions Label":3}
{"Functions Text":"at the center is blocked by the thick dusty torus acting as the \u201ccoronograph\u201d","Functions Label":3}
{"Functions Text":"this makes HzRGs true obscured type-2 quasars, allowing us to probe their host galaxies and CGM without strong AGN contamination (e.g.","Functions Label":3}
{"Functions Text":"for radio-quite type-2 sources, see","Functions Label":3}
{"Functions Text":"This is in contrast with previous studies","Functions Label":6}
{"Functions Text":"where the backward modeling approach is employed to constrain the probability of mass for a given richness,","Functions Label":6}
{"Functions Text":"These studies are based on the hypothesis that magnetic fields are passively transported by the plasma flow and provide a characterisation of advection and diffusion processes in the quiet photosphere from granular to supergranular scales (see, e.g","Functions Label":0}
{"Functions Text":"These studies reveal an anomalous scaling of magnetic field transport with a superdiffusive character consistent with a Levy walk inside supergranules and a more Brownian-like motion in their boundary.","Functions Label":0}
{"Functions Text":"These studies pointed out the large magnetic temporal variability and the critical effect of stellar rotation and mass on magnetic field generation through dynamo mechanism, leading in some parameter regimes to configurations with cyclic activity","Functions Label":0}
{"Functions Text":"The H\u03b2 BEL is considered to be rotating gas in a flat \u201cpancake-like\u201d region in which the normal to the BEL disk is parallel to the jet axis","Functions Label":2}
{"Functions Text":"Thus, the FWHM that appears in Equation (4) depends on the LOS.","Functions Label":2}
{"Functions Text":"This method has since identified a large number across the extragalactic sky, i.e., more than 100 lensed candidates at z > 1","Functions Label":0}
{"Functions Text":"Observations from local galaxies","Functions Label":0}
{"Functions Text":"have shown H2O emission to be ubiquitous with intensities as bright as CO lines.","Functions Label":0}
{"Functions Text":"Such high-precision RV surveys include those being undertaken currently with","Functions Label":0}
{"Functions Text":"and CHIRON","Functions Label":0}
{"Functions Text":"We estimated the precession period using the theory from Terquem et al. (1999) and the binary parameters taken from","Functions Label":2}
{"Functions Text":"\u2013 Mh = 0.8M\u2299 (the mass of the hot WD companion), Mp\u2215Mh = 1.65 (where Mp is the mass of the primary companion), D = 15.5 AU (the mean semi-major axis of the system), and e = 0.25 (eccentricity).","Functions Label":2}
{"Functions Text":"Driven by dynamical friction and global torques from this disc, the pair of MBHs decays very efficiently down to separations of the order of \u223c1\u20130.1 pc, where it forms a gravitationally bound binary","Functions Label":0}
{"Functions Text":"and the kilonova AT 2017gfo in the ultraviolet\u2013optical\u2013infrared band","Functions Label":0}
{"Functions Text":"as well as the combination of the H2O-K2 index with pEWs to derive [Fe\/H]","Functions Label":0}
{"Functions Text":"These have revealed a surprising diversity in the orbital alignments (for example","Functions Label":0}
{"Functions Text":"which is in contrast to the Laplacian ideals of planets forming inside a flat disk, coplanar with the stellar equator and staying there","Functions Label":1}
{"Functions Text":"Following our previous work","Functions Label":2}
{"Functions Text":"we have adopted here a G+L profile fit.","Functions Label":2}
{"Functions Text":"The tilt angle compared to a completely edge-on orientation was suggested to be 3\u00b0 in the model of Hogerheijde et al. (1995) and","Functions Label":2}
{"Functions Text":"A tilt angle of 3\u00b0 is equivalent to an enhancement factor of 20 for the measured column densities.","Functions Label":2}
{"Functions Text":"The Largest Linear Sizes (LLS) and radio powers of relics are correlated, as well as the integrated spectral index and the radio power","Functions Label":0}
{"Functions Text":"An alternative and attractive pathway for seed BH formation is via the so-called direct collapse","Functions Label":1}
{"Functions Text":"where a supermassive star (SMS) with ${\\sim } 10^{5}\\, \\mathrm{M}_{\\odot }$ collapses into a BH with a similar mass by general relativistic instability","Functions Label":1}
{"Functions Text":"Both kinds of event are too common to be entirely explained with PPI+CC progenitors, and it is likely that both classes contain events with a diversity of physical mechanisms (e.g.,","Functions Label":1}
{"Functions Text":"The task of estimating stellar ages has been addressed by several authors and lots of different methods are found in the literature. For instance, there are (i) empirical methods, which use a deterministic relation between a given parameter and the age of a star (first proposed by Skumanich 1972). This is the case of","Functions Label":0}
{"Functions Text":"decay of chromospheric activity","Functions Label":0}
{"Functions Text":"Adopting an expansion velocity equal to half the velocity interval where the structure is observed, Vexp = 7.0 \u00b1 1.3 km\u2009s\u2212 1 , the molecular mass given in Table 1 and the atomic and ionized masses estimated by","Functions Label":2}
{"Functions Text":"1450 and 3000 M\u2299, respectively, we obtain Ekin = (2.5 \u00b1 1.0) \u00d7 1049 erg, assuming a 40\u2009per\u2009cent error for the masses.","Functions Label":2}
{"Functions Text":"performed SPH (smoothed particle hydrodynamics) simulations and studied water loss in planetary embryos and water retained in significant fragments after a collision. They concluded that the impact velocity and the impact angle play a key role in the water loss of a planetary embryo after a collision.","Functions Label":0}
{"Functions Text":"We leave a more detailed investigation of this change to future work. Here, we simply mention two possible explanations: The change in slope may be a reflection of the differences in the dynamical state (e.g. mass-to-light ratio; M\/L) at the outskirts of BCGs","Functions Label":7}
{"Functions Text":"Among the four s-process elements mentioned above, GES provides the abundances of Y II (the first s-process peak element) and Ba II (the second s-process peak element) for all our sample stars. Their abundances behave differently in the Galactic thick and thin discs","Functions Label":1}
{"Functions Text":"In the presence of molecular clouds surrounding the SNR, escaping CRs can illuminate the clouds through pp interactions, producing gamma-ray emission with a flux depending on the amount of nuclear CRs released by an SNR and the diffusion coefficient in the interstellar medium (ISM;","Functions Label":0}
{"Functions Text":"By default, these techniques are applicable only to single-frequency sky images: even for multiwavelength observatories such as the Herschel Space Observatory","Functions Label":0}
{"Functions Text":"or Planck","Functions Label":0}
{"Functions Text":"the standard detection pipelines have produced individual source catalogs for each frequency band (see e.g.,","Functions Label":0}
{"Functions Text":"The next logical step is to boost the signal of faint sources by combining the different bands into a single detection, that is, \u201cmultifrequency detection\u201d.","Functions Label":3}
{"Functions Text":"The derived N(H i) is an order of magnitude less than a typical value through a disk of a spiral galaxy with stellar mass >1010 M\u2299, measured by The H i Nearby Galaxy Survey (THINGS","Functions Label":1}
{"Functions Text":"Open clusters are a valuable alternative, being on average younger","Functions Label":0}
{"Functions Text":"and therefore a better tracer of the gradients in the disc out of which the most recent stars formed.","Functions Label":0}
{"Functions Text":"While tides on the progenitor of the second-born black hole can spin up the progenitor star","Functions Label":1}
{"Functions Text":"this effect can be counteracted by mass loss in stellar winds, and more detailed simulations find only low or moderate spin increases due to tides","Functions Label":1}
{"Functions Text":"It is particularly important to understand if cluster mergers","Functions Label":3}
{"Functions Text":"or, alternatively, if they have no direct effect (e.g.","Functions Label":3}
{"Functions Text":"The possible presence of dust in the habitable zones of nearby main-sequence stars is considered a major threat for the direct imaging and characterization of Earth-like extrasolar planets (exo-Earths) with future dedicated space-based telescopes. Several independent studies have addressed this issue and concluded that visible to mid-infrared direct detection of exo-Earths would be seriously hampered in the presence of dust disks 10 to 20\u00c2 times brighter than the solar zodiacal cloud assuming a smooth brightness distribution (e.g.,","Functions Label":0}
{"Functions Text":"This model was successfully applied to","Functions Label":0}
{"Functions Text":"as well as atoll sources","Functions Label":0}
{"Functions Text":"so it could be a universal model for NS-LMXBs.","Functions Label":0}
{"Functions Text":"The overall incidence rate of magnetic upper main sequence stars in close binaries is less than 2 per cent","Functions Label":1}
{"Functions Text":"although this fraction is significantly higher if one includes wide long-period systems","Functions Label":1}
{"Functions Text":"The patchy beam scenario is one of the common beam models that has been used to explain the emission properties of pulsars (see","Functions Label":0}
{"Functions Text":"Previous studies showed that WL masses obtained from the tangential shear fitting were biased low up to 10 per\u2009cent with a scatter of \u223c25 per\u2009cent","Functions Label":0}
{"Functions Text":"The main source of the bias are due to substructures and triaxiality. When a cluster whose major axis is perpendicular to the line of sight, i.e elongated in the sky-plane, a mass obtained with the spherical NFW profile is typically underestimated.","Functions Label":0}
{"Functions Text":"Observations indicate that the abundance of SiO does not differ significantly between envelopes around M-, S-, and C-type stars, although in all them the SiO abundance decreases with increasing mass-loss rate","Functions Label":1}
{"Functions Text":"IRAS 16293-2422 (hereafter IRAS 16293) was chosen for this work as the quintessential example of such an object. IRAS 16293 is adequate for this role because formaldehyde has previously been detected with notable variations in abundances in three differentiated regions of its protodisk","Functions Label":3}
{"Functions Text":"Being associated with old stellar populations, they represent the basis of an alternative Population II distance scale","Functions Label":0}
{"Functions Text":"more suitable to calibrate secondary distance indicators that are not specifically associated with spiral galaxies (e.g. the globular cluster luminosity function, see","Functions Label":0}
{"Functions Text":"and references therein).","Functions Label":0}
{"Functions Text":"The difference between the Saro et al. (2013) and","Functions Label":1}
{"Functions Text":"galaxy scaling relations depends on the details of the semi-analytic and hydrodynamical implementations used in Saro et al. (2013) and","Functions Label":1}
{"Functions Text":"respectively.","Functions Label":1}
{"Functions Text":"Still several schemes have been developed to define groups within galaxy catalogues. They mainly invoke Friends of Friends (FoF) like algorithms based on projected separation, radial velocities and even luminosities to identify what are called \u2018groups\u2019 of galaxies (e.g.","Functions Label":0}
{"Functions Text":"Possibly the material is accelerated by radiation pressure","Functions Label":0}
{"Functions Text":"or cosmic rays (CRs; e.g.","Functions Label":0}
{"Functions Text":"but alternatively the high-speed cool gas may be due rapid radiative cooling in some situations.","Functions Label":0}
{"Functions Text":"In addition, it also shows evidence of relativistic jets","Functions Label":0}
{"Functions Text":"Although a supermassive BH can be modeled by adding a Keplerian potential, it is much simpler to model the BH as this small Gaussian","Functions Label":2}
{"Functions Text":"This mechanism would lead to tori that are a few tens of parsec wide and are dynamic, evolving structures as proposed to interpret several recent observational studies and compilations (e.g.,","Functions Label":1}
{"Functions Text":"ROSINA observations provided evidence that this comet is formed from pristine material that has not been significantly altered after its formation in the first Myr of the solar nebula stage. The high abundance of","Functions Label":0}
{"Functions Text":"of molecular oxygen","Functions Label":0}
{"Functions Text":"all indicate that comet 67P formed at low temperature and did not experience any substantial global-scale heating after its formation.","Functions Label":0}
{"Functions Text":"However, laboratory and theorectical studies showed that quantum tunnelling does not contribute much to the mobility of H atoms on silicate, carbonaceous or solid amorphous water (ASW) surfaces","Functions Label":1}
{"Functions Text":"Previous infrared spectroscopy failed to clearly detect the signatures of ongoing active star formation at the central few arcsec region of the NGC 1068 nucleus due to the lack of polycyclic aromatic hydrocarbon (PAH) emission features","Functions Label":1}
{"Functions Text":"which are a good probe of star formation activity","Functions Label":1}
{"Functions Text":"However, the proposed astrophysical pathways to mergers remain highly debated. Possible compact-object merger pathways include isolated binary evolution","Functions Label":0}
{"Functions Text":"individual periodic signals or continuous waves (CWs","Functions Label":0}
{"Functions Text":"Combining different samples from various instruments at different redshifts therefore inevitably introduces ENLR size\u2013luminosity relations with different slopes \u03b1 depending on the details of target selection and analysis approaches. Slopes ranging from","Functions Label":1}
{"Functions Text":"\u03b1\u2004=\u20040.25\u2005\u00b1\u20050.02","Functions Label":1}
{"Functions Text":"are reported in the literature.","Functions Label":1}
{"Functions Text":"Growing indirect observational evidence suggests that magnetars could act as the central engines of both LGRBs and short-duration GRBs","Functions Label":7}
{"Functions Text":"Different approaches of subgrid models were explored","Functions Label":0}
{"Functions Text":"to mechanical feedback where the momentum boost during the unresolved adiabatic phase is calibrated through small-scale ISM simulations and injected into the ISM","Functions Label":0}
{"Functions Text":"Simulations of dwarf galaxies in recent years have often adopted one of these approaches for SN feedback. Although many are considered successful in reproducing observations, few attempts have been made to compare these models in full cosmological simulations. It is therefore important to gauge how the evolution of simulated dwarf galaxies (especially at the low mass end) is dependent on feedback models, in order to provide a more robust model with realistic uncertainties for future observations.","Functions Label":3}
{"Functions Text":"Both observations and simulations have suggested that there may be a positive trend between the mean black hole accretion rate and star-formation rate (SFR; e.g.,","Functions Label":1}
{"Functions Text":"However, recent observations of the pickup helium focusing cone using the Plasma and Suprathermal Ion Composition (PLASTIC","Functions Label":2}
{"Functions Text":"on board the Solar and Terrestrial Relations Observatory Ahead (STEREO A) spacecraft measured the peak density and determined the inflow longitude to be","Functions Label":2}
{"Functions Text":"After first being reported in the Earth\u2019s magnetosheath","Functions Label":0}
{"Functions Text":"Therefore, GRB afterglows are good probes of burst environment and the interstellar dust and gas in distant, star-forming galaxies","Functions Label":3}
{"Functions Text":"The determination of the magnetic configuration is also based on a method proposed by Chen et al. (2014), i.e., those filaments that follow Martin's Rule","Functions Label":2}
{"Functions Text":"are of the inverse-polarity type, and those that disobey Martin's Rule are of the normal-polarity type.","Functions Label":2}
{"Functions Text":"Complementing these observations, the spectroscopic confirmation","Functions Label":0}
{"Functions Text":"of over a dozen sources has seen impressive advances with ground-based spectroscopy (e.g., probing the rest-frame UV and FIR with Keck\/MOSFIRE, VLT\/X-Shooter, and ALMA), particularly for the brightest and rarest objects.","Functions Label":0}
{"Functions Text":"and $\\mathcal {G}(z) = g(z)\/g_0$, with g(z) as the growth factor at redshift z and g0 = g(z = 0) (e.g.","Functions Label":2}
{"Functions Text":"found a positive correlation between flux and spectral slope for a sample of bright RXTE AGN in the 2\u201310\u2009keV band. This could affect the relative fluxes seen in our sample which are plotted in Fig. B.1. We have attempted to quantify this for the different detectors used in the creation of our light curves.","Functions Label":2}
{"Functions Text":"In response, shock acceleration transport models were developed in recent years based on the numerical solutions of the focused transport equation","Functions Label":0}
{"Functions Text":"to take advantage of the fact that focused transport is not restricted to small pitch-angle anisotropies.","Functions Label":0}
{"Functions Text":"The fit also provided a low value of electron temperature (kT) consistent with the high value of \u03b2 obtained","Functions Label":5}
{"Functions Text":"The variability within the GRMHD models was found to be an important limitation for constraining black hole parameters, as attested by, for example, the small difference in recovered parameters between the EHT2021 and EHT2021+ arrays. The analysis pipeline may be extended to include a characterization of the source variability as part of the model selection process (e.g.,","Functions Label":7}
{"Functions Text":"which could improve the constraining power beyond the averaging method introduced here.","Functions Label":7}
{"Functions Text":"Many other authors, in an attempt to contribute to the solution of the cuspy-core problem, performed the RC decomposition considering a constant M\/L","Functions Label":0}
{"Functions Text":"Investigations show the layered accretion in the inner disk, where the midplane region is \u201cdead\u201d due to low ionization while the surface layer is \u201cactive\u201d due to sufficient ionization","Functions Label":0}
{"Functions Text":"The traditional habitable zone concept assumes a planet with a functioning silicate-weathering feedback and a positive CO2 greenhouse effect","Functions Label":0}
{"Functions Text":"Global glaciation may be triggered on such a planet through a rapid drawdown of atmospheric CO2 that reduces q below the thresholds at which the non-Snowball states disappear.","Functions Label":0}
{"Functions Text":"For \u03c30 \u2273 2.45, the spread of \u03b7 for the observed galaxies (e.g.","Functions Label":1}
{"Functions Text":"broadens and spans both positive and negative \u03b7 values. In fact, majority of the galaxies tend to have positive \u03b7s. This change in behaviour is well known.","Functions Label":1}
{"Functions Text":"Nowadays, global simulations of convective dynamos are able to reproduce cyclic magnetic fields and dynamo solutions resembling many features of the solar magnetic field evolution","Functions Label":5}
{"Functions Text":"Several groups have been devoted to searching for new CL-AGNs, and tens of candidates have been discovered based on large optical and X-ray surveys, such as the Sloan Digital Sky Survey (e.g.,","Functions Label":0}
{"Functions Text":"Note that even in longer time spans, such as from cycle 1 to 24, the sunspot number seems to vary periodically in different periods, like the often-discussed Gleissberg cycle","Functions Label":0}
{"Functions Text":"Radial migration of stars via cold torquing, also known as \u201cchurning,\u201d by a bar and spiral waves","Functions Label":2}
{"Functions Text":"then allows for the populations to spatially overlap in the solar neighborhood.","Functions Label":2}
{"Functions Text":"In Fig. 11 (upper panels) we show the evolution of the spectral break measured through the DB definition","Functions Label":2}
{"Functions Text":"as well as the relative strength (the ratio) between the two (lower left panel).","Functions Label":2}
{"Functions Text":"We use the Mishima et al. (1983) formulation (see Appendix of","Functions Label":2}
{"Functions Text":"Examples of relics in this category are those in","Functions Label":0}
{"Functions Text":"and Abell 85","Functions Label":0}
{"Functions Text":"A few CTTSs binaries are thought to potentially be accreting through accretion streams. These include DQ Tau","Functions Label":0}
{"Functions Text":"None of these stars shows the type of H\u03b1 variations seen in PTFO 8-8695 where the accretion-related emission appears to move from one side of the line profile to the other as it spirals onto one or both of the stars.","Functions Label":6}
{"Functions Text":"The colored rectangles represent the errors of the DEM curve, which are calculated from 100 Monte Carlo (MC) realizations of the observational data","Functions Label":2}
{"Functions Text":"Finally, a number density ratio (rd = n0\/ne) of \u223c0.02 between outside and inside of the flaring loop is determined, which is very close to the density contrast from recent observations","Functions Label":5}
{"Functions Text":"Quasars\u2019 lifetimes are not long ( 0.1 Gyr,","Functions Label":0}
{"Functions Text":"Conventional parametric techniques correct for this effect by dividing the measured flux by a polynomial function of the coordinates of the photometric centroid; some variants may include time-dependence (e.g.,","Functions Label":0}
{"Functions Text":"There is another possibility of the FB formation due to the tidal disruption of stars","Functions Label":0}
{"Functions Text":"and the acceleration of individual particles by the arising shock waves.","Functions Label":0}
{"Functions Text":"At Io, the total neutral volcanic content (SO2, SO, NaCl, KCl, Cl, and dissociation products) ejected to space (Section 4.2.1) by the incident plasma is estimated to be, on average, \u223c1000 kg s\u22121 (e.g.,","Functions Label":0}
{"Functions Text":"Later, numerical algorithms based on Monte Carlo techniques were developed to solve radiative transfer for more general cases. Now theoretical studies mostly rely on them (e.g.,","Functions Label":0}
{"Functions Text":"Allowing for the maximum value of this interval (which would imply a significant foreground galaxy halo), we recover a minimum host contribution of ${\\rm DM}_{\\rm host, min} \\approx 60~\\rm pc~cm^{-3}$. This is consistent with estimates for host galaxy contributions from theoretical and empirical treatments","Functions Label":5}
{"Functions Text":"Since Eggen et al. (1962) showed a model of the MW\u2019s formation process from the kinematic analysis of halo stars in the solar neighborhood, many studies of this Galactic fossil component have been carried out using a large number of newly available halo samples, with their assembly requiring considerable observational efforts over the past decades. These include, for example,","Functions Label":0}
{"Functions Text":"LAMOST","Functions Label":0}
{"Functions Text":"and more.","Functions Label":0}
{"Functions Text":"Above the turnover, the GMC mass function has a power-law form with \u03b2 \u223c 1.9, close to the observed range of \u03b2 \u2208 [1.6, 1.8] for clouds in the Milky Way","Functions Label":1}
{"Functions Text":"The rotational period of RX J1856 is P = 7 s and the X-ray pulsed fraction is the lowest among the XDINSs, \u223c1.3\u2009per\u2009cent","Functions Label":0}
{"Functions Text":"This anticorrelation between stellar mass and \u03bbeff is qualitatively consistent","Functions Label":5}
{"Functions Text":"as well as other observational evidence (e.g.","Functions Label":5}
{"Functions Text":"Moreover, the GR analyses with lensing and internal kinematics of both clusters indicate that the total mass profile is well fitted by the NFW model","Functions Label":5}
{"Functions Text":"We test in Section 2 two available one-dimensional (1D) codes:","Functions Label":2}
{"Functions Text":"and a modified version of the Eulerian, 1D hydrodynamic flash4.0 code with thermonuclear burning","Functions Label":2}
{"Functions Text":"against the \u03c10,7 = 1 case.","Functions Label":2}
{"Functions Text":"We show that with resolutions that are typical for multidimensional full-star simulations, the V1D and the flash results are not satisfactory (up to $50{{\\ \\rm per\\ cent}}$ error in V1D and up to $20{{\\ \\rm per\\ cent}}$ error in flash).","Functions Label":1}
{"Functions Text":"This progress has led to a general consensus about the main physical ingredients required to describe the evolution of the galaxy population (e.g.","Functions Label":0}
{"Functions Text":"In the past, various limits on LIV have been obtained from the spectral time lags of individual GRBs or a large sample of GRBs (e.g.,","Functions Label":0}
{"Functions Text":"Indeed, variability between the yields of different mergers is required to explain observed abundances in metal-poor stars","Functions Label":2}
{"Functions Text":"Measurements from Muller et al. (1980), Danjo et al. (1984), Mueller et al. (1985), and","Functions Label":1}
{"Functions Text":"demonstrated onsets below the ionization threshold.","Functions Label":1}
{"Functions Text":"The rate at which water vapour will be released is da\/dt \u223c 1.5 \u00d7 10\u22123 \u03bcm yr\u22121 (scaled to the distance of the ring, from the result of","Functions Label":2}
{"Functions Text":"), where a is the vertical thickness of the layer.","Functions Label":2}
{"Functions Text":"Due to the complicated physical processes involved in spectral line formation in a 3D atmosphere (e.g.","Functions Label":2}
{"Functions Text":"it is difficult to quantify higher order effects beyond the linear relation between $\\mathfrak {v}$ and W\u03bb; that is, the systematic uncertainty of the linear fitting.","Functions Label":1}
{"Functions Text":"Dense cores, where stars form, are located along or at the intersections of some of these fine substructures (e.g.","Functions Label":0}
{"Functions Text":"Theoretical models explain this inefficiency through a combination of mechanisms that provide support against gravitational collapse, including turbulence, magnetic fields, stellar feedback, and dynamical stabilization","Functions Label":0}
{"Functions Text":"Currently, a limited number of observations","Functions Label":0}
{"Functions Text":"are available to explore the environment dependence of the metallicity","Functions Label":0}
{"Functions Text":"Although most galaxies have an implied SFR that scatters within a factor two around the MS, some do show a significantly higher SFR. Those objects also exhibit a higher gas content, shorter gas depletion times (e.g.,","Functions Label":0}
{"Functions Text":"The predictions are based on experimental data from","Functions Label":2}
{"Functions Text":"for ethylene glycol","Functions Label":2}
{"Functions Text":"It has also been generally believed accordingly that most activity (namely active galactic nuclei\u2014AGNs) of supermassive black holes (BHs) at the centers of galaxies at low redshifts","Functions Label":0}
{"Functions Text":"appear to be fueled by the random accretion of gas via internal, secular processes working close to the BH (say, within a few hundred parsec,","Functions Label":0}
{"Functions Text":"Additionally, glycolaldehyde (C2 H4O2), the simplest form of sugar and one of the first intermediates in the formose reaction","Functions Label":0}
{"Functions Text":", has also been detected in this object for the first time in space in 2012","Functions Label":0}
{"Functions Text":"On the other hand, the super-Chandrasekhar WDs were often explained by incorporating different physics, such as a","Functions Label":0}
{"Functions Text":"presence of charge in the WDs","Functions Label":0}
{"Functions Text":"and the 3D numerical simulations","Functions Label":0}
{"Functions Text":"show that parameters of the differential rotation and convection, e.g. the typical size and turnover time of convective flows, depend on the general stellar parameters, such as mass, age, the spectral class and the rotation rate.","Functions Label":0}
{"Functions Text":"They were discovered as dark silhouettes against the galactic background at 8 and 15 \u03bcm with the Midcourse Space Experiment (MSX,","Functions Label":2}
{"Functions Text":"The comparison sample is compiled from the literature up to z \u223c 3","Functions Label":2}
{"Functions Text":"Such a Comptonisation mechanism accounts for the power-law-like shape of the X-ray primary continuum emission and the high-energy roll-over observed in various nearby AGNs (e.g.","Functions Label":0}
{"Functions Text":"while similar works were performed on INTEGRAL data (e.g.","Functions Label":0}
{"Functions Text":"Physically, it is the rotation that develops a toroidal magnetic field and a poloidal electric field in the lab frame (or the inertial frame), which seems to imply that \u03a6 would not be chosen arbitrarily and would be self-consistently determined by the MHD equations, given the \u03a8 and \u03a9 specified (e.g.,","Functions Label":0}
{"Functions Text":"Based on its SED, MWC 758 has been classified as a pre-transition disk","Functions Label":0}
{"Functions Text":"The distribution of number density, core radius, and concentration parameter remains the same, indicating that the population of clusters in the point source catalog is more compact than the extent-selected sample. The extent-selected sample does not show a clear bias toward cool-core clusters or clusters with a central AGN, but contains the fraction of cool-cores is similar to that of SZ surveys","Functions Label":1}
{"Functions Text":"In this sample, we observe the opposite trend.","Functions Label":6}
{"Functions Text":"and have coupled the code to SN ejecta models","Functions Label":2}
{"Functions Text":"The large mass and solid angle covered by highly concentrated galaxy clusters make them ideal gravitational lenses, which can be used as \u2018cosmic telescopes\u2019 to observe very distant galaxies (e.g.","Functions Label":2}
{"Functions Text":"For example, the well-known density\u2013morphology relation reveals that the ellipticals are preferably found inside the dense groups and clusters, whereas the spirals are intermittently distributed in the fields","Functions Label":0}
{"Functions Text":"More recently, indications of radial anisotropy in the outer regions of DM haloes have been obtained from numerical simulations (e.g.","Functions Label":0}
{"Functions Text":"We have performed the first detailed dissection of the stellar populations of the Milky Way disc in age, [Fe\/H] and $\\mathrm{[ \\alpha \\mathrm{\/Fe]}}$ space, bridging the gap between the detailed observational understanding of MAPs (e.g.","Functions Label":4}
{"Functions Text":"In 2007, it displayed a complex symmetric dimming pattern of up to ~ 3 magnitudes during a 56 day eclipse. This has been attributed to the transit of a substellar companion (called \u201cJ1407 b\u201d) with a mass of 60\u2013100 MJup","Functions Label":0}
{"Functions Text":"Interestingly, the D2 and D3 glide terms for these variants were found to vary by several tens of microarcseconds in the comparison to ICRF2, in line with the level of the systematics observed for those terms. Such findings are not unexpected since Galactic acceleration manifests itself as a dipolar deformation in the source coordinates (e.g.,","Functions Label":5}
{"Functions Text":"Nuclear optical line emission has been reported from spectroscopy","Functions Label":0}
{"Functions Text":"There is some tentative evidences for alignment with respect to the magnetic field","Functions Label":3}
{"Functions Text":"in, e.g., the IRAS 4A system at cm wavelengths","Functions Label":3}
{"Functions Text":"For the case of \u03c1IA = 1.3 (magenta), a decrease of the amplitude of the primary can hardly be observed, as expected for low-amplitude wave","Functions Label":5}
{"Functions Text":"Similar rapid changes in the optical-UV flux are typically seen in other BLS1s, especially those at low Lbol\/LEdd (e.g.","Functions Label":5}
{"Functions Text":"The mechanism by which a nascent millisecond magnetar might power a GRB jet has been studied in detail over the past decade","Functions Label":0}
{"Functions Text":"Other authors observed different systems and likewise saw chro-mospheric excess emissions","Functions Label":0}
{"Functions Text":"In fact, the X-ray continuum in AGNs is well modelled by a power law with a high energy roll-over (e.g.","Functions Label":0}
{"Functions Text":"The fraction of clumpy galaxies was studied from z = 0 up to the most distant galaxies identified today at z ~ 10","Functions Label":0}
{"Functions Text":"Another major coolant of the ISM is [O\u2009i]63\u2009\u03bcm","Functions Label":0}
{"Functions Text":"For V593 Cen, we updated the orbital parameters using more complete light curves. The orbital inclination of 83\u00b0.18 is similar to the result (82\u00b0.6) obtained by","Functions Label":5}
{"Functions Text":"Using the critical intensity advocated by recent studies","Functions Label":1}
{"Functions Text":"this ranges from a few Gpc\u22123 (e.g.","Functions Label":1}
{"Functions Text":"to 10\u22126 to 10\u22124 Mpc\u22123","Functions Label":1}
{"Functions Text":"In addition to these clean-based approaches, recent developments in the field of compressive sensing (CS) applied for astronomical imaging have given birth to many imaging algorithms, particularly for RI","Functions Label":0}
{"Functions Text":"Leveraging optimization frameworks, these methods aim to solve the underlying image recovery problem by enforcing sparsity of the image of interest in some suitable domain.","Functions Label":0}
{"Functions Text":"Unprecedented flux and spectral variability during these episodes have been observed","Functions Label":0}
{"Functions Text":"These IGM transmissions are estimated from Monte Carlo simulations (","Functions Label":2}
{"Functions Text":") which generate 10\u2009000 sightlines for redshifts consistent with the H\u2009i cloud distribution defined analytically by Inoue et al. (2014).","Functions Label":2}
{"Functions Text":"The problem of accretion on to an SMBH has been studied via hydrodynamical simulations (e.g.","Functions Label":0}
{"Functions Text":"Although such fundamental physics is well known, it has not been well studied in SNR shocks. In fact, it is usually assumed that the Ly\u2009\u03b2 photons are at the limits of either completely optically thick or optically thin at SNR shocks, i.e. they are completely converted to H\u2009\u03b1 photons or not at all (e.g.","Functions Label":1}
{"Functions Text":"Similar energy dependent pulse arrival time behavior can also be found in","Functions Label":0}
{"Functions Text":"and XTE J1807\u2013294","Functions Label":0}
{"Functions Text":"with different break point energies.","Functions Label":0}
{"Functions Text":"Prominences are generally believed to be supported by the magnetic tension force of the dips in sheared arcades","Functions Label":0}
{"Functions Text":"For grains consisting of two or three materials, we first derive effective optical constants following the Maxwell Garnett mixing rule","Functions Label":2}
{"Functions Text":"The dynamics of stars can be related to the gravitational potential that they inhabit via the collisionless Boltzmann equation. For systems in a steady state with certain symmetry properties (typically spherical or axisymmetric) it is possible to find solutions to the phase-space distribution of a stellar tracer population, either through distribution function modelling or via the moments of the Boltzmann equation","Functions Label":0}
{"Functions Text":"A good example of this effect is the Virgo cluster, the closest rich galaxy cluster, considered a ram pressure stripping laboratory since a number of clearly ram pressure stripped galaxies have been observed (e.g.,","Functions Label":0}
{"Functions Text":"The HCN(1\u20130)\/HCO+ ratios for M31 GMCs","Functions Label":2}
{"Functions Text":"are indicated by the turquoise shaded region in panels c and d.","Functions Label":2}
{"Functions Text":"Using Bayesian analysis to fit","Functions Label":0}
{"Functions Text":"and a similar distribution function analysis using 5D phase-space data from Gaia","Functions Label":0}
{"Functions Text":"This was done using the complex dielectric function for the sample obtained by heating boehmite at 1173 K from","Functions Label":2}
{"Functions Text":"assuming a spheroid with depolarization parameters of (0.35, 0.035).","Functions Label":2}
{"Functions Text":"While the importance of including GR gravity in simulations of core-collapse supernovae has always persisted in the literature and is in use in many current and state-of-the-art multidimensional, core-collapse supernova calculations","Functions Label":1}
{"Functions Text":"many modern simulations have used a purely Newtonian approximation for gravity","Functions Label":1}
{"Functions Text":"This has been shown using","Functions Label":0}
{"Functions Text":"as well as cosmological simulations","Functions Label":0}
{"Functions Text":"Large numbers of works have extensively studied the binary-disk system in the Newtonian regime with","Functions Label":0}
{"Functions Text":"and hydrodynamical simulations","Functions Label":0}
{"Functions Text":"If we considered the AIA 304 \u212b observations alone, the on-disk condensation, and hence coronal rain events we report here would resemble those occurring in magnetically closed field lines","Functions Label":1}
{"Functions Text":"which are generally interpreted as a manifestation of the heating-condensation cycles due to thermal nonequilibrium","Functions Label":1}
{"Functions Text":"However, combining the observations of SDO and STEREO A and B at different viewing angles, we find that the on-disk coronal rain in this study corresponds to the downflows of condensations facilitated by reconnection between open and closed structures.","Functions Label":1}
{"Functions Text":"More specifically, fast- and slow-mode magnetoacoustic waves in coronal plasma structures are well-known to be subject to a frequency-dependent damping by e.g. resonant absorption and thermal conduction (e.g.","Functions Label":2}
{"Functions Text":"Here we additionally make the assumption that stellar mass comprises 50% of the baryonic content of galaxies by mass at these redshifts, a value broadly consistent with the few measurements made at or near these redshifts (e.g.,","Functions Label":2}
{"Functions Text":"Moreover, the disk formation process has been revealed to be much more complicated for binary and multiple cases, both in observations","Functions Label":0}
{"Functions Text":"In spite of its huge infrared luminosity, the host galaxy is classified from the optical morphology as an ordinary Sa-type galaxy ([R\u2019]SAB[s]a;","Functions Label":1}
{"Functions Text":"Typical values are close to D2 = 1.4\u20131.5","Functions Label":5}
{"Functions Text":"which are consistent with the fractal dimension as derived for the young stellar structures.","Functions Label":5}
{"Functions Text":"In particular,","Functions Label":5}
{"Functions Text":"and Li etal. (2016) both found that the rotation measure predicted from the ADAF is roughly consistent with the observational values.","Functions Label":5}
{"Functions Text":"The majority of past applications of this method constrained the IGM thermal state by fitting the low-b-$N_{\\rm H\\, {\\small I}}$ cutoff of the $b-N_{{{{\\rm H\\, {\\small I}}}}{}}$ distribution","Functions Label":0}
{"Functions Text":"Furthermore, statistical variations in the observed magnetic field direction near the SWTS were included as a time series to model time variations in the injection and DSA of pickup ions to simulate the highly volatile nature of actual DSA at the SWTS","Functions Label":1}
{"Functions Text":"In previous work","Functions Label":1}
{"Functions Text":"we used a custom filter centred on the deep 1.45 \u00b5m feature present in YPMOs to distinguish between them and background sources. In the 2\u20135 \u00b5m range covered by NIX, such water features are far less dominant, and there are strong telluric features across some of this range that would make a similar \u2018water\u2019 technique difficult to use. Instead, we use the differing spectral shape in K-band of very low mass brown dwarfs when compared to earlier spectral type stars.","Functions Label":1}
{"Functions Text":"Clarke et al. (2019) and Buck (2020) suggest that bimodality should be common in disc galaxies, whereas","Functions Label":1}
{"Functions Text":"suggest that it is rare.","Functions Label":1}
{"Functions Text":"RCW 86:","Functions Label":2}
{"Functions Text":"GeV","Functions Label":2}
{"Functions Text":"For our disk model, we are using the power-law profile for the scattering surface height H and the separation r found by","Functions Label":2}
{"Functions Text":"for the disk around HD 97048. This profile describes the flaring discovered in this source reasonably well up to a separation of ~270 au.","Functions Label":2}
{"Functions Text":"These PESs have also been able to account for even subtle effects such as the GP","Functions Label":0}
{"Functions Text":"This is likely to need to be considered for different possible exterior disc models and in addition the planets may have built up their masses as they went (see e.g.","Functions Label":7}
{"Functions Text":"These considerations are beyond the scope of this paper.","Functions Label":7}
{"Functions Text":"However, there is no theoretical argument (or pathology) against GWs propagating faster than light (see","Functions Label":2}
{"Functions Text":"and references therein)","Functions Label":2}
{"Functions Text":"In past years, several alternatives have been proposed to constrain the redshift of BL Lac objects, including","Functions Label":0}
{"Functions Text":"or from the neutral hydrogen in the intergalactic medium (e.g.","Functions Label":0}
{"Functions Text":"While this approach initially appeared to work remarkably well in the case of starburst galaxies","Functions Label":1}
{"Functions Text":"there is now ample evidence that there is no tight universal relation between the UV slope and the","Functions Label":1}
{"Functions Text":"Such an approach, also known as floating chunk offset method (FCO;","Functions Label":2}
{"Functions Text":"has proven extremely reliable even in the presence of complex activity signals, as shown by Malavolta et al. (2018).","Functions Label":1}
{"Functions Text":"The initial condition is the Orszag\u2013Tang vortex (OTV) (e.g.,","Functions Label":2}
{"Functions Text":"In the case of GRBs, approximately 1\/6 of examples are consistent with a galaxy nucleus","Functions Label":1}
{"Functions Text":"showed that the annual Ursid shower was related to comet 8P\/Tuttle, a Jupiter family comet with a period of 13.6yr (JPL-HORIZONS, ssd.jpl.nasa.gov) and a perihelion distance slightly greater than 1au.","Functions Label":0}
{"Functions Text":"High-resolution CO observations are critical for evaluating where high-redshift galaxies fall on the true surface density version of the Schmidt\u2013Kennicutt relation, where \u03a3SFR and \u03a3gas can be compared on a pixel-by-pixel basis within individual galaxies (as done for local galaxies; e.g.,","Functions Label":3}
{"Functions Text":"Studies have shown that heating mainly escapes through the outflow cavity in deeply embedded sources","Functions Label":0}
{"Functions Text":"Secondly, in practice, determining the location of the cutoff is vulnerable to systematic effects, such as contamination from the narrow metal lines","Functions Label":0}
{"Functions Text":"The process of morphological quenching","Functions Label":1}
{"Functions Text":"where the formation of a stellar bulge stabilizes the disk against further star-formation, is also improbable.","Functions Label":1}
{"Functions Text":"The production of elements in the region of Sr, Y, and Zr is more efficient for slightly neutron-rich conditions, corresponding to RLn = 1.35","Functions Label":2}
{"Functions Text":"We observe a very similar behavior and dependency of abundances on the Ye distribution for all exploding models of the 15 M\u2299 progenitor.","Functions Label":5}
{"Functions Text":"Atiras or Interior Earth Objects (IEOs) have aphelion distances 0.983 au and can only be observed at low solar elongations (often 70\u25cb); Vatiras have aphelia 0.718 au, are observed at very low solar elongations (typically 40\u25cb\u201345\u25cb), and just one such object is currently known","Functions Label":0}
{"Functions Text":"The distances of the nebulae from the illuminating star are about 1 pc, assuming that they are located near the plane of the sky occupied by \u03b3 Cas","Functions Label":2}
{"Functions Text":"NLs have high accretion rates (\u223c10\u22128 M\u2299 yr\u22121), so are in a persistent high state, and they gather above the period gap in the period distribution of CVs","Functions Label":0}
{"Functions Text":"In particular, the SPS approach has been applied to observations of various Galactic and extragalactic environments (e.g.,","Functions Label":0}
{"Functions Text":"showing power spectral slopes \u03b2 roughly ranging from \u22122.7 to \u22123.7 depending on the tracers used (e.g., H i, carbon monoxide (CO), and dust).","Functions Label":1}
{"Functions Text":"Since the halo concentration cannot be reliably measured for haloes with fewer than about \u223c400 particles, we use the method presented by Ramakrishnan, Paranjape & Sheth (2021) to assign concentrations cvir (assuming","Functions Label":2}
{"Functions Text":"NFW profiles) conditioned on the mass and local tidal environment of individual haloes.","Functions Label":2}
{"Functions Text":"Finally, the MFD internal shock (IS) model for GRBs also suffers some criticisms, such as","Functions Label":6}
{"Functions Text":"and inconsistency with some empirical (Amati\/Yonetoku) relations","Functions Label":6}
{"Functions Text":"their projected axis is oriented perpendicular to the disk midplane whose inclination with respect to the line-of-sight was estimated to be less than 30\u00b0 (namely, the disk is seen approximately edge-on;","Functions Label":0}
{"Functions Text":"data release as well as calibration vectors for the MaNGA survey","Functions Label":2}
{"Functions Text":"DR14 data release","Functions Label":2}
{"Functions Text":"in Fig. 6.","Functions Label":2}
{"Functions Text":"In the upper panel, we show small-scale features in calibration vectors from the same plate (number 3647) processed by the DR9 (blue), DR12 (green), and DR14 (red) pipelines. The spectra are obtained by normalizing the large-scale features in calibration vectors with a cubic b-spline with break points separated by 50 \u00c5. The three spectra are mostly identical while the smooth curving features at the wavelengths of Balmer series in DR9 disappear in DR12 and DR14. From DR12, the pipeline corrects the features with linear interpolation across wavelength regions with Balmer \u03b2, \u03b3, and \u03b4 lines","Functions Label":1}
{"Functions Text":"One can also observe the change in the median residual spectra of DR9 and DR12 in Fig. 1. However, the H\u03b1 feature remains uncorrected from DR9 to DR14.","Functions Label":1}
{"Functions Text":"Given our very limited knowledge of the ternary C\/O\/Ne phase diagram","Functions Label":6}
{"Functions Text":"this effect cannot be quantitatively implemented in our evolution models.","Functions Label":6}
{"Functions Text":"However, we note that our current understanding of 22Ne phase separation is remarkably consistent with the missing cooling delay.","Functions Label":5}
{"Functions Text":"Interestingly, we found that, four HSPs did not show any IDV","Functions Label":1}
{"Functions Text":"The newest model developed by","Functions Label":0}
{"Functions Text":"is based on similar ideas, but makes use of the optical H\u03b1 surface brightness and a wide set of various calibrators.","Functions Label":0}
{"Functions Text":"It is worthwhile noting that laboratory experiments on the coagulation growth of water-ice particles have a long history outside astronomy and planetary science, since coagulation is observed in daily life and is a plausible route to the formation of snowflakes (e.g.","Functions Label":0}
{"Functions Text":"Indeed, the first molecular searches of PNe turned up negative (e.g.,","Functions Label":0}
{"Functions Text":"Treatment of errors for combining distance moduli across methods or across measurements is suggested by","Functions Label":2}
{"Functions Text":"and Tully et al. (2016) to be based on weighted estimates such as the uncertainty of the weighted mean, albeit with caution partly due to the heterogeneous origin of the compiled data and partly due to Malmquist bias.","Functions Label":2}
{"Functions Text":"Further, the higher contrast of the acoustic features in EE power spectrum compared to astrophysical foregrounds","Functions Label":7}
{"Functions Text":"will ultimately provide independent and tighter constraints on the standard cosmological parameters, such as the scalar spectral index ns, than those from the temperature data alone.","Functions Label":7}
{"Functions Text":"The role of twisted magnetic field in the MHD waves has been studied in many theoretical works (e.g.","Functions Label":0}
{"Functions Text":"However, a hot region with radius 3\u20134 times smaller than R can still produce a pulsed fraction below current limits of 20\u201340 per\u2009cent in the spin period range 0.1\u20130.4 s of known CCOs (see Section 1; for pulsed fraction dependence on spot size, see, e.g.","Functions Label":2}
{"Functions Text":"Indeed, the ultraviolet and X-ray variability detected for many of these LINERs","Functions Label":5}
{"Functions Text":"is in favour of a direct view of the AGNs (i.e. perpendicular to the disc under the UM). This is consistent with the fact that most of the [O\u2009III] morphologies found for LINERs are spheroids, if we assume that the [O\u2009III] traces the NLR.","Functions Label":5}
{"Functions Text":"showed that the main differences between the migration recipes from Jim\u00e9nez & Masset (2017) and Paardekooper et al. (2011) lie in the computation on the corotation torque.","Functions Label":1}
{"Functions Text":"According to this framework, HERGs are powered by accretion of cold gas, provided by e.g., a recent merger with a gas-rich galaxy, while LERGs accrete hot intergalactic gas from dense environments at a low rate","Functions Label":0}
{"Functions Text":"with fuelling from major mergers strongly disfavoured by recent observations (e.g.,","Functions Label":0}
{"Functions Text":"he protoplanetary embryos masses scale as M \u2248 r3(2 \u2212 x)\/2\u03943\/2","Functions Label":2}
{"Functions Text":"where \u0394 is the mutual Hill radii separations between embryos orbits.","Functions Label":2}
{"Functions Text":"The flux ratio \u03d5(\u03b1)\/\u03d5(0) can be derived by using the dust phase function","Functions Label":2}
{"Functions Text":"Several SNe surveys have set strong constraints on cosmological models from the distance\u2013redshift relation (e.g.","Functions Label":0}
{"Functions Text":"However the measured apparent magnitudes, have a residual scatter arising from its intrinsic scatter and effects due to line-of-sight (LOS) structures.","Functions Label":0}
{"Functions Text":"In systems with very large super-Eddington mass-transfer rates, matter presumably piles up around the NS and forms a growing, bloated cloud engulfing a large fraction of the accretion disc. A system will only avoid a CE if it manages to evaporate the bulk of the transferred matter via the liberated accretion energy at a distance from the NS larger than the trapping radius. Otherwise, the incoming material has too much negative binding energy to be ejected. At the same time, this trapping radius must be located inside the Roche lobe of the NS in order to avoid a CE","Functions Label":1}
{"Functions Text":"An LBV star provides an adequate explanation for the transient time-scale, the isolation (e.g.","Functions Label":1}
{"Functions Text":"the lack of a host H\u2009ii region (Fig. 2 and 3; see below, however), and the transient\/main source offset (d \u2248 0.3\u2009kpc, for D \u2243 8\u2009Mpc; Table 1; see below, however).","Functions Label":1}
{"Functions Text":"As a result of the analysis of 3 min oscillations detected in observations from the Atmospheric Imaging Assembly instrument","Functions Label":0}
{"Functions Text":"on-board the Solar Dynamic Observatory (SDO;","Functions Label":0}
{"Functions Text":"These studies all used an invariant quantity (the Reynolds stress or thewave action for rotating or magnetic flows) as a diagnostic tool to interpret the role of the critical level in terms of energy transmission and to quantify exchanges between the wave and the mean flow","Functions Label":0}
{"Functions Text":"Only a few hot corinos have been identified so far either with single dish or interferometric observations:","Functions Label":0}
{"Functions Text":"HH212","Functions Label":0}
{"Functions Text":"Sparse and\/or irregular sampling is a very common issue in SF analysis","Functions Label":3}
{"Functions Text":"Active suppression of these speckles requires measurement of the electric field associated with the speckles directly from a coronagraphic image using a focal plane wavefront sensor (FPWFS). Several FPWFSs have been proposed such as phase diversity","Functions Label":0}
{"Functions Text":"Observations of such \u2018low-luminosity\u2019 ULXs","Functions Label":0}
{"Functions Text":"have revealed changes in the disc emission that may imply the creation of a radiation pressure supported, larger scaleheight flow in the inner regions","Functions Label":0}
{"Functions Text":"or magnetic pressure support","Functions Label":0}
{"Functions Text":"Whether the core collapses or the deflagration disrupts the core depends sensitively on the ignition density","Functions Label":2}
{"Functions Text":"This is consistent with other results (e.g.","Functions Label":5}
{"Functions Text":"which have shown that galaxies having higher current SFR relative to their past averaged SFR are likely to deviate above the IRX\u2013\u03b2 relation, i.e. have larger AFUV(IRX) for a given AFUV(\u03b2).","Functions Label":5}
{"Functions Text":"Despite this qualitative agreement, the Kong et al. mean numerical relation for their UV-selected sample of 50 local starbursts is not a good fit to the FIR-selected SFRS data as shown in Fig. 9.","Functions Label":6}
{"Functions Text":"We excluded stars with saturated photometry","Functions Label":2}
{"Functions Text":"by limiting the magnitudes of the detected VISTA\/VVV sources to 13.8, 12.8, and 12.8, for the J, H, and KS bands, respectively.","Functions Label":2}
{"Functions Text":"While this is an important difference between the two line lists, generally speaking, it is suggested that using very strong lines often introduces complications such as non-LTE effects into a chemical abundance analysis (e.g.,","Functions Label":2}
{"Functions Text":"For example, using Gaia Data Release 2 (DR2)","Functions Label":0}
{"Functions Text":"Kounkel et al. (2018) and Zari et al. (2019) demonstrated that the Orion star-forming region is composed of a variety of populations with different spatial and kinematic properties each that are all likely generated in multiple events instead of in a progressive star formation history (see also","Functions Label":0}
{"Functions Text":"discussing three bursts of star formation in the Orion Nebula cluster).","Functions Label":0}
{"Functions Text":"Many systems have not been taken into account due to several issues. For instance, the system PG1115+080","Functions Label":1}
{"Functions Text":"from the CASTLES survey has been discarded because the lens mass model is steeper than isothermal.","Functions Label":1}
{"Functions Text":"Theoretical predictions are now available","Functions Label":0}
{"Functions Text":"but they have not yet been thoroughly tested against observations, because only very few stripped stars with sufficiently strong wind mass-loss have been identified and studied in detail so far (e.g.,","Functions Label":0}
{"Functions Text":"More generally, a body of work in various domains,","Functions Label":0}
{"Functions Text":"to geophysical fluid dynamics (e.g.","Functions Label":0}
{"Functions Text":"has tried to understand the properties of wave propagation and dissipation around co-rotation and, more generally, at all special locations in fluids that correspond to singularities in the linear wave propagation equation.","Functions Label":0}
{"Functions Text":"Here, we report on Large Binocular Telescope (LBT) observations of an isolated pulsar, PSR\u2009J2043+2740","Functions Label":0}
{"Functions Text":"detected by","Functions Label":0}
{"Functions Text":"and Fermi","Functions Label":0}
{"Functions Text":"The grain-surface network has been further updated to include all studied routes to water formation under interstellar and circumstellar conditions","Functions Label":2}
{"Functions Text":"We estimated the projected spatial wavelength \u03bbproj of the \u201cwiggling\u201d wave according to \u03bb = \u03bbproj\u2215sin i, where i is the angle between the jet symmetry axis and the line of sight, and T = \u03bb\u2215\u03c5, where \u03c5 is the jet velocity, from","Functions Label":2}
{"Functions Text":"State-of-the-art PT has proven successful in predicting the large-scale behaviour of the velocity PDF and the correspondent monopole and quadrupole of the redshift-space correlation function (e.g","Functions Label":0}
{"Functions Text":", at least for massive haloes, M \u223c 1013\u2009M\u2299.","Functions Label":0}
{"Functions Text":"However, the addition of weak bars in low-mass blue galaxies is insufficient to resolve the apparent disagreement between Erwin (2018) and many SDSS-based studies","Functions Label":1}
{"Functions Text":"which instead seems likely to be due to the very different sample selection of the S4G and SDSS galaxy samples.","Functions Label":1}
{"Functions Text":"We recalculated the lifetimes of molecules assuming AV\u2004=\u20043 mag, and with (1) standard dust properties (i.e. with composition and size distribution as of interstellar dust) or (2) with larger and less opaque grains, at the gas-to-dust mass ratio of 124 (see","Functions Label":2}
{"Functions Text":"for more details on the assumed dust properties).","Functions Label":2}
{"Functions Text":"The 10.0\u201370.0 keV flux of the source is found to be (2.26 \u00b1 0.01) \u00d7 10\u22129 erg cm-2s-1, much lower than the value (5.6 \u00b1 0.3) \u00d7 10\u22129 erg cm-2s-1, previously reported from SUZAKU data","Functions Label":6}
{"Functions Text":"To speed them up, we used the Modified Random Walk method implemented in RADMC-3D","Functions Label":2}
{"Functions Text":"For example, there is good evidence","Functions Label":0}
{"Functions Text":"that the local overdensity correlates with the group-centric distance (e.g.,","Functions Label":0}
{"Functions Text":"One should note that during studies of the isolated Abell groups","Functions Label":1}
{"Functions Text":"only a rudimentary alignment was found and related only to the brightest cluster members.","Functions Label":1}
{"Functions Text":"We also manually perform the absolute wavelength calibration using a relatively strong neutral line, O\u202fI 1355.60 \u00c5 (see","Functions Label":2}
{"Functions Text":"The extended star formation history and the broad range of metallicity (\u22121.5 \u2272 [Fe\/H] \u2272 0.2) discovered in the stream fields can be explained by a disk galaxy progenitor","Functions Label":2}
{"Functions Text":"In the case of NGC 7213, the photometric data included in the analysis are:","Functions Label":2}
{"Functions Text":"and the FIR photometry by","Functions Label":2}
{"Functions Text":"However, such a degeneracy can be broken when the inner edge of the disk is very close to the compact object","Functions Label":1}
{"Functions Text":"Asteroid 469219 librates around $\\omega _{\\rm r}=-90{^\\circ }$ for Venus, the Earth, and Jupiter. This behaviour corresponds to domain III in","Functions Label":2}
{"Functions Text":"horseshoe-retrograde satellite orbit transitions and librations (around $\\omega _{\\rm r}=-90{^\\circ }$ or 90\u00b0). For a given cycle, the lower part corresponds to the horseshoe phase and the upper part to the quasi-satellite or retrograde satellite phase.","Functions Label":2}
{"Functions Text":"Indeed, constraints from explosion parameters have shown the majority of CCSNe to be consistent with lower mass progenitors, as opposed to more massive Wolf\u2013Rayet stars","Functions Label":0}
{"Functions Text":"GRBs likely represent a population with rather larger initial masses","Functions Label":0}
{"Functions Text":"It is thought that the early pre-solar nebula was hot (>1500 K), such that both volatiles and refractories (Tsub \u2273 1400 K) are in the gas phase out to larger distances","Functions Label":0}
{"Functions Text":"Such lens model has found widespread astrophysical applications in the literature","Functions Label":0}
{"Functions Text":"In particular, detailed analysis of the radial column density profiles indicates that, at least in the nearby clouds of the Gould Belt, molecular filaments are characterized by a narrow distribution of crest-averaged inner widths with a typical full width at half maximum (FWHM) value Wfil\u200b\u200b\u2004\u223c\u2004\u200b\u200b0.1 pc and a dispersion of less than a factor of \u223c2","Functions Label":0}
{"Functions Text":"The different cosmologies used in the Millenium simulation (in particular, \u03c38 = 0.9; Springel et al. 2005) by Saro et al. (2013) and the simulations by","Functions Label":1}
{"Functions Text":"\u03c38 = 0.8) may also play a role.","Functions Label":1}
{"Functions Text":"To perform the fitting to the data, we adopted the Python package emcee","Functions Label":2}
{"Functions Text":", a pure-Python implementation of Goodman & Weare\u2019s Affine Invariant Markov chain Monte Carlo (MCMC) Ensemble sampler.","Functions Label":2}
{"Functions Text":"SN 2006jd was observed at 1638 days, an epoch very similar to that of SN 2014C, with Spitzer\/IRAC and WISE","Functions Label":2}
{"Functions Text":"In all three cases, the photometry and spectra from 1 to 10 \u03bcm are well fitted by purely carbonaceous dust models, which we overplot in Figure 6 using dust parameters from the literature.","Functions Label":5}
{"Functions Text":"The motion of the photospheric footpoints of the coronal magnetic field may also trigger the forced magnetic reconnection, which may be caused by the explosive solar coronal events (e.g.,","Functions Label":0}
{"Functions Text":"The presence of the substructure has been confirmed by","Functions Label":0}
{"Functions Text":"as well as by more recent SZE measurements","Functions Label":0}
{"Functions Text":"By using these techniques, some studies show a correlation between both 12 + log\u2009(O\/H) and log\u2009(N\/O)","Functions Label":0}
{"Functions Text":"Studies of clusters and groups at $z$ \u223c 0 have evidently shown that outskirts of groups and clusters","Functions Label":3}
{"Functions Text":"and filaments of galaxies","Functions Label":3}
{"Functions Text":"are favourable sites for galaxy transformations.","Functions Label":3}
{"Functions Text":"Still, some correction residuals persist and render the AO PSF shape complex to model. Consequently, standard parametric models that reliably reproduce the seeing-limited PSFs, such as a Moffat function","Functions Label":1}
{"Functions Text":"become inefficient at describing the AO PSF.","Functions Label":1}
{"Functions Text":"One of the methods based on the synergy between UV and WL observations is the Doppler dimming technique","Functions Label":2}
{"Functions Text":"This result is in broad agreement with models of jet launching from ADAFs (e.g.,","Functions Label":5}
{"Functions Text":"which predict the formation of a thin and mildly-relativistic outer layer.","Functions Label":5}
{"Functions Text":"Both clusters host two kinematically distinct populations","Functions Label":0}
{"Functions Text":"More details can be found in our previous papers","Functions Label":0}
{"Functions Text":"A bright X-ray background source such as","Functions Label":0}
{"Functions Text":"or a GRB (e.g.","Functions Label":0}
{"Functions Text":"can be used to detect the WHIM by producing absorption features in its energy spectra","Functions Label":0}
{"Functions Text":"References for the observational data are as follows: RX J0852.0\u22124622:","Functions Label":2}
{"Functions Text":"GeV","Functions Label":2}
{"Functions Text":"With the obtained abundances [C\/Fe] = +2.2 dex and [C\/N] = +1.15, HD 112869 occupies the region of CEMP-s stars on the plots [C\/Fe] versus [Fe\/H] and [C\/N] versus [Fe\/H] (see Figures 5 and 6 in","Functions Label":2}
{"Functions Text":"Another possible effect of the AGN activity on the molecular gas is through outflows. This possibility is supported by observations of individual objects: For example, Carniani et al. (2017),","Functions Label":0}
{"Functions Text":"and Loiacono et al. (2019) find low gas fractions in powerful AGN at cosmic noon hosting high-velocity molecular and ionized outflows","Functions Label":0}
{"Functions Text":"During the transition from the subcritical to the supercritical regime, sources show two different branches in their hardness\u2013intensity diagram (HID) which are known as horizontal branch (HB) and diagonal branch (DB)","Functions Label":0}
{"Functions Text":"This correlation, hereafter referred to as the R\u2013\u03c3v relation, is usually interpreted as the result of turbulent motions in the interstellar medium on all scales","Functions Label":0}
{"Functions Text":"Observation of magnetic fluctuations in the SW indicates that omnidirectional power spectra approach a k\u22121 wavenumber dependence and that low-frequency turbulence exhibits some sunspot cycle variability","Functions Label":0}
{"Functions Text":"For a circular polarized wave, the dispersion relation in the laboratory frame is given by (e.g.,","Functions Label":2}
{"Functions Text":"We measured 164 \u00b1 13 background-subtracted counts between 0.2 and 2.0 keV, as determined using calc_data_sum in Sherpa","Functions Label":2}
{"Functions Text":"The cluster then forms a dense core of high-mass stars and once it starts to collapse, binaries form in the centre. These perturb their neighbours, and we begin to observe massive stars escaping from the mass segregated core","Functions Label":0}
{"Functions Text":"Equation (7) of","Functions Label":2}
{"Functions Text":"then yields Lbol ~ 1.7\u20132.8 L\u2299, depending on whether the NIR flux is neglected (which may be the case) or extrapolated from \u03b3 = \u22122.","Functions Label":2}
{"Functions Text":"They are, however, computationally much more expensive and their complexity makes it more difficult to test underlying modelling assumptions compared to GCMs with simplified thermal forcing. The latter are thus better suited to run simulations for various scenarios, to understand large-scale flow and circulation properties in 3D climate models under different conditions","Functions Label":1}
{"Functions Text":"In addition, recent observational and theoretical studies on RSGs and SNe II indicate that RSG wind mass-loss rates may be independent from metallicity","Functions Label":0}
{"Functions Text":"It is also possible to build embedded void lens models with non-spherically symmetric density profiles given that the lowest-order embedded lens theory is applicable to any distributed lens","Functions Label":0}
{"Functions Text":"The first kind of current-sheet formation is associated with the MHD instabilities (e.g., resistive tearing mode and ideal kink mode) known as spontaneous magnetic reconnection (e.g.,","Functions Label":0}
{"Functions Text":"he SFR reported in Table C.1 refers to a stellar mass range from Mlow = 0.1M\u2299 to Mup = 100M\u2299, is averaged over the past \u0394t = 100 Myr, and was calculated using the standard SFR(LIR) relationship from","Functions Label":2}
{"Functions Text":"here scaled to a Chabrier 2003, IMF) (1)\\begin{equation} \\label{eq:sfr} \\textit{SFR}=10^{-10}\\times L_{\\rm IR}[{L}_{\\sun}]\\, {M}_{\\sun}~{\\rm yr}^{-1}. \\end{equation}SFR=10-10\u00d7LIR[L\u2299]\u2009M\u2299yr-1.","Functions Label":2}
{"Functions Text":"Recent advances in understanding the properties of magnetohydrodynamic (MHD) turbulence","Functions Label":3}
{"Functions Text":"stimulate a renewed investigation on density statistics","Functions Label":3}
{"Functions Text":"which provide important insight into key physical processes such as star formation in the turbulent and magnetized ISM","Functions Label":3}
{"Functions Text":"The surface temperatures of such hydrostatic, strongly inflated models computed with plane parallel grey atmospheres are then compared with the fictitious effective temperatures at \u03c4 = 20 of the atmosphere calculations performed by","Functions Label":2}
{"Functions Text":"Moreover, Draine\u2019s formulation is accounted to determine the lunar surface\u2019s photoelectric efficiency (","Functions Label":2}
{"Functions Text":") \u2013 its spectral dependence can be represented as ${\\chi _{\\nu r}} = {\\chi _o}[1 - ({\\phi _r}\/{E_\\nu })]$.","Functions Label":2}
{"Functions Text":"Since the source emission has been stable for more than 15 years","Functions Label":2}
{"Functions Text":"we performed the joint fit with the longest, burst-free NuSTAR observations (ObsID = 30001025012) and XMM-Newton observations that were performed \u223c11 years earlier.","Functions Label":2}
{"Functions Text":"However, LC\u2009II\/LFIR is not constant, but declines with increasing LFIR, known as the \u2018[C\u2009ii] deficit\u2019","Functions Label":0}
{"Functions Text":"Despite the considerable scatter in both colors and color gradients","Functions Label":1}
{"Functions Text":"the tight correlation between color and stellar mass of the host galaxies holds true in both the region identified as intermediate and outer in Sect. 7.","Functions Label":1}
{"Functions Text":"Including baryon physics introduces some distortions in the scaling relations between the mass and other physical quantities such as temperature, X-ray, or optical luminosity","Functions Label":0}
{"Functions Text":"As happens within Earth\u2019s clouds, exoplanet clouds are likely gravitationally stratified, meaning that smaller, lighter grains become concentrated at the top of the clouds, while larger, heavier grains remain at lower elevation","Functions Label":2}
{"Functions Text":"The source is a known source that appears in many sky survey catalogues, including Gaia, where its G-band magnitude is listed as 14.1 and its inferred temperature is ~5000 K (see","Functions Label":2}
{"Functions Text":"for how the listed temperature we extract from the Gaia catalogue is inferred from the Gaia data).","Functions Label":2}
{"Functions Text":"More complex and fragmented mixing structures are generated in the higher resolution simulation, which indicates that the process producing these structures is not completely resolved at the current resolution (see, e.g.,","Functions Label":2}
{"Functions Text":"These often-called starburst galaxies, with an IR luminosity LIR \u223c (0.1\u20135) \u00d7 1012 L\u2299 (e.g.,","Functions Label":0}
{"Functions Text":"become increasingly more common at high z.","Functions Label":0}
{"Functions Text":"Although spin misalignments may be introduced by natal supernova kicks, episodes of mass transfer and tidal torques serve to realign component spins before the formation of the final black hole binary","Functions Label":1}
{"Functions Text":"However, from spectro-polarimetric observations of a \u03b3-ray emitting NLSy1 galaxy, PKS 2004 \u2212 447","Functions Label":1}
{"Functions Text":"and accretion disc modelling of a sample of 23 radio-detected NLSy1 galaxies","Functions Label":1}
{"Functions Text":"indicate that they have masses similar to the blazar class of AGNs.","Functions Label":1}
{"Functions Text":"The GP effect, while not significant at temperatures relevant to astrophysics, is important below 1 K as illustrated in a series of calculations on H + HD (v, j) collisions for vibrational levels v = 4 \u2212 9","Functions Label":3}
{"Functions Text":"Indriolo & McCall (2012) find a mean \u03b6H of 1.8 \u00d7 10\u221216 s\u22121 in their sample of diffuse molecular sight lines, and values as large as \u223c1 \u00d7 10\u221215 s\u22121 have been reported in the literature","Functions Label":1}
{"Functions Text":"It should be noted that only a handful of studies so far have looked at the correlation between \u03b1 and global galaxy properties:","Functions Label":0}
{"Functions Text":"while","Functions Label":0}
{"Functions Text":"identified H\u202fII regions via Pa\u03b1","Functions Label":0}
{"Functions Text":"However, the stellar number densities required for tidal truncation are high, and in practice few observed regions satisfy this condition","Functions Label":1}
{"Functions Text":"Since long cosmologists have felt motivated to look for alternative explanations for the DE beyond a rigid cosmological constant \u039b. The scalar field paradigm was then profusely used also to make the cosmic vacuum dynamical: \u039b = \u039b(\u03d5). In the old days, the main aim was to adjust the large value of \u039b typically predicted in QFT to be zero. There were many early proposals (see e.g.","Functions Label":0}
{"Functions Text":"Second, while the predicted shadow feature is nearly independent of the spin or orientation of the black hole to within 10%","Functions Label":0}
{"Functions Text":"the emission region surrounding the black hole depends on the details of the underlying accretion process and is intrinsically time variable primarily due to the stochastic nature of magnetorotational-instability-driven turbulence and magnetic reconnection in the accretion flow.","Functions Label":0}
{"Functions Text":"We adopt a different perspective in proceeding from the basic guiding center kinetic equation (e.g.,","Functions Label":2}
{"Functions Text":"instead of the transformed Vlasov equation (Skilling 1975) used by Zank et\u00c2 al. (2014).","Functions Label":1}
{"Functions Text":"It has already been tested with real data collected by the LIGO and Virgo detectors","Functions Label":0}
{"Functions Text":"though the constraints obtained so far with this \u2018statistical\u2019 method are not competitive with the ones derived from GW170817 and its EM counterpart, mainly because of the poor spatial resolution of the current network of ground-based interferometers.","Functions Label":6}
{"Functions Text":"In fact, this concept pre-dates the large-scale use of IFU with works dealing with, for instance, photometric disc\/bulge decompositions of surface brightness profiles (e.g. see","Functions Label":0}
{"Functions Text":"However, resolving individual spots may be imprecise with poor instrumentations, and a new series, based only on sunspot groups, was proposed, called the group sunspot number, GSN","Functions Label":0}
{"Functions Text":"We note that a similar result was found in observations of the Seyfert 1.2 IC\u00c2 4329a and the narrow-line Seyfert 1 SWIFT J2127.4+5654 with NuSTAR","Functions Label":5}
{"Functions Text":"In the recent paper by","Functions Label":5}
{"Functions Text":"the Helios proton data radial gradients of the GCR flux were found to be 6.6 \u00b1 4% above 50 MeV and 2 \u00b1 2.5% between 250 and 700 MeV between 0.4 and 1 AU. These results are in agreement with those from Pamela\/Ulysses (within the statistical and systematic errors).","Functions Label":5}
{"Functions Text":"The collision velocity dependence of the coefficient of restitution between particles was observed in experiments","Functions Label":0}
{"Functions Text":"Assuming a set of stellar population models","Functions Label":2}
{"Functions Text":"to generate spectral energy distributions for galaxies at the emission-line redshift, and fitting them to the available photometry, can give estimates of physical quantities of the galaxies like total stellar mass (the normalization between the observed flux and best-fit model), the star formation rate, metallicity, and the age of the stellar populations, i.e., the galaxy (e.g.,","Functions Label":2}
{"Functions Text":"Generally, during the hopping process, the acceleration first shows a gradual increase, and then decreases rapidly at the end of control torque, during which the reaction force is highly fluctuating due to intermittent transmissions of acoustic energy along force-chain-like networks","Functions Label":0}
{"Functions Text":"as illustrated in Fig 3.","Functions Label":0}
{"Functions Text":"Most recently, Rodriguez-Almeida reported the first unambiguous detection of ethanethiol in the ISM, toward the G+0.603-0.027 molecular cloud","Functions Label":0}
{"Functions Text":"On galactic scales massive molecular winds are common in local Seyfert galaxies (e.g.","Functions Label":0}
{"Functions Text":"Unfortunately, measurements of UV radiation are strongly hampered by the interstellar medium absorption (up to 70%\u201390%), which is significant even for relatively close stars, so that estimates of stellar UV radiation strongly rely on modeling (see","Functions Label":0}
{"Functions Text":", for a recent review).","Functions Label":0}
{"Functions Text":"The standard model of such a turbulent dynamo producing a large-scale magnetic field involves the amplification of seed magnetic fields due to the usual \u03b1 effect, where \u03b1 is a measure of the net kinetic helicity in the flow (see, e.g.,","Functions Label":0}
{"Functions Text":"Our results are consistent with this idea and provide additional evidence for IGM gas feeding into galaxies through streams from the cosmic web (e.g.,","Functions Label":5}
{"Functions Text":"In the literature there are several theoretical works on the evolution of [Ba\/Fe] and [Y\/Fe] in the Galactic thin disc (e.g.","Functions Label":0}
{"Functions Text":"The main and novel aspect of our work is the analysis of the diffuse radio emission resulting from radio haloes in galaxy clusters","Functions Label":4}
{"Functions Text":"In cosmological hydrodynamical simulations, the O vi absorbing gas lies behind the halo accretion shock and is maximal in L* galaxies because their virial temperature is close to the temperature T \u2248 105.5 K where the O+5 ionization fraction peaks","Functions Label":2}
{"Functions Text":"Red novae are recognized as manifestations of on-going mergers of non-compact stars such as main-sequence dwarfs, sub-giants, or red giants","Functions Label":0}
{"Functions Text":"This method and its variants","Functions Label":0}
{"Functions Text":"have been used to estimate the angular power spectrum of the diffused galactic foreground","Functions Label":0}
{"Functions Text":"These works propagate the uncertainties in each visibility estimate and combine that with the sample variance error in measuring the power spectrum to quote uncertainties in the power spectrum estimates.","Functions Label":0}
{"Functions Text":"However, the theoretical works that describe the fundamental properties of the low angular momentum accretion and that usually treat the steady solution of the equations have so far been carried out only for nonmagnetized and usually also nonviscous flows","Functions Label":0}
{"Functions Text":"The spatial density measured with para-H2CO (303\u2013202) and C18O (2\u20131) in N113 and N159W is n(H2) ~ 105 cm\u22123 on a size of ~30\u2033","Functions Label":2}
{"Functions Text":"We perform this emissivity calculation separately for the main sample of spectroscopically confirmed LBGs and LAEs from M13 (using the UV luminosity functions from","Functions Label":2}
{"Functions Text":"for LAEs),","Functions Label":2}
{"Functions Text":"We note that Capak et al. (2011) found that AzTEC3 belongs to a spectroscopically confirmed protocluster containing eight galaxies within a 1 arcmin2 area, and therefore the environment might also play a role in the galaxy size evolution (see also","Functions Label":0}
{"Functions Text":"However, it is currently unclear whether the environmental effects in a galaxy overdensity will lead to a more compact or more extended radio-emitting size than field galaxies.","Functions Label":1}
{"Functions Text":"Among the main proposed formation channels for merging binary COs, we find:","Functions Label":0}
{"Functions Text":"via stable mass transfer (e.g.","Functions Label":0}
{"Functions Text":"The gas-phase chemical network from R\u00f6llig et al. (2007) (mainly based on the UMIST99 ratefile;","Functions Label":2}
{"Functions Text":"allows us to reproduce the C+, CO, and HCO+ abundances in PDRs","Functions Label":2}
{"Functions Text":"so we use this network together with the ionization of the atomic species and corresponding recombinations in the H\u2009ii regions.","Functions Label":2}
{"Functions Text":"Another element of the realistic phenomenological hadronic EoS corresponds to the short-range repulsive interaction of the hard core nature between particles","Functions Label":0}
{"Functions Text":"Although the production of HCOOH has also been investigated experimentally","Functions Label":0}
{"Functions Text":"its formation process and chemical link to nitrogen-bearing species are puzzling.","Functions Label":3}
{"Functions Text":"So far, the biggest efforts were focused into two, somewhat complementary approaches. The first is represented by simulations like","Functions Label":0}
{"Functions Text":"Millennium II (ms-II;","Functions Label":0}
{"Functions Text":"These follow structure formation in a large cosmological volume at the expense of having a medium or a low-mass resolution. Such simulations provide the formation histories for a very large number of medium- and high-mass DM haloes, but do not necessary resolve all the details relevant for galaxy formation.","Functions Label":0}
{"Functions Text":"To accurately describe the shape and internal structure of Jupiter, various interior models with new ingredients, such as two-layer and three-layer structure models, have been established by several groups","Functions Label":0}
{"Functions Text":"A potentially powerful tool that was suggested in the literature is the measurement of deuteration fractions, which may be translated into time-scales via chemical models","Functions Label":0}
{"Functions Text":"Such carbonaceous mantles are efficiently processed by UV photons","Functions Label":0}
{"Functions Text":"but can stay H-rich as long as the radiation field is attenuated","Functions Label":0}
{"Functions Text":"We used shielding functions from","Functions Label":2}
{"Functions Text":"which include effects in lines.","Functions Label":2}
{"Functions Text":"Indeed, the assignment in","Functions Label":6}
{"Functions Text":"was based on only one line of the gGg\u2032 conformer of ethylene glycol about 200 cm-1","Functions Label":6}
{"Functions Text":"above the lowest-energy aGg\u2032 conformer \u2013 and thus tentative.","Functions Label":6}
{"Functions Text":"In this work, we will provide the \u03b6(T, f) function calculated under the assumption of ionization equilibrium using the CHIANTI spectral code","Functions Label":2}
{"Functions Text":"as detailed below. In this framework it is straightforward to users to replace the CHIANTI values for the equilibrium ion fractions by their own values calculated under nonequilibrium conditions, depending on the physical process they model.","Functions Label":2}
{"Functions Text":"Observations have shown that the IRX-\u03b2 relation varies with","Functions Label":0}
{"Functions Text":"age","Functions Label":0}
{"Functions Text":"In addition, several observational studies have suggested that the star formation rate (SFR) of the clouds appears to increase over their lifetimes. For example, studies of young clusters embedded in moderate-mass MCs (\u223c104M\u2299) (e.g.","Functions Label":0}
{"Functions Text":"have shown that their age histograms contain a large majority of young (1\u20132 Myr) objects, but also a tail of older (up to several Myr) ones suggesting an accelerating star formation activity, sometimes followed by a subsequent decline","Functions Label":0}
{"Functions Text":"It is likely that some of these products are also formed in our experiments, but except for CO2, HNCO, and NCO\u2212, they cannot be unequivocally identified with IR spectroscopy alone. Some of them have the same functional groups as urea and their IR spectra present absorptions in the same spectral regions, albeit with different band shapes and intensities. They could contribute somehow to the changes, both in shape and intensity, observed in the absorption bands during processing and thus introduce uncertainty, but by analogy with the literature results just mentioned","Functions Label":1}
{"Functions Text":"we expect that the prevalent dissociation channels will lead to small molecules that will not interfere much with the absorptions of urea.","Functions Label":1}
{"Functions Text":"IRIS observations show that Fe\u202fXXI 1354.08 \u00c5 is a hot (\u223c11 MK) and broad emission line and is always blended with many narrow chromospheric lines at the flaring ribbons","Functions Label":2}
{"Functions Text":"Haloes were identified using rockstar","Functions Label":2}
{"Functions Text":"The most common way to derive galaxy sizes is by performing light-profile fitting assuming a given shape of the surface brightness profile using a \u03c72 minimization","Functions Label":0}
{"Functions Text":"\\label{number5} \\end{eqnarray}k\u03b1=\u03ba\u03b1\/h\u03b1,\u2001k\u03b2=\u03ba\u03b2\/h\u03b2.Equations (2) and (5) give a direct and elegant expression for the perpendicular wave vector as (7)\\begin{eqnarray} \\vec{k}_\\perp \\approx -(\\bdel \\omega_{\\rm c}) t, \\label{number6} \\end{eqnarray}k\u22a5\u2248\u2212(\u2207\u03c9c)t,which is a generalisation to three dimensions of the results of Mann et al. (1995),","Functions Label":2}
{"Functions Text":"and","Functions Label":2}
{"Functions Text":"for lower dimensional systems, which developed phase mixing in only one perpendicular coordinate.","Functions Label":2}
{"Functions Text":"The observed optical light curves are smoother than expected and an insufficient fraction of the X-ray emission hits the disc to power the optical variability (e.g.","Functions Label":1}
{"Functions Text":"Moreover, due to their low density, voids are naturally sensitive to dark energy and thus the interest to use them as probe of alternative Dark Energy models and modified gravity scenarios is increasing","Functions Label":3}
{"Functions Text":"The 16th and 84th percentile of the resulting peak flux density distributions, together with the systematic flux scale density uncertainty of 5%","Functions Label":2}
{"Functions Text":"for the FIRST and LoTSS survey, respectively, are used to determine the error on the spectral index.","Functions Label":2}
{"Functions Text":"Significant progress has been made in recent times through detailed full-quantum scattering calculations, based on quantum chemical data, for the cases of simple atoms such as Li, Na, Mg and Ca","Functions Label":0}
{"Functions Text":"Bound galaxies (subhaloes) were identified within the simulations using the subfind algorithm","Functions Label":2}
{"Functions Text":"in the same manner as in the EAGLE simulations","Functions Label":5}
{"Functions Text":"As a result, recent studies have shifted to using dark-matter halo masses as large as 1011 M\u2299","Functions Label":0}
{"Functions Text":"based on halo abundance matching arguments.","Functions Label":0}
{"Functions Text":"However, the results of","Functions Label":6}
{"Functions Text":"show strong offsets in the kinematics of the gas from the host galaxy (\u2248100\u2009km s\u22121;","Functions Label":6}
{"Functions Text":"whereas the COS-AGN sightlines do not (bottom panel of Fig. 6)","Functions Label":6}
{"Functions Text":"Recently, three unusual TDE candidates have been discovered by Swift, i.e., Swift J164449.3+573451, Swift J2058.4+0516, and Swift J1112.2-8238 (hereafter Sw J1644+57, Sw J2058+05, and Sw J1112-82 for short, respectively), which have very bright nonthermal hard X-ray and radio emissions","Functions Label":3}
{"Functions Text":"In analyses of the resolved star formation properties of nearby disks, a near-unity index for the Schmidt\u2013Kennicutt relation is also found in regimes where the molecular gas dominates the total gas mass surface density (\u03a3gas >9 M\u2299 pc\u22122; e.g.,","Functions Label":5}
{"Functions Text":"As pointed out by","Functions Label":1}
{"Functions Text":"and Abbott et al. (2022), a natural consequence from having a (approximate) Gaussian distribution is a reasonable concordance among the three different error measurements, that is, \u27e8\u03c3\u03b1\u27e9\u223c\u03c368\u2004\u223c\u2004\u03c3std.","Functions Label":1}
{"Functions Text":"Direct observational evidence for AGN feedback on galactic scales in such environments remains sparse. More specifically, while outflows have been observationally detected in a number of instances around AGN in various gas phases, most of these detections have been made in ultra-luminous infrared galaxies or some of the closest quasar\u2013host galaxies","Functions Label":0}
{"Functions Text":"with only a few examples where the AGN have been shown to couple with kpc-scale outflows that are capable of impacting star-formation on galactic scales (for a review","Functions Label":0}
{"Functions Text":"Thus, it is still unclear to what extent the general AGN population could drive kpc-scale galactic outflows capable of possibly limiting or quenching star-formation in the local Universe.","Functions Label":3}
{"Functions Text":"Lupus 3 MMS is a Class 0 protostar with a bolometric luminosity (Lbol) of 0.41 L\u2299 and a bolometric temperature (Tbol) of 39 K in the Lupus 3 cloud at a distance of 200 pc","Functions Label":0}
{"Functions Text":"The parameter m play crucial role in the launching of Blandford\u2013Payne type wind from the accretion disc","Functions Label":0}
{"Functions Text":"While He lines are often removed due to substantial differences between magnetometry results obtained from He versus metallic lines (e.g.","Functions Label":1}
{"Functions Text":"in this case He lines were left in the mask since the majority of the Stokes V line flux comes from these lines, and the Stokes V profiles extracted using a line mask with He lines excluded did not result in detectable Zeeman signatures.","Functions Label":1}
{"Functions Text":"Thanks to large spectroscopic surveys, the search for these chemically peculiar stars is becoming more efficient. Using high spectral resolution surveys, multiple elements, like C, N, O, Na, Mg, and Al, can be measured, depending on the wavelength range and signal-to-noise ratio. Toward this,","Functions Label":0}
{"Functions Text":"and Gaia-ESO survey have led to the discovery of a large group of N-rich field stars","Functions Label":0}
{"Functions Text":"The residence time can be calculated as the time it takes to deflect the accelerated electron by an angle ~1\/\u0393sh","Functions Label":2}
{"Functions Text":"In addition, there is evidence demonstrating that bars can enhance star formation in the central regions of galaxies (e.g.","Functions Label":0}
{"Functions Text":"This connection between radio emission and star formation is strongly supported by the close infrared (IR)-radio correlation observed in galaxies (e.g.","Functions Label":0}
{"Functions Text":"We use the quadratic limb-darkening coefficients reported by","Functions Label":2}
{"Functions Text":"to establish the stellar center-to-limb intensity profile,","Functions Label":2}
{"Functions Text":"However, to date only the FIRE collaboration has implemented the two moment method (capable of dealing with CR streaming) in such simulations, and \u2013 in contrast to, for instance, van de Voort et al. (2021) \u2013 the plasma \u03b2 in their winds is too high for the acoustic instability to develop","Functions Label":1}
{"Functions Text":"Ohmic dissipation operates in high-density regions with weak field, AD dominates in highly ionized and low-density regions, and the Hall effect lies in between","Functions Label":0}
{"Functions Text":"The spectral properties of LAEs are usually interpreted as coming from young (\u227250 Myr) and low-mass (M*\u200b\u2004 \u2004\u200b1010\u2006M\u2299) galaxies","Functions Label":0}
{"Functions Text":"which are actively star forming (SFR\u200b\u2004\u223c\u2004\u200b1\u2005\u2212\u2005100\u2006M\u2299\u2006yr\u22121) and dust poor (dust attenuation AV\u200b\u2004 \u2004\u200b0.2, see e.g.","Functions Label":0}
{"Functions Text":"Using deep LOFAR 150 MHz observations in the 7 deg2 Bo\u00f6tes field","Functions Label":0}
{"Functions Text":"studied the FIRC at 150 MHz from z\u2004\u223c\u20040.05 out to z\u2004\u223c\u20042.5. They found fairly mild redshift evolution in the logarithmic IR to radio luminosity ratio in the form of qIR\u2004\u223c\u2004(1\u2005+\u2005z)\u22120.22\u2005\u00b1\u20050.05.","Functions Label":0}
{"Functions Text":"However, if the FIRC is non-linear (i.e. the logarithmic slope is different from one), then it implies that the qIR parameter would depend on luminosity.","Functions Label":1}
{"Functions Text":"The interplanetary manifestations of CMEs","Functions Label":0}
{"Functions Text":"can be measured by a spacecraft at about 1 AU and exhibit the following characteristics:","Functions Label":0}
{"Functions Text":"counterstreaming suprathermal electron (CSE) strahls and declining speed","Functions Label":0}
{"Functions Text":"In particular, if the field line angular velocity is set much less than the horizon angular velocity by distant plasma and a very tenuous plasma exists in the event horizon magnetosphere, then radiation resistance will determine the flow dynamics of accretion as well as the rotational energy extraction by a putative jet","Functions Label":0}
{"Functions Text":"Therefore, here, we first consider whether Eddington-limited accretion in such a neutron star LMXB might explain the observed radio behaviour in Sw J1858. The neutron star LMXBs with the highest mass accretion rates are the Z-sources, which are thought to accrete near or at the Eddington luminosity, tracing out Z-shaped tracks in their X-ray colour\u2013colour diagrams","Functions Label":2}
{"Functions Text":"Also, in this scenario, Sw J1858 should not have resided in the much more radio bright Horizontal Branch during any of the observations, which is unlikely given the time-scales and commonness of transitions between the branches","Functions Label":1}
{"Functions Text":"A possible explanation for these low braking indices may be through the emission of a relativistic particle wind","Functions Label":0}
{"Functions Text":"For example, Sirko et al. (2004), Kafle et al. (2012),","Functions Label":0}
{"Functions Text":"Kafle et al. (2014) and King et al. (2015) fit an ellipsoidal distribution of velocities","Functions Label":0}
{"Functions Text":"Taking into account all these effects, the HPR of the overall RASS PSF is 84\u2033","Functions Label":0}
{"Functions Text":"However, this method leads to systematic errors as creation of 1D light profile by either averaging over the galaxy image or by taking a single cut along the major axis do not properly take into account non-axisymmetric features like a bar or isophotal twist (for more details see","Functions Label":0}
{"Functions Text":"As of today, many more mass ejection channels have been discussed:","Functions Label":0}
{"Functions Text":"and by viscous effects","Functions Label":0}
{"Functions Text":"The course of the outburst was monitored in","Functions Label":0}
{"Functions Text":"sub-millimeter","Functions Label":0}
{"Functions Text":"It has been demonstrated that the statistical predictions of the \u2018bubble model\u2019 and the 21cmFAST agree fairly well with radiative\u2013hydrodynamic simulations","Functions Label":5}
{"Functions Text":"at least when recombination, feedback, etc. are ignored.","Functions Label":1}
{"Functions Text":"Because of their scale height","Functions Label":2}
{"Functions Text":"these two sequences are associated with the thick disc (high-alpha) and thin disc (low-alpha), respectively.","Functions Label":2}
{"Functions Text":"This is in agreement with the finding that the thick disc has a shorter scale length than the thin disc","Functions Label":5}
{"Functions Text":"In the case of collimated relativistic jets, magnetic fields must play an important role","Functions Label":3}
{"Functions Text":"A periodogram of these RVs showed a clear signal at 35.57 days, but the TESS photometry and the RHK index","Functions Label":6}
{"Functions Text":"indicate a stellar rotation period of around 35 days, calling for caution.","Functions Label":6}
{"Functions Text":"The accretion rate then reaches the standard value predicted for MYSOs of $10^{-3}\\, \\rm M_{\\odot }\\, \\rm yr^{-1}$","Functions Label":1}
{"Functions Text":"up to the onset of the disc formation happening at ${\\approx } 12\\, \\rm kyr$.","Functions Label":1}
{"Functions Text":"Since the planet is synchronized within a timescale of a few thousand years, the stellar tide drives the secular orbital evolution","Functions Label":0}
{"Functions Text":"This method required","Functions Label":2}
{"Functions Text":"to assume an effective medium theory, such that a pellet is a mixture of one of their samples with a matrix of air.","Functions Label":2}
{"Functions Text":"The slow rising afterglow light curves also rejected a uniform top-hat jet","Functions Label":1}
{"Functions Text":"We have not included in our models the effects of \u2018kicks\u2019 caused by asymmetric emission of gravitational waves, which have been proposed to be possibly responsible for ejecting BHs from haloes with shallow potential wells, thus halting or reducing the growth of high-redshift BHs hosted in small haloes (e.g.","Functions Label":6}
{"Functions Text":"This effect, however, seems to affect less than 10 per cent of binaries","Functions Label":1}
{"Functions Text":"Whether or not any theoretical mechanism presently exists to explain the formation of giant planets in binary systems, the fact remains that at least a few binary systems, such as \u03b3 Cephei","Functions Label":2}
{"Functions Text":"do harbor planets. Therefore, some formation mechanism does in fact exist.","Functions Label":2}
{"Functions Text":"Owing to its proximity","Functions Label":0}
{"Functions Text":"and nearly edge-on orientation, the Bar provides an ideal laboratory for testing PDR models","Functions Label":0}
{"Functions Text":"and a primary target for observational studies of physical and chemical structures of PDRs (e.g.,","Functions Label":0}
{"Functions Text":"At high nb the density profile inside the WS cell extends towards the edge of the cell, pointing out that the WS approximation may be close to its limits of validity","Functions Label":0}
{"Functions Text":"Moreover, higher SFRs could be induced by an increased efficiency of star formation due to the enhanced fragmentation in gas-rich, turbulent, and gravitationally unstable high-redshift disks","Functions Label":0}
{"Functions Text":"Regarding its distance, there are currently two different methodologies based on parallaxes from Hipparcos","Functions Label":0}
{"Functions Text":"and isochrone fitting, respectively.","Functions Label":0}
{"Functions Text":"Traditionally, bulges were thought to invariably form early-on via","Functions Label":0}
{"Functions Text":"or mergers","Functions Label":0}
{"Functions Text":"with the disk gradually building up around them.","Functions Label":0}
{"Functions Text":"Whereas this inside-out galaxy formation scenario appears consistent with important integral characteristics of CBs (e.g., their red colors), it does not offer a plausible explanation for the presence of PBs in present-day LTGs.","Functions Label":1}
{"Functions Text":"No fits of these sizedistributions are available, but the figures in","Functions Label":2}
{"Functions Text":"and Price et al. (2010) indicate that the differential sizes may follow a log-normal distribution.","Functions Label":2}
{"Functions Text":"These stellar absorption lines are intrinsically weak in star-forming galaxies, with EW0 typically well bellow 1 \u00c5 (e.g.","Functions Label":0}
{"Functions Text":"The general morphologies and the locations of the high-twist fields are also in agreement with many previous studies","Functions Label":5}
{"Functions Text":"Second,","Functions Label":1}
{"Functions Text":"discovered that the distributions of X-ray photon spectral indices between RLAGNs and their radio-quiet counterpart are very similar","Functions Label":1}
{"Functions Text":"The location of the star (Teff \u2243 45 000 K, log\u2009g \u2243 4.5;","Functions Label":5}
{"Functions Text":"is consistent with a current mass of M\u223c0.55 M\u2299 which implies an initial mass in the main sequence of \u223c1 M\u2299.","Functions Label":5}
{"Functions Text":"By taking into account the results of the initial qualitative classification by Le F\u00e8vre et al. (2020) and of the more recent quantitative analysis of a subsample of the ALPINE targets by","Functions Label":4}
{"Functions Text":"we proceed with a more in-depth characterization of the [CII]-detected galaxies aimed at obtaining a robust merger fraction at z\u2004\u223c\u20045.","Functions Label":4}
{"Functions Text":"Because they are detected in a wide variety of interstellar sources","Functions Label":0}
{"Functions Text":"and even in comets","Functions Label":3}
{"Functions Text":"it is of prime importance to understand well how these precursor molecules form.","Functions Label":3}
{"Functions Text":"However, it is worth noting that since GRB relativistic blast waves generate synchrotron radiation as they expand into the circumstellar (wind generated) medium","Functions Label":2}
{"Functions Text":"we expect the forward-shock of the afterglow to peak more brightly at 15.7\u2009GHz and at earlier times than the peaks recorded by Chandra & Frail (2012).","Functions Label":1}
{"Functions Text":"We therefore require a higher monitoring cadence at early times (within 5\u2009d post-burst) to detect similar radio peaks.","Functions Label":2}
{"Functions Text":"The high-twist region in our result is also in agreement with","Functions Label":5}
{"Functions Text":"the location of the flare ribbons","Functions Label":5}
{"Functions Text":"The flexibility in ESPRESSO\u2019s operations has been tackled by adopting a new DFS deployment plan described in","Functions Label":0}
{"Functions Text":"that is exceptional under various aspects because it has to cope with various telescope and instrument configurations while remaining operationally simple.","Functions Label":0}
{"Functions Text":"Many studies (e.g.","Functions Label":2}
{"Functions Text":"have shown that the macro model cannot explain the flux ratios in this lens, which suggested the presence of microlensing or dark matter substructures. Thus, to avoid possible biases caused by flux ratios, we only use the lensed quasar positions and the extended arc to constrain the mass model, which is also the standard procedure for H0 measurements in TDCOSMO Collaboration. Ignoring the fluxes of the lensed quasar images will not affect the constraining power of the imaging data, since the lensed arc emission is much more constraining than the lensed quasar fluxes.","Functions Label":2}
{"Functions Text":"The mechanism of gamma-ray emission may be predominantly due to hadronic processes, where relativistic protons interact with gas and subsequently produce gamma rays through neutral pion decay","Functions Label":0}
{"Functions Text":"The initial mass function of first stars is thought to be more or less top-heavy","Functions Label":0}
{"Functions Text":"Theoretical considerations and simulations of MHD turbulence in the presence of a significant background\/guide magnetic field suggest that solar wind turbulence can to lowest order be modeled in terms of a combination of a dominant quasi-2D turbulence component of coherent structures (small-scale magnetic islands) perpendicular to the background\/guide field and a minor parallel-propagating Alfv\u00e9n wave turbulence component","Functions Label":0}
{"Functions Text":"a view that is consistent with analysis of solar wind observations","Functions Label":5}
{"Functions Text":"and with the finding that quasi-2D turbulence alone is not sufficient to explain observed solar wind turbulence","Functions Label":5}
{"Functions Text":"Due to different emission zone locations, standard pulsar radiation models include the","Functions Label":0}
{"Functions Text":"the slot-gap (SG) (e.g.,","Functions Label":0}
{"Functions Text":"models.","Functions Label":0}
{"Functions Text":"By averaging over 222 976 supergranular cells and applying time-distant helioseismic inversions,","Functions Label":1}
{"Functions Text":"found a symmetrical flow in supergranules, which is directed radially away from the centre of the cells to its periphery, with horizontal velocities in the range of 0.3\u20130.6 km s\u22121. Their velocity profile is found to increase with increasing distances to the supergranule centre up to a maximum value from where on a continuous decrease for larger distances starts.","Functions Label":1}
{"Functions Text":"Scudder & Olbert (1979) also predict that the halo Ebp\/kBTc ratio remains constant with heliocentric distance, whereas","Functions Label":6}
{"Functions Text":"find that the halo Ebp\/kBTc ratio decreases with heliocentric distance.","Functions Label":6}
{"Functions Text":"This is crucial since, although space weather forecasting often focuses on estimating the onset and intensity of geomagnetic storms","Functions Label":0}
{"Functions Text":"Previous works in the literature have shown an increase of [C\/O] ratios as [O\/H] increases (e.g.","Functions Label":1}
{"Functions Text":"but our ratios present a quite large dispersion that together with the shorter range in [O\/H] prevents us from seeing a clear behaviour.","Functions Label":1}
{"Functions Text":"Additional followup observations in the optical, near-IR, submm and other wavelengths were targeted at the lensed z = 3.26 source and the foreground objects responsible for the lensing, resulting in detailed analyses of this lensing system by","Functions Label":0}
{"Functions Text":"and Bussmann et al. (2013).","Functions Label":0}
{"Functions Text":"Theoretical models explain this inefficiency through a combination of mechanisms that provide support against gravitational collapse, including turbulence, magnetic fields, stellar feedback, and dynamical stabilization","Functions Label":0}
{"Functions Text":"In Figure\u00c2 2, we compare our determination of the stellar surface density fraction to a simple theoretical model and to the best fit of a sample of lens galaxies by","Functions Label":2}
{"Functions Text":"Other proposed solutions include those","Functions Label":0}
{"Functions Text":"or through dynamical feedback driven by starbursts or active galactic nuclei (AGNs;","Functions Label":0}
{"Functions Text":"The linear separation of the V and 37 GHz emission region can be estimated using the relation","Functions Label":2}
{"Functions Text":"Secondly, the chemical abundance of SF galaxies at z \u223c 2 is lower by 0.1\u20130.3\u2009dex for a given stellar mass compared to those at low-z","Functions Label":0}
{"Functions Text":"When also considering the central band in rare cases it is plausible to witness multiple-peaked or otherwise complex spectral line profiles (e.g. see the discussions by","Functions Label":0}
{"Functions Text":"This also stresses the need for systemic tracers beyond \u2009Ly\u03b1 to distinguish IGM signatures and pinpoint the origins of various spectral features.","Functions Label":3}
{"Functions Text":"More recently, unified EoSs for NS have been derived by the Brussels-Montreal group","Functions Label":0}
{"Functions Text":"has also mentioned the well known problem of the \u201canomalous ions\u201d, that is, the observed high intensities of the Li- and Na-like (as Si\u2009iv) ions","Functions Label":0}
{"Functions Text":"Additional searches in the infrared (IR) regime have yielded a few more candidates (e.g.","Functions Label":0}
{"Functions Text":"Several studies show that one can distinguish at least classes of channels, such as isolated binaries and dynamically induced mergers,","Functions Label":0}
{"Functions Text":"as well as the orbital eccentricity at some reference GW frequency","Functions Label":0}
{"Functions Text":"In the sub-Keplerian flow, shocks are formed when the Rankine\u2013Hugoniot conditions are satisfied","Functions Label":0}
{"Functions Text":"This is the most intense emission detected so far from a Galactic GC, again suggesting the presence of a large number of MSPs. However, no direct radio detection of these objects has been obtained so far in this system","Functions Label":3}
{"Functions Text":"Unlike common chemical peculiarities seen in Am and Ap stars, \u03bb Bo\u00f6tis stars are not constrained to slow rotation","Functions Label":1}
{"Functions Text":"Since the PG108.3 cloud consists of three evolved H ii regions, one can thus speculate that the formation of young sources in the region might have been triggered by the expanding bubble. However, our observations largely do not favor such a process because in such a scenario one would expect the distribution of young YSOs or star-forming cores at the outskirts of the H ii regions (see, e.g.,","Functions Label":1}
{"Functions Text":"In contrast, we find that no young Class I sources around S147 and most of Class I sources around S148 are cospatial with the Class II sources located near the center of the ionized gas.","Functions Label":1}
{"Functions Text":"In addition, some models","Functions Label":0}
{"Functions Text":"exhibit low-frequency GW emission due to the standing accretion shock instability (SASI","Functions Label":0}
{"Functions Text":"This condition corresponds for CG X-1 to the requirement MBH \u2273 1.5\u2009vw,\u200910004\u03b42 M\u2299, where MBH is the BH mass, vw,\u20091000 is the wind velocity in units of 1000\u2009km\u2009s\u22121, and \u03b4 \u2248 1 is a dimensionless parameter","Functions Label":2}
{"Functions Text":"see also","Functions Label":2}
{"Functions Text":"In some cases, twisted magnetic flux tubes appear close enough to flow vortices, leading to magnetic and kinetic vortex structures closely coexisting in regions with high plasma-\u03b2","Functions Label":0}
{"Functions Text":"Hence, if we assume that FRBs produced by magnetars are created in the magnetosphere close to the polar cap, we can expect them to be significantly beamed","Functions Label":1}
{"Functions Text":"The recent discovery of peculiar highly overluminous SNeIa,","Functions Label":0}
{"Functions Text":"indicates a huge Ni-mass and confirms the highly super-Chandrasekhar white dwarfs, having mass 2.1\u20132.8\u2009M\u2299, as a suitable progenitors","Functions Label":0}
{"Functions Text":"Predicting the amplitude of a solar cycle can be done using solar polar magnetic fields from the previous cycle as \u201cprecursors\u201d of the next cycle","Functions Label":0}
{"Functions Text":"Although the chemical retrievals follow different strategies (equilibriumversus free-chemistry), both indicate that a depletion of TiO relative to VO is needed to explain the observed emission spectrum, supporting the earlier findings by","Functions Label":5}
{"Functions Text":"Further support for this interpretation was provided by the findings of stronger impact of large-scale tides on the galaxy spin orientation in denser filaments","Functions Label":5}
{"Functions Text":"using filament density as a proxy for the thickness of filaments","Functions Label":0}
{"Functions Text":"Furthermore, the more clearly an event is identified as a starting track, the more probable it is to be an astrophysical rather than atmospheric background. Down-going atmospheric neutrino events at high energy are likely to be accompanied by muons produced in the same cosmic-ray shower that triggers the veto and reduces the atmospheric neutrino background","Functions Label":0}
{"Functions Text":"However, if this fraction is very low, as required if GW170817 leaves behind a black hole","Functions Label":1}
{"Functions Text":"the fast magnetar model may fail to explain the small fraction of LGRB\/SLSN-like hosts in FRB samples.","Functions Label":1}
{"Functions Text":"The general morphologies and the locations of the high-twist fields are also in agreement with many previous studies","Functions Label":5}
{"Functions Text":"Later versions of the model used a more moderately top-heavy IMF in starbursts, triggered by disc instabilities rather than mergers, and found similarly good agreement with the number counts","Functions Label":0}
{"Functions Text":"In particular, we have also used the ML1 (\u03b1 = 1,a = 1 \/ 8,b = 1 \/ 2,c = 24,","Functions Label":2}
{"Functions Text":"We used the","Functions Label":2}
{"Functions Text":"tracks, as recommended by Bruzual & Charlot (2003)","Functions Label":2}
{"Functions Text":"propose a scenario where it is the high temperature that is responsible for the HCN enhancement, whereby neutral-neutral reactions with high reaction barriers are enhanced","Functions Label":0}
{"Functions Text":"thus leading to the possible enhancement of HCN and the depletion of HCO+ via newly available formation and destruction paths, respectively.","Functions Label":0}
{"Functions Text":"However, while of course higher gas temperatures are expected in AGN-dominated regions, these are not unique to these environments, as starburst regions and\/or regions where outflows dominate can also harbour high enough temperatures for such enhancement to occur. Additionally, the higher temperatures could increase HCN excitation, relative to HCO+ and CS, without necessarily changing their relative abundances","Functions Label":3}
{"Functions Text":"Finally, infrared radiative pumping is also a possible explanation of the HCN intensity enhancement relative to HCO+ and CS. Infrared pumping is a result of the emission of 14 \u03bcm infrared photons due to the presence of hot dust around AGN. These photons vibrationally excite HCN to the \u03bd2\u2004=\u20041 state. Upon de-exciting from this state back to the vibrational ground state, \u03bd\u2004=\u20040, the HCN line intensities are thus pumped to higher fluxes","Functions Label":3}
{"Functions Text":"However, we note that it is also not unlikely that the 12 \u03bcm infrared photons can similarly vibrationally excite HCO+, thus nullifying the extent of this effect","Functions Label":3}
{"Functions Text":"Using this method, surveys of star-forming regions with (sub)mm facilities such as SMA and ALMA have determined that protoplanetary disks have typical masses of 0.1%\u20130.5% of that of their host star (e.g.,","Functions Label":0}
{"Functions Text":"Alternatively, mass transfer rate-related events such as X-ray state changes and disc instability can also cause long-term modulations","Functions Label":1}
{"Functions Text":"Our target locations are not on a major maria and near sites repeatedly observed in previous Earthshine photometry because they were expected to have roughly comparable albedos","Functions Label":3}
{"Functions Text":"The WD companions to Be stars proved unexpectedly elusive","Functions Label":0}
{"Functions Text":"suggest that a baryon-poor outflow can explain the high-energy afterglow emission of GRB 200415A, while a baryon-rich outflow is also viable if the dissipation happens below the photosphere via internal shocks. Therefore, in this paper, we calculate two situations that the ejecta is dominated by electron\u2013positron pairs or protons, respectively.","Functions Label":3}
{"Functions Text":"The density can be expressed in number density of hydrogen atoms (mH = 1.6727 \u00d7 10-27\u2009kg), which follows roughly (2)\\begin{equation} \\label{density} n_{\\rm H} = 2.0 \\; {\\rm e}^{-\\frac{|z|}{100\\,{\\rm pc}}}, \\end{equation}nH=2.0e\u2212|z|100\u2009pc,where z is the galactic height","Functions Label":2}
{"Functions Text":"and nH is given in atoms per cm3.","Functions Label":2}
{"Functions Text":"However, as all results show that EII product ion fractions decrease as the complexity of the molecules increases","Functions Label":3}
{"Functions Text":"The analysis, described in detail in Field et al. (2013), is remarkably successful in describing important characteristics of spontelectrics, such as the deposition temperature dependence of the surface polarization charge, including the counterintuitive behavior of solid methyl formate","Functions Label":1}
{"Functions Text":"The disk-wind model suggests that the BLR gas comes from winds produced by the accretion disk","Functions Label":0}
{"Functions Text":"Pioneering work with integral field unit (IFU) observations of four GPs","Functions Label":0}
{"Functions Text":"reveals that two are rotationally supported, with seemingly undisturbed morphology, and two are dispersion-dominated, leading the authors to conclude that mergers may not be a necessary driver of their star formation properties, and by extension, for their LyC emission.","Functions Label":0}
{"Functions Text":"This region exhibits a steeper density gradient in its outer envelope, with qout \u2243 \u22122.5, also illustrated by the cloud structure studied with probability density function","Functions Label":5}
{"Functions Text":"Interesting enough, these two portions of the stream are separated by a very narrow region across which Alfv\u00e9nicity changes abruptly, from high to low","Functions Label":0}
{"Functions Text":"During the occurrence of X-class flares, the complex AR had shown \u03b4-sunspots, which are identified with a complex distribution of sunspot groups in which the umbrae of positive and negative polarities share a common penumbra","Functions Label":0}
{"Functions Text":"This scenario is strengthened by the recent observations of warm Neptunes at the border of the desert, on the verge of","Functions Label":5}
{"Functions Text":"considerable mass-loss.","Functions Label":5}
{"Functions Text":"Instead we believe it to trace the metal-poor gas that acts as a replenishment mechanism of galaxies throughout the universe. It has indeed been suggested that GRB hosts in general are fuelled by recent metal-poor gas inflow","Functions Label":1}
{"Functions Text":"The general dynamics of this process have been studied extensively in purely hydrodynamical simulations","Functions Label":0}
{"Functions Text":"For a warped disc, the binary separation and the mass ratio suggest that M81 X-6 lies in the intermediate instability zone for radiation-driven warping in X-ray binaries (see fig. 1 of","Functions Label":1}
{"Functions Text":"Furthermore, the hard radiation fields in star-forming dwarf galaxies, along with their lower dust abundance, result in extended ionized gas regions prominent on global galaxy scales","Functions Label":1}
{"Functions Text":"In some cases, double relics have been detected on opposite sides of the cluster centre (e.g.,","Functions Label":0}
{"Functions Text":"In these clusters it is possible to constrain the merger history, providing important information about the formation processes of relics.","Functions Label":0}
{"Functions Text":"The mass accretion and loss rates for Class 0\/I low-mass protostars span the range of 10\u22126\u201310\u22128 M\u2299 yr\u22121, and the derived jet efficiencies (ratio between mass ejection and accretion rates) range between \u223c1 per\u2009cent and 10 per\u2009cent (e.g.","Functions Label":0}
{"Functions Text":"On the other hand, FRB 20180916B has a nominal RM and has shown a gradual variation in RM value over the two year timescale","Functions Label":6}
{"Functions Text":"Modified Two Stream Instability (MTSI) due to relative drift between reflected ions and incoming solar wind electrons (fast drift), and incoming solar wind ions and electrons (slow drift) has been frequently considered","Functions Label":1}
{"Functions Text":"At low energies they assumed the ENA energy spectra provided by Fuselier et al. (2012). They derived a total pressure of 2.5 pdyn cm\u22122 in all three plasma regions in the nose of the heliotail","Functions Label":1}
{"Functions Text":"Pressure contributions from the slowed solar wind, magnetic pressure, and the pressure exerted from pickup ions and anomalous cosmic rays all had to be taken into account to obtain this total pressure.","Functions Label":1}
{"Functions Text":"However, it is tempting to speculate that environmental effects from such a rich field could be playing a role in the production of this wind nebula (e.g., triggering of pair cascade by external gamma rays from a nearby source","Functions Label":3}
{"Functions Text":"It is unquestionable that such a unique sample of Cepheids \u2013 likely all members of the cluster and at the same distance, chemical composition and age \u2013 would constitute a milestone in our understanding of the Cepheid pulsational scenario. Indeed, it offers an unprecedented opportunity to investigate both empirical and theoretical estimates of the luminosity and colour of the pulsating structures and their relation with the observed periods. For this reason, many authors have studied the NGC 1866 Cepheids","Functions Label":3}
{"Functions Text":"in both the optical and near-infrared bands, and have tested different methods to calibrate the PL relations in different filters.","Functions Label":3}
{"Functions Text":"The abundance of real-world applications of ANNs is largely a consequence of two properties: (i) an ANN is capable of closely approximating any continuous function that describes the relationship between an outcome and a set of covariates, known as the universal approximation theorem","Functions Label":0}
{"Functions Text":"Mechanisms suggested to produce these small-scale magnetic helicity fluxes are: advection of magnetic fields by an outflow from the disk through the galactic fountain or wind","Functions Label":0}
{"Functions Text":"Similar results are obtained in studies of individual galaxies at z\u2004\u223c\u20046\u20138","Functions Label":5}
{"Functions Text":"However, given the low angular resolution of these data, they can not rule out the possibility that one or more merging [C\u202fII]-bright satellites are mimicking the smooth gradient observed in the velocity maps","Functions Label":1}
{"Functions Text":"Massive YSO outflows mapped in high-velocity CO lines have collimation factors R = length\/width \u223c2.05 \u00b1 0.96 as compared to R \u223c 2.81 \u00b1 2.16 for low-mass stars","Functions Label":1}
{"Functions Text":"indicating a weak tendency that outflows associated with massive stars are less collimated than those from low-mass stars as previously thought","Functions Label":1}
{"Functions Text":"The combined detector and telescope PSFs are described in detail in","Functions Label":0}
{"Functions Text":"In addition,","Functions Label":1}
{"Functions Text":"and the snow line is located at a greater distance from the central star","Functions Label":1}
{"Functions Text":"As a consequence, these planets are most likely formed at greater orbital distances and, due to the shorter disk timescale, inward migration is halted; they thus reach their final position at a relatively large distance from the parent star.","Functions Label":1}
{"Functions Text":"Specifically, we create mock data cubes that mimic ALFALFA observations","Functions Label":2}
{"Functions Text":"Recent work also finds that transient spiral structure","Functions Label":0}
{"Functions Text":"may lead to the formation of moving groups,","Functions Label":0}
{"Functions Text":"Thus, in order to discover all planets in a system, one either needs to image old stars \u2013 which seems currently impossible given the already low detection rate around young stars probed by large DI surveys (e.g.,","Functions Label":0}
{"Functions Text":"\u2013 or try to minimize the impact of the stellar activity of young stars.","Functions Label":0}
{"Functions Text":"Furthermore, even spherical grains can produce polarized emission by self-scattering of large grains in an anisotropic radiation field","Functions Label":1}
{"Functions Text":"FSRQs have high luminosity and a thin and radiatively efficient black hole accretion disk","Functions Label":0}
{"Functions Text":"Besides RAVE, other surveys have published successive DRs that are available for public use. At the time of writing, there is open access to the DR16 of the Apache Point Observatory Galactic Evolution Experiment (APOGEE;","Functions Label":0}
{"Functions Text":"The user defined heating is therefore highly stratified, spatially smooth and steady (e.g.","Functions Label":1}
{"Functions Text":"KOI-94","Functions Label":3}
{"Functions Text":"is interesting because of the presence of a Saturn mass planet in a similar orbit to 55 Cancri.","Functions Label":3}
{"Functions Text":"The innermost planet lies just outside a pair of secular resonances at 3.0 d (eccentricity) and 3.4 d (inclination) and so is consistent with a lack of inclination excitation. If we allow for the existence of a 1 M\u2295 planet interior to this, eccentricity resonances are found at 0.9 and 2.1 d (and a mean motion resonance at 1.9 d) and inclination resonances at 1.2 and 2.1 d. Thus, a planet that has tidally migrated to orbital periods 2 d in this system could have had its inclination pumped up and have avoided transit.","Functions Label":1}
{"Functions Text":"We expect to detect the GWB first, followed by detection of individual SMBHBs","Functions Label":0}
{"Functions Text":"that stand out above the GWB.","Functions Label":0}
{"Functions Text":"In particular, the damping behavior of a large plate or surface is expected to differ from that of a same-sized particle, so that the velocity dependence of the coefficient of restitution might be an effect of the experimental setup in","Functions Label":1}
{"Functions Text":"and Higa et al. (1996).","Functions Label":1}
{"Functions Text":"Strong non-potential field arcades have been observed in hot X-ray sigmoids on scales of hundreds of arseconds","Functions Label":0}
{"Functions Text":"This range of lengths over a range of temperatures and magnetic field topologies points directly to self-similar mechanisms influencing plasma and magnetic field dynamics at a range of scales.","Functions Label":0}
{"Functions Text":"Absorption coefficients for pure water ice (kH2O) at sub-mm-to-cm wavelengths are discussed extensively by","Functions Label":0}
{"Functions Text":"who also provides several analytic formulations to estimate them as a function of frequency and temperature along with illustrative plots.","Functions Label":0}
{"Functions Text":"This trend is in agreement with the metallicity dependent yields from","Functions Label":5}
{"Functions Text":"which provide higher carbon as [Fe\/H] increases from massive stars (i.e. also increasing the O production) but lower carbon from low and intermediate mass stars as [Fe\/H] increases (i.e. less production of C).","Functions Label":5}
{"Functions Text":"Recent numerical studies","Functions Label":0}
{"Functions Text":"show that the retention of BHs in dense stellar clusters of wide mass range, beginning from low-\/medium-mass young and open clusters","Functions Label":0}
{"Functions Text":"through globular clusters","Functions Label":0}
{"Functions Text":"comprise environments where BHs can pair up through close dynamical interactions, which, furthermore, lead to general-relativistic (hereafter GR) coalescences of these BBHs.","Functions Label":0}
{"Functions Text":"We note that in our calculations, we assume a source size that is 1.8 times larger than the FWHM, following the approach of Readhead (1994) and","Functions Label":2}
{"Functions Text":"We followed the second approach since there are natural thermal instabilities in the plasma, such as instability caused by X-ray irradiation","Functions Label":2}
{"Functions Text":"The abundances of these rare but massive subhaloes has important implications for, among others, the statistics of massive satellite galaxies (e.g.","Functions Label":3}
{"Functions Text":"The prior mean functions that we discussed are the following: zero mean function, the theoretical function of angular size calculated from the angular diameter distance under the assumption of three cosmological models: flat \u039bCDM with \u03a9m = 0.27, so-called Rh = ct universe","Functions Label":2}
{"Functions Text":"A cross-correlation method was applied to derive continuous 2D speed maps of a CME from coronagraphic images by","Functions Label":2}
{"Functions Text":"As seen in Fig. 8 there are no Bullet cluster analogues (structures of approximate mass and dissociation) in L210N1024NR, this is unsurprising as a simulation requires a significantly larger volume than that of L210N1024NR ((210cMpc\u2009h\u22121)3) to expect such an object (e.g.","Functions Label":2}
{"Functions Text":"This phenomenon is observed to start at higher frequencies (where the emission is produced closer to the compact object) and terminates as the jet break evolves through the radio band","Functions Label":0}
{"Functions Text":"There are two primary causes for darkness in GRBs: attenuation by dust, or rest frame ultraviolet H\u2009i absorption at high redshift","Functions Label":0}
{"Functions Text":"The number density of the ambient medium is assumed to be","Functions Label":2}
{"Functions Text":"In absorption, bands at 3.4, 6.85, and 7.25 \u03bcm are also observed in the diffuse interstellar medium (ISM) of our Galaxy, as well as in extragalactic ISM, and can be well represented by a material with a significant amount of aliphatic character, also called HAC or a-C:H, which is a family of hydrogenated amorphous carbons (e.g.","Functions Label":5}
{"Functions Text":"there is a second OB star mentioned by","Functions Label":0}
{"Functions Text":"but its location is actually outside the structure","Functions Label":0}
{"Functions Text":"The origin of hard lag is not clearly known. One possible explanation is provided by the propagation fluctuation model in which fluctuations associated with accretion flow propagate inwards in an accretion disc and thus resulting in the emission of the soft photons from relatively outer regions earlier than the hard photons from the innermost regions","Functions Label":0}
{"Functions Text":"The Sun is situated at the inner edge of the Orion arm","Functions Label":0}
{"Functions Text":"Also for dSphs, for which the determination of the dark matter density distribution is more difficult, there are indications that cored dark matter density profiles may be favoured with respect to cuspy profiles","Functions Label":1}
{"Functions Text":"though this finding is still debated","Functions Label":1}
{"Functions Text":"The discrepancy can be calculated using a statistic like \u03c72","Functions Label":1}
{"Functions Text":"but here we will work with the Freeman\u2013Tukey discrepancy since it is weight independent","Functions Label":1}
{"Functions Text":"We assume ages between about 100 yr, for the most compact sources, and 105 yr for sources with LS of several kpc, as derived from radiative and kinematic ages of sources (e.g.","Functions Label":2}
{"Functions Text":"These values were computed by an analysis of the differences between the Portsmouth stellar masses of our galaxies","Functions Label":2}
{"Functions Text":"Previous studies have considered the implications of structure models on the true energetics and rates of GRBs","Functions Label":0}
{"Functions Text":"while the \u03a3nl parameter encodes the smoothing of the BAO peak due to non-linear effects","Functions Label":2}
{"Functions Text":"Especially during recent decades, high-resolution observations of solar super-fine structures indicate that small spicules, minor hot jets along small-scale magnetic channels from the low atmosphere upwards to the corona, petty tornados and cyclones, and small explosive phenomena such as mini-filament eruptions and micro- and nano-flares\u2014all of these small-scale magnetic activities contribute greatly to coronal heating","Functions Label":0}
{"Functions Text":"In this case, the multiple bright blobs are plasmoids formed by bursty reconnection in this current sheet, another phenomenon commonly found in high-Lundquist-number reconnection simulations (e.g.,","Functions Label":2}
{"Functions Text":"Our estimate of the stellar mass fraction agrees","Functions Label":5}
{"Functions Text":"and with the estimates from strong lensing studies (see for example","Functions Label":5}
{"Functions Text":"which produced stellar mass fractions in the range 30%\u00e2\u0080\u009370% integrated inside the Einstein radius of the lenses.","Functions Label":5}
{"Functions Text":"In particular, solar wind samples containing more Alfv\u00e9nic fluctuations are typically associated with less developed turbulence, as inferred from both shallower spectra and reduced intermittency (see","Functions Label":0}
{"Functions Text":"and references therein).","Functions Label":0}
{"Functions Text":"Conversely, for LINERs, that are powered by RIAF discs, the relation between bolometric AGN and jet power is difficult to model because jet emission can dominate their entire SED","Functions Label":1}
{"Functions Text":"The foregrounds, system noise, and calibration errors together keep the current observations at bay from directly detecting the EoR 21-cm signal. As a consequence, the first detection is likely to be statistical in nature. These observations plan to measure the power spectrum (PS) of the EoR 21-cm signal (e.g.","Functions Label":3}
{"Functions Text":"Therefore, during our fitting procedure we use the frequencies determined in","Functions Label":2}
{"Functions Text":"as starting values plus their derived errors as Gaussian priors","Functions Label":2}
{"Functions Text":"Magnetic braking of the system is a possible explanation for the measured $\\dot{P}$, but other explanations, such as resonant interactions between the binary and the possible circumbinary disc, have been proposed","Functions Label":1}
{"Functions Text":"while \u2018achromatic\u2019 flux variability (no colour evolution,","Functions Label":0}
{"Functions Text":"have also been reported.","Functions Label":0}
{"Functions Text":"Even though arguments (e.g. variability,","Functions Label":6}
{"Functions Text":"exist that favour a compact corona, we used extended coronae.","Functions Label":6}
{"Functions Text":"To obtain the structural parameters of the LSBG candidates, the detected sources are usually fitted with a S\u00e9rsic model","Functions Label":1}
{"Functions Text":"Specific procedures such as GALFIT","Functions Label":1}
{"Functions Text":"or IMFIT","Functions Label":1}
{"Functions Text":"are used to obtain accurate morphological and structural parameters. However, the computational cost of these is very high, becoming a bottleneck in LSBG analysis pipelines. For this reason, it is advisable to minimize the number of LSBG candidates prior to their S\u00e9rsic fitting to save computational time. This is not trivial because structural parameters from automated segmentation catalogs are much less accurate than S\u00e9rsic fit modeling, making correct screening of the sample challenging. As a last step, a \u201csupervision\u201d of all the objects matching the criteria of the sample is necessary in order to discard the frequent presence of false positives. These are sources that, although meeting the imposed criteria, are clearly not LSBGs. Examples of false positives are clumped sources that have been considered as a single source, faint reflections due to the optics of the instrumentation, or artifacts present in the images. Depending on the data volume analyzed, the number of objects to be supervised can become very high.","Functions Label":1}
{"Functions Text":"Other single-dish samples of SMGs have also been obtained at 1.1\u20131.3 mm using","Functions Label":0}
{"Functions Text":"and at 2 mm with GISMO","Functions Label":0}
{"Functions Text":"A few years later the authors searched with a larger field systematically around many nebulae for extended emission features without detecting the very low surface brightness halo we investigate here","Functions Label":0}
{"Functions Text":"The model uses the hybrid approximation where electrons are considered as a massless, charge-neutralizing fluid and ions are described by a particle-in-cell model","Functions Label":2}
{"Functions Text":"It has been shown elsewhere that these models produce similar results to those of numerical cosmological simulations and other SAMs","Functions Label":5}
{"Functions Text":"and that they are also in agreement with higher redshift observations of galaxy populations","Functions Label":5}
{"Functions Text":"the reionization history","Functions Label":5}
{"Functions Text":"We also show the Spitzer Infrared Nearby Galaxy Sample","Functions Label":2}
{"Functions Text":"analyzed in da Cunha et al. (2008) as purple stars for comparison.","Functions Label":2}
{"Functions Text":"But why is there such a wide range of radial gradient slopes measured? There are several possibilities. (1) Measurement uncertainty. Measurement errors will cause some variations, but it is unlikely to produce a factor of 3 difference in slope. Homogeneity in observing procedures and data analysis may be more important given the variations in abundance that can be derived for the same source (for further discussion see","Functions Label":1}
{"Functions Text":"The angular speed was estimated based on the global velocity gradient along the major axis of the dense core observed with single-dish telescopes","Functions Label":2}
{"Functions Text":"Following the results shown in Fig. 2 of","Functions Label":2}
{"Functions Text":"we roughly estimated that XO-2N could have ingested an amount of iron slightly higher than 5 M\u2295 to increase its photospheric iron content by ~0.05 dex, given its Teff ~ 5300 K.","Functions Label":2}
{"Functions Text":"The Albedos, A1 and A2, and gravity darkening coefficients, g1 and g2, were set to generally adopted values for the given spectral types of the components","Functions Label":2}
{"Functions Text":"Marks et\u00c2 al. (2014, in preparation) show that random pairing with subsequent dynamical processing does indeed reproduce at least the observed low-mass stellar population (see also","Functions Label":0}
{"Functions Text":"This initial binary population is then altered by dynamical evolution. Close binaries with orbital periods below about 10\u00c2 days undergo eigenevolution","Functions Label":0}
{"Functions Text":"and tend to equalize the companion masses. Note that this eigenevolution term alters the very-low-mass end of the star-like IMF. For the purpose of this work, however, these effects only play a negligible role.","Functions Label":0}
{"Functions Text":"Strong non-potential field arcades have been observed in","Functions Label":1}
{"Functions Text":"micro-sigmoids in soft X-ray imaging on scales of \u223c50\u2033","Functions Label":1}
{"Functions Text":"and now at EUV temperatures in QS-like mixed network fields with lengths down to \u223c10\u2033. This range of lengths over a range of temperatures and magnetic field topologies points directly to self-similar mechanisms influencing plasma and magnetic field dynamics at a range of scales.","Functions Label":1}
{"Functions Text":"A number of detailed studies suggest that the radio emission beam consists of a central core emission surrounded by conal emission arranged in nested rings","Functions Label":0}
{"Functions Text":"Surveys of radio bursts in decimetric wavelengths is presented in papers by Isliker & Benz (1994) and","Functions Label":0}
{"Functions Text":"within 1\u20133 GHz and 0.8\u20132.0 GHz frequency ranges, respectively.","Functions Label":0}
{"Functions Text":"FDs caused by high-speed streams (HSS) from coronal holes (CHs) have a recurrent character","Functions Label":0}
{"Functions Text":"Let us stress that implementing nulling in weak-lensing analysis is central in order to avoid extracting biased information from the small scales that lack a full theoretical understanding (including due to the effect of baryon physics that needs to be modelled in weak-lensing surveys","Functions Label":7}
{"Functions Text":"This magnetic structure would also be consistent with polarised radio synchrotron emission above and below the planes of galaxies known to host outflows in the nearby Universe, with the polarisation direction aligned with the orientation of the outflow cone (see, e.g.","Functions Label":5}
{"Functions Text":"Also, we consider $Q^{+}_{{\\rm diss}}-Q^{-}_{{\\rm rad}}=fQ^{+}_{{\\rm diss}}$ in ADAFs (where f, the advection parameter, is defined by","Functions Label":2}
{"Functions Text":"The linear relationship that we observe between breakpoint energy and core temperature is in line with previous measurements (e.g.","Functions Label":5}
{"Functions Text":"for both the halo and strahl.","Functions Label":5}
{"Functions Text":"For more details, we refer the readers to","Functions Label":0}
{"Functions Text":"While we know that very massive stars (VMS) above 100\u2009\u2009M\u2299 exist","Functions Label":0}
{"Functions Text":"this mass is significantly diminished via stellar winds already during core hydrogen (H) burning","Functions Label":0}
{"Functions Text":"Previous works","Functions Label":1}
{"Functions Text":"have found very high reddening and densities associated with ionised outflows in local objects","Functions Label":1}
{"Functions Text":"Perhaps a more likely mechanism is convective overshooting, which was first studied by Freytag et al. (1996) in a white dwarf context and more recently by Tremblay et al. (2015) and","Functions Label":0}
{"Functions Text":"through detailed 3D simulations.","Functions Label":0}
{"Functions Text":"High-mass star forming regions (HMSFRs) also present a rich chemical diversity. One of the best known examples is provided by Orion-KL. This source harbours: (i) a dichotomy between the spatial distribution of complex O-bearing and complex N-bearing species, with the latter species probing the hotter gas (see,","Functions Label":0}
{"Functions Text":"The","Functions Label":0}
{"Functions Text":"photometric follow-up started in August, 2010, and ended in October, 2012, coinciding with these LBT data.","Functions Label":0}
{"Functions Text":"The discrepancy is even larger in the case of the low-mass models of","Functions Label":6}
{"Functions Text":"After combining with the existing NB2071 data (186 min integration), we reconstructed all the data using the reduction pipeline mcsred2","Functions Label":2}
{"Functions Text":"which is written as iraf3 scripts","Functions Label":2}
{"Functions Text":"Using the diagonal elements of the 14N quadrupole coupling tensor in NEFA","Functions Label":2}
{"Functions Text":"we have computed the expected hyperfine splitting of all lines in the W band.","Functions Label":2}
{"Functions Text":"From studies on the optical\u2013IR colour\u2013magnitude diagram, it is known that FSRQs in general show an RWB trend, which is attributed to them having a luminous accretion disc","Functions Label":0}
{"Functions Text":"Based on a literature review for papers where VLBI parallax measurements were determined using an in-beam calibrator, we find 24 similar measurements, the majority of which have been used to measure parallaxes to pulsars","Functions Label":2}
{"Functions Text":"These galaxies hereafter referred to as LyC leakers, possess many properties similar to those of high-redshift galaxies both at z \u223c 2\u20133 and z$\\gtrsim$ 6 such as compact morphology with similar galaxy radii (e.g.","Functions Label":1}
{"Functions Text":"Later on, Gomes et al. (2005), Gallardo et al. (2012), and","Functions Label":0}
{"Functions Text":"showed that the Lidov\u2013Kozai mechanism raised by the giantplanets inside a mean-motion resonance with Neptune is able to raise the perihelion of small bodies beyond 60 au in a few thousands of million years.","Functions Label":0}
{"Functions Text":"Since these characteristics are somewhat consistent with model predictions for drift mode of MTSI","Functions Label":5}
{"Functions Text":", we do not rule out the possibility of some waves at certain frequencies and during some intervals being generated by the slow drift mode of MTSI.","Functions Label":5}
{"Functions Text":"We used data for two clusters observed by Kaluzny and his collaborators with the highest number of CBs (except for \u03c9 Centauri).","Functions Label":2}
{"Functions Text":"In M4,","Functions Label":0}
{"Functions Text":"detected nine CBs with one BS among them","Functions Label":0}
{"Functions Text":"Polarimetricimages with","Functions Label":2}
{"Functions Text":"SPHERE","Functions Label":2}
{"Functions Text":"show a gap at around 36 au, with an outer ring at a separation >40 au from the star.","Functions Label":2}
{"Functions Text":"In this concern, a large family of dynamical DE models with time-varying EoS parameters has been proposed in the literature (for some earlier attemts, see","Functions Label":0}
{"Functions Text":"However, there is an important caveat; PAHs are destroyed by ionizing radiation from newly formed stars","Functions Label":1}
{"Functions Text":"leading to a deficit in the 8 \u03bcm luminosity in galaxies with low metallicity, whereas PAHs are less well shielded by metals","Functions Label":1}
{"Functions Text":"Extreme mass ratio systems are prone to unstable mass transfer and thus to CEE, and although the exact value of the boundary is not well-constrained, we assume that this occurs for evolved donors in systems with q\u2004\u2272\u20040.4, following previous works such as Wellstein et al. (2001), Hurley et al. (2002) and","Functions Label":0}
{"Functions Text":"In Fig. 5 we compare the distributions of the core radii (Rcore) constrained by the V06 model and the concentration parameter (cSB) between these two samples.","Functions Label":1}
{"Functions Text":"The concentration parameter is defined as the ratio of the surface brightness within 0.1 R500 to the surface brightness within R500","Functions Label":0}
{"Functions Text":"Intuitively, the expectation is that the smaller the core radius, the more compact the cluster.","Functions Label":0}
{"Functions Text":"The left panel of Fig. 5 clearly shows that the clusters in the point source sample have relatively smaller core radii, hence the emission is more concentrated in a smaller area. Consistently, the concentration of the point source sample shows a clear excess in higher values than the extent-selected sample, indicating that a significantly larger fraction of cool-core clusters and clusters host a central AGN.","Functions Label":1}
{"Functions Text":"assuming a mean beam efficiency \u03b7MB = 0.49","Functions Label":2}
{"Functions Text":"In space, an analogous process to carbon soot formation occurring on Earth can be initiated through the completion of that first aromatic ring and may also lead to the synthesis of PAHs","Functions Label":0}
{"Functions Text":"This has led to significant theoretical development, focused on the resonant interaction of electrons with the whistler and fast-magnetosonic whistler (FM\/W) modes (e.g.","Functions Label":0}
{"Functions Text":"Observations have struggled to confirm these theories.","Functions Label":6}
{"Functions Text":"Moreover, the degree of central concentration of a halo depends on its formation epoch and hence on its total mass (e.g.,","Functions Label":1}
{"Functions Text":"This is consistent with the magnetic field measured by Hubrig et al. (2009), 89 \u00b1 26 G, although non detections have also been reported","Functions Label":5}
{"Functions Text":"In our long-term project aimed at reconstructing the past magnetic activity on the Sun","Functions Label":3}
{"Functions Text":"we also use indirect measurements of magnetic fields obtained, in particular, from chromospheric spectroheliograms.","Functions Label":3}
{"Functions Text":"In the work by","Functions Label":2}
{"Functions Text":", the maximum of the field strength was found to be 0.15 T. The magnetic field could be even stronger in the active region near the sunspot. Therefore, we set b0 = 0.05 T in Case I and Case II, and b0 = 0.15 T in Case IIa.","Functions Label":2}
{"Functions Text":"Historically, systematic studies of galactic outflows in nearby and high-z galaxies have focused on","Functions Label":0}
{"Functions Text":"and the atomic phase \u2013 based on the Na D or Mg II lines in absorption (e.g.,","Functions Label":0}
{"Functions Text":"Moreover, it is observed that this relationship does not apply to radio-loud magnetars, which in general show larger duty cycles than what one would expect from the extrapolation of this tentative relation for radio pulsars to magnetars (see, e.g.,","Functions Label":1}
{"Functions Text":"To allow fast calculations, we make the major assumption that the grains are spherical and compute their optical properties using the Mie theory","Functions Label":2}
{"Functions Text":"with the Fortran 90 version of the BHMIE routine given in","Functions Label":2}
{"Functions Text":"The oxygen line ratio [O\u202fIII]\u03bb 5007 \u00c5\/[O\u202fII] \u03bb\u03bb3726, 3728 \u00c5 (O32) proposed by Jaskot & Oey (2013) and","Functions Label":2}
{"Functions Text":"was successfully used to select LyC-leaking candidates","Functions Label":2}
{"Functions Text":"From the theoretical point of view, it is believed that low-mass main-sequence stars synthesize 3He through the p\u2013p chains with peak abundances of few 10\u22123 by number","Functions Label":0}
{"Functions Text":"We note that the measured values must be corrected for instrumental effects, in particular for the signal convolution with the instrumental PSF, which can introduce significant cancellation of the disk signal","Functions Label":2}
{"Functions Text":"first presented the dynamical estimate of mass of the source to be around 7.4 \u00b1 1.1\u2009M\u2299.","Functions Label":2}
{"Functions Text":"It was only in 1928 that Baade first classified it as a GC owing to its high latitude, richness in faint stars and presence of variable stars","Functions Label":0}
{"Functions Text":"First, ultra-hot Jupiters are accessible objects to observe. Their short orbital periods (1\u20132\u2009d) and hot, extended atmospheres make them perfect targets for transmission spectroscopy","Functions Label":3}
{"Functions Text":"Based on a radial velocity of $-13\\pm 17\\, {\\rm km^{\\rm -1}}$ and a distance of 2.07 \u00b1 0.18 kpc","Functions Label":2}
{"Functions Text":", we can calculate the UVW velocities of the SM star, i. e. $U=-5.2\\pm 14\\, {\\rm km^{\\rm -1}}$, $V=197\\pm 10\\, {\\rm km^{\\rm -1}}$, and $W=3.1\\pm 5\\, {\\rm km^{\\rm -1}}$.","Functions Label":2}
{"Functions Text":"From the application of Comptonization models, such high-energy data allow to constrain the plasma temperature, which is commonly found to range from 50 to 100 keV","Functions Label":0}
{"Functions Text":"Each of the new detrended light curves, jointly with the nominal PDC-SAP flux, is then processed through the transit least squares (TLS) package","Functions Label":2}
{"Functions Text":"in the search for transits.","Functions Label":2}
{"Functions Text":"In contrast to the classical box least-squares (BLS) algorithm","Functions Label":1}
{"Functions Text":"the TLS algorithm uses an analytical transit model that takes the stellar parameters into account.","Functions Label":1}
{"Functions Text":"For the case of \u03b2 Pictoris and HD 169142, also having giant planets at long distances, CA models seem to be favored","Functions Label":0}
{"Functions Text":"The exact value of the interferometer\u2019s modulation efficiency (ME), which acts essentially as an additional throughput loss, is the major source of uncertainty on the absolute flux calibration","Functions Label":0}
{"Functions Text":"We also show as a gray band the best fit for the stellar fraction in the form of stars determined by","Functions Label":2}
{"Functions Text":"in a study of a large sample of lens galaxies using strong lensing and photometry,","Functions Label":2}
{"Functions Text":"In the past decade, owing to the rise of large spectroscopic surveys of galaxies with well-determined physical properties (e.g. SDSS), all sky UV surveys (e.g. GALEX), and improved sensitivity of UV spectrographs (e.g. COS), studies of the gaseous haloes of galaxies could systematically connect gas absorption properties to galaxy properties in statistically meaningful samples (e.g.","Functions Label":0}
{"Functions Text":"the number of known SMGs is now of the order of a few thousand (e.g.,","Functions Label":0}
{"Functions Text":"and intensive observational efforts have been devoted to understanding their physical properties.","Functions Label":0}
{"Functions Text":"Dissipative effects such as shear and bulk viscosities work towards suppressing GR driven instabilities and has been studied by various authors over the past few years","Functions Label":0}
{"Functions Text":"We recall that in these models (see also","Functions Label":2}
{"Functions Text":"the dense clouds can be either self-gravitating virialised clouds, which implies that their internal velocity dispersion (\u0394vsg) is locked to their mass (Mvir) and size (R) through \u0394vsg\u2004=\u2004(GMvir\/G)1\/2, or unbound clouds, for which \u0394v\u2004\u226b\u2004\u0394vsg.","Functions Label":2}
{"Functions Text":"We approximate the PSR body as a perfect sphere. However, due to the spin of the PSR the true shape is more oblate. This will ultimately influence the pitch angle of the ray with the neutron star surface. This effect is considered to be minor, but the method could easily be extended to account for this oblateness (see","Functions Label":7}
{"Functions Text":"XRD performed by","Functions Label":1}
{"Functions Text":"of the sample of bayerite prepared at 1273 K suggests only \u03b8-alumina was present, and their infrared and NMR spectroscopy confirms this.","Functions Label":1}
{"Functions Text":"From the convective flux as presented in","Functions Label":5}
{"Functions Text":"one also would expect a similar temperature gradient in the overshooting zone.","Functions Label":5}
{"Functions Text":"Of course, the recent report of an absorption signal in the sky-averaged spectrum at z \u223c 17 from EDGES (Bowman et al. 2018)","Functions Label":3}
{"Functions Text":"or a brighter background","Functions Label":3}
{"Functions Text":"than models in \u039bCDM cosmologies generally predict.","Functions Label":3}
{"Functions Text":"Subsequent observations have led to the detection of new metastable ammonia masers, including","Functions Label":0}
{"Functions Text":"NH3 (2,2)","Functions Label":0}
{"Functions Text":"However, over the last few years a number of multifrequency compact source detection techniques have been proposed in the literature","Functions Label":3}
{"Functions Text":"Despite a direct conflict","Functions Label":1}
{"Functions Text":"with the theoretical expectation that the IMF should vary as the star-forming environment alters","Functions Label":1}
{"Functions Text":"the observed IMFs of star clusters in the local Universe are consistent with no variation","Functions Label":1}
{"Functions Text":"In this case, the mass of the white dwarf is also calculated from the IMFR of","Functions Label":2}
{"Functions Text":"Many previous works","Functions Label":2}
{"Functions Text":"used a constant smoothing length.","Functions Label":2}
{"Functions Text":"Using 3D simulations,","Functions Label":0}
{"Functions Text":"computed mode line profiles in both the velocity and the intensity power spectrum alternatively at mean unity optical depth and instantaneous unity optical depth. Their results indeed show that the modulation of the \u201cobserved\u201d intensity fluctuations due to radiative transfer could be significant enough to reverse the sense of mode asymmetry.","Functions Label":0}
{"Functions Text":"For the lowest 41 energy levels, we see that our calculated energies and previous fac energies","Functions Label":5}
{"Functions Text":"belonging to the n = 3 complex in Ni\u2009xiv agree well with each other and both set of calculation are of the same accuracy.","Functions Label":5}
{"Functions Text":"However, our calculated ground state configuration levels show better agreement with measured energies in comparison to those of fac calculations (7.2 per cent).","Functions Label":6}
{"Functions Text":"As predicted by asymptotic theory, the pulsation periods for \u03b3 Dor and SPB stars were observed to form period spacing patterns (e.g.","Functions Label":0}
{"Functions Text":"On the other hand, the stellar rotation leads to shifts in the observed pulsation mode frequencies","Functions Label":3}
{"Functions Text":"Indeed, the ultraviolet and X-ray variability detected for many of these LINERs","Functions Label":1}
{"Functions Text":"is in favour of a direct view of the AGNs (i.e. perpendicular to the disc under the UM).","Functions Label":1}
{"Functions Text":"This is consistent with the fact that most of the [O\u2009III] morphologies found for LINERs are spheroids, if we assume that the [O\u2009III] traces the NLR.","Functions Label":5}
{"Functions Text":"These objects spend most of their time in quiescence at very low accretion rates, but occasionally, they produce outbursts that last from a few months to a year. Their flux then rises by several orders of magnitude across the whole electromagnetic spectrum (see, e.g.,","Functions Label":0}
{"Functions Text":"WDS 02499+0856 turned out to be a quadruple system, when the northern component was found to be a double-lined (SB2) binary from the DDO spectroscopic observations","Functions Label":0}
{"Functions Text":"Typically about a dozen events occur during each solar cycle, although only two GLEs were reported in cycle 24, probably due to the change in the state of the heliosphere","Functions Label":0}
{"Functions Text":"SEP events with gigaelectronvolt components are accompanied by type II radio bursts from meter (m) wavelengths to kilometer (km) wavelengths","Functions Label":0}
{"Functions Text":"Many important results were noticed based on the spectral fitting of RXTE data of this source. The mass accretion rate was found to be constant along with the Z phase in Sco-like variation and different mechanisms were proposed to explain the spectral and timing variations during the Z phase variations","Functions Label":0}
{"Functions Text":"he RWI can be triggered at steep radial density gradients","Functions Label":0}
{"Functions Text":"such a gradient may be generated at the viscosity transition between regions in which the magnetorotational instability can operate (e.g.","Functions Label":0}
{"Functions Text":"This group was complemented by","Functions Label":2}
{"Functions Text":"the four candidate HVSs from the LAMOST survey","Functions Label":2}
{"Functions Text":"Numerous studies have been performed using chemical models","Functions Label":0}
{"Functions Text":"For comet 8P\/Tuttle, it is however not possible to distinguish the solution of a binary nucleus that formed in the first billion years of our Solar System","Functions Label":1}
{"Functions Text":"from a more recent origin following its injection into the inner Solar System (e.g.,","Functions Label":1}
{"Functions Text":"Low gas temperatures are associated with Serpens South ranging from 8.9 to 16.8 K with an average of 12.3 \u00b1 1.7 K, which is consistent with the mean value of 11 \u00b1 1 K found by","Functions Label":5}
{"Functions Text":"This seems to suggest that its presence closely traces star formation sites, resulting in a linear relation, as found by De Looze et al. (2014) and Herrera-Camus et al. (2015). While at low-redshift and close to solar metallicity such a relation is well established, as shown by several observations","Functions Label":5}
{"Functions Text":"and also numerical simulations (see, e.g.","Functions Label":5}
{"Functions Text":"significant deviations can arise in different ISM conditions, like at lower metallicity or in presence of a strong ionizations field, that are more typically found in the high-redshift Universe.","Functions Label":1}
{"Functions Text":"Improvements in cosmological measurement in recent years have been said to hail an era of \u201cprecision cosmology,\u201d with observations of","Functions Label":0}
{"Functions Text":"luminosity distance\u2013redshift relation of Type Ia supernovae (SNIa;","Functions Label":0}
{"Functions Text":"providing constraints on cosmological model parameters at percent, or subpercent, level precision.","Functions Label":0}
{"Functions Text":"Possible compact-object merger pathways include isolated binary evolution","Functions Label":0}
{"Functions Text":"accompanied by mass transfer","Functions Label":0}
{"Functions Text":"These parameters are entirely consistent with those found in preliminary studies","Functions Label":5}
{"Functions Text":"Here, we present a new approach to derive the VDF based on the lens redshift distribution","Functions Label":2}
{"Functions Text":"and to constrain its evolution out to z \u223c 1, given its strong dependency on the dynamical properties of galaxies (i.e. stellar velocity dispersion) and the number density of gravitational lenses (i.e. galaxy evolution).","Functions Label":2}
{"Functions Text":"Beyond this redshift, matters are complicated by uncertainties about the density evolution and the build-up of high black hole masses in the early universe","Functions Label":0}
{"Functions Text":"These conclusions have been strengthened by recent observations by Siana et al. (2015), who found no convincing detection in their deep HST imaging with WFC3-UVIS of five LyC emitters extracted from the sample of Nestor et al. (2011), or by Mostardi et al. (2015), who only found one robust LyC emitter after a reanalysis of a sample of 16 galaxies by","Functions Label":5}
{"Functions Text":"However,","Functions Label":6}
{"Functions Text":"reported that there is no correlation between the turbulent and outflow energies.","Functions Label":6}
{"Functions Text":"Robust lens models of galaxy clusters are built thanks to the identification of large numbers of multiply lensed sources, which can span a large redshift range","Functions Label":0}
{"Functions Text":"The existence of a shock is also indicated by orbital-phase- and frequency-dependent radio eclipses of the MSP (since plasma structures at the shock attenuates the radio), where in RBs the eclipse fraction can be >50% (e.g.","Functions Label":0}
{"Functions Text":"of the orbital phase (while the MSP remains largely uneclipsed at inferior conjunction of the pulsar).","Functions Label":0}
{"Functions Text":"M15 show, via use of covariance spectra (see","Functions Label":0}
{"Functions Text":"for a review of the technique), that the ULX continuum emission originates from at least two components that cross at \u223c1 keV.","Functions Label":0}
{"Functions Text":"Recent observations during the STEREO era, however, question this simple picture, especially since the nature of events showing wide longitudinal SEP spreads appears to be more complicated. It was found that 3He-rich events extend over more than 130\u00b0 in longitude","Functions Label":0}
{"Functions Text":"and that near-relativistic electron events can spread up to almost all around the Sun.","Functions Label":0}
{"Functions Text":"For these reasons, detections in emission at high-redshifts are currently limited to deep fields","Functions Label":3}
{"Functions Text":"while detections at z1 are now becoming available","Functions Label":3}
{"Functions Text":"Many studies of the outburst evolution of these sources have been reported in the literature (e.g.","Functions Label":0}
{"Functions Text":"the various outbursts observed do not have any detectable recurrence period and, in addition, show a complex behaviour in both soft and hard energy ranges and very different luminosities.","Functions Label":0}
{"Functions Text":"The angular expansion rate of 0.64 arcsec yr\u22121 obtained from comparing X-ray images from 2007 and 2009","Functions Label":2}
{"Functions Text":"gives an upper limit for the age of about 160 yr, less if (as is almost certainly the case) deceleration has occurred;","Functions Label":2}
{"Functions Text":"This boils down to quantifying the relation between molecular gas and star formation rate (SFR), which appears nearly linear in nearby discs","Functions Label":0}
{"Functions Text":"In precision cosmology, Bayesian inference is the main tool for setting constraints on cosmological parameters","Functions Label":0}
{"Functions Text":"Both the correlation of VHE emission with the CMZ and the lack of a cutoff in the diffuse spectrum support a hadronic scenario, capable of explaining both VER J1745\u2013290 and the diffuse emission","Functions Label":0}
{"Functions Text":"The three transitions of singly ionized Sulfur (Sii; upper ionization potential 23.3 eV) at \u03bb\u03bb1250.58, 1253.81, 1259.52\u00c5 represent important tracers for neutral and weakly ionized gas in the local interstellar and intergalactic medium and in distant galaxies (e.g.","Functions Label":2}
{"Functions Text":"In addition, the apparent speed and length of these network jets are positively correlated, which is very similar to what has already been reported in previous works","Functions Label":5}
{"Functions Text":"with the sole exception of cluster ESO121-3 and very recently also KMHK1592, as reported by","Functions Label":6}
{"Functions Text":"Later, indirect evidence of the existence of intracluster magnetic fields has been given by several statistical studies on the effect of the Faraday rotation on the radio signal from background galaxies or galaxies embedded in galaxy clusters","Functions Label":0}
{"Functions Text":"The nonlinear PT for MG was developed initially in","Functions Label":2}
{"Functions Text":"and has been further studied in several other works","Functions Label":4}
{"Functions Text":"Observations on smaller, sub galactic scales, have proven more problematic for \u039bCDM, with suggestions that the low abundance (e.g.","Functions Label":1}
{"Functions Text":"inferred for haloes hosting Milky Way satellites are inconsistent with the numerous substructures with cuspy density profiles that form in Milky Way-like CDM haloes.","Functions Label":1}
{"Functions Text":"The LS-Ska","Functions Label":0}
{"Functions Text":"EoSs were constructed using the Skyrme effective nuclear forces Ska and SLy4, respectively.","Functions Label":0}
{"Functions Text":"The collision effect can become important in the case of higher density medium where the collision rate $\\tau _c^{-1}$ (either inelastic collision rate or Van der Waals collision rate) dominates over optical pumping rate $B_{lu}\\bar{J}^0_0$ (see","Functions Label":0}
{"Functions Text":"First, thermodynamic calculations of conditions in photodissociation regions (PDRs) have been coupled with self-consistent equations for the thermally driven disc wind","Functions Label":2}
{"Functions Text":"The confirmation of their cosmological origin allows them to be widely proposed as promising tools for studying the universe and fundamental physics, e.g., the distribution of baryons in the intergalactic medium (IGM) or diffuse gas","Functions Label":3}
{"Functions Text":"As a result, magnetars have been suggested as the central engines for some GRBs, including both long and short events","Functions Label":0}
{"Functions Text":"This problem might be alleviated in future simulations by introducing more realistic top boundary conditions like that used in","Functions Label":7}
{"Functions Text":"These vortices tend to have a long lifetime and are widely observed in space, laboratory, and numerical simulation of plasma","Functions Label":0}
{"Functions Text":"It was argued that magnetic flux ropes in the solar wind can be viewed to first order as being quasi-two-dimensional (quasi-2D) helical contracting and merging flux-rope structures based on three-dimensional (3D) simulations of compressible MHD turbulence that included a strong guide magnetic field","Functions Label":0}
{"Functions Text":"Following the approach of Nguyen et al. (2010), we have inferred a GCE relationship between \u03b429Si and initial 18O\/16O, which is based on a tight correlation between 29Si\/28Si and 46Ti\/48Ti ratios in SiC mainstream grains (Figure 11, left; data from","Functions Label":2}
{"Functions Text":"Such non-evolving VDF has been extensively applied in the previous studies on lensing statistics","Functions Label":0}
{"Functions Text":"n these regions, CRs have a wide variety of effects, one of the most important is being a producer of atomic hydrogen through the dissociation of H2","Functions Label":0}
{"Functions Text":"Secondly, the total metal flux into the disc across the outer boundary cannot exceed that supplied by advection of gas with metallicity $\\mathcal {Z}_{\\rm CGM}$ into the disc, since otherwise this would imply the presence of a metal reservoir external to the disc that is supplying metals to it, which is true only in special circumstances, e.g. during or after a merger","Functions Label":2}
{"Functions Text":"The dust-based estimates of G18 and","Functions Label":0}
{"Functions Text":"(and, by extension, the z\u2004\u223c\u20043 semi-constraints) assume a gas-to-dust ratio (G\/D).","Functions Label":0}
{"Functions Text":"We recall a few salient features obtained in those papers and reproduced here: in the initial stages (two leftmost panels), the rising portion of the flux tube has a mushroom shape, akin to an air bubble rising in water (e.g.,","Functions Label":5}
{"Functions Text":"We speculate that some stars of the Hyades stream might be remnants of the Hyades cluster, while others may be the dynamical effect of non-axisymmetric components","Functions Label":2}
{"Functions Text":"The RVs were measured using the two-dimensional cross-correlation algorithm TODCOR","Functions Label":2}
{"Functions Text":"The captured material can form a quasi-spherical shell","Functions Label":0}
{"Functions Text":"The standard internal shock model of blazars considers that the discrete ejecta with higher speeds (with Lorentz factor \u0393f) catch up with the preceding slower ejecta (with Lorentz factor \u0393s), and the collision leads to the nonthermal emission (e.g.,","Functions Label":0}
{"Functions Text":"Indeed, some misaligned circumbinary discs have already been reported","Functions Label":3}
{"Functions Text":"and HD 98800B","Functions Label":3}
{"Functions Text":"The two panels show model spectra at times t = 0, 1, 3, 5, and 7\u00e2\u0080\u0089Myr after a coeval burst of star formation, using evolutionary tracks with rotation, at solar metallicity (Z = 0.014 from","Functions Label":2}
{"Functions Text":"After the discovery of the first FRB","Functions Label":0}
{"Functions Text":"a number of dedicated facilities have been conducted to search FRBs, such as","Functions Label":0}
{"Functions Text":"and the Five-hundred-meter Aperture Spherical radio Telescope (FAST;","Functions Label":0}
{"Functions Text":"All these efforts result in an increasing rate of new FRB detections. Among them, more than 20 repeating FRBs have been reported.","Functions Label":0}
{"Functions Text":"If Tr 24 is also slightly younger than NGC 6231, as we argue below, our M-stars in Tr 24 will reach down to lower masses than in NGC 6231, with a steep increase in the detected M-star population: adopting the IMF from","Functions Label":2}
{"Functions Text":"the predicted number of cluster M stars doubles considering the mass interval 0.25\u20130.5 M\u2299 rather than 0.35\u20130.5 M\u2299.","Functions Label":2}
{"Functions Text":"The second scenario involves mass transfer episodes and the evolution of the binary is obtained following the prescriptions of the bse package","Functions Label":2}
{"Functions Text":"following the parameter assumptions detailed in Camacho et al. (2014).","Functions Label":2}
{"Functions Text":"The covariance of the 3PCF, on the other hand, is not diagonal, even for Gaussian fluctuations, which makes the modelling more difficult","Functions Label":0}
{"Functions Text":"In the last 20 years, disc-oscillation and resonance models and wave models have been proposed (e.g.","Functions Label":0}
{"Functions Text":"Temporal variability studies during the 2012 September\u2013October multi-band flaring period found a near-simultaneous \u03b3-ray and optical flaring behavior, inferring a co-spatial origin","Functions Label":1}
{"Functions Text":"As reported in previous works","Functions Label":2}
{"Functions Text":"this interval is characterized by two different spectral scalings: a typical inertial range \u223c \u03c45\/3 is found at large scales (i.e., \u03c4 > \u03c4b), while a steeper scaling \u223c \u03c47\/3 is found at small scales (i.e., \u03c4 \u03c4b), with \u03c4b \u223c 2.4 s","Functions Label":2}
{"Functions Text":"For a galaxy of halo mass Mh, the relation between the halo mass and the velocity dispersion is simply Mh = 2\u03c32R\/G; while the velocity dispersion can be directly related to the black hole mass using the MBH\u2013\u03c3 relation","Functions Label":2}
{"Functions Text":"The most basic result, already mentioned in Sect. 4.4.1, is that initial conditions which have a finite nonzero flux integral (called \u2018the mass\u2019 in the mathematical literature for the PME) converge toward the ZKBP solution with the same flux integral (\u2018mass\u2019) asymptotically in time","Functions Label":1}
{"Functions Text":"Theorem 18.2); here, allowance is made for either a positive or negative flux integral by globally changing the sign of the ZKBP solution","Functions Label":1}
{"Functions Text":"However, systems in a state of high mass accretion often do not show an optically thick soft X-ray component; instead, many exhibit optically thin hard X-ray emission","Functions Label":0}
{"Functions Text":"with an X-ray luminosity much smaller than expected, i.e., much smaller than the disk luminosity.","Functions Label":0}
{"Functions Text":"A significant contribution to the stack SED comes from a few sources, the most important one is RMC143. This was already identified as a massive nebula","Functions Label":0}
{"Functions Text":"Signatures of past mergers take the form of faint extended tidal features such as tails (e.g.","Functions Label":0}
{"Functions Text":"\u2013 which are typically produced by major mergers","Functions Label":0}
{"Functions Text":"Several studies of lower-luminosity AGN host morphologies with inactive control samples have been conducted in HST extragalactic survey fields (e.g.,","Functions Label":0}
{"Functions Text":"[C\u2009ii]\u2009158-\u03bcm luminosity, L[C\u2009II], has been discussed as an indicator of SFR (e.g.","Functions Label":3}
{"Functions Text":"One important thing to note, that is particularly relevant here, is that most of those coherent emitters for which we know the properties of the radio spectrum have quite steep spectra, typically going as \u03bd\u22122 or even \u03bd\u22123 (see e.g.","Functions Label":3}
{"Functions Text":", in contrast with a typical \u03bd\u22120.8 for optically thin synchrotron emission. This means that low-frequency instruments such as LOFAR may be intrinsically at an advantage to find coherent emitters (in addition to having larger fields of view).","Functions Label":3}
{"Functions Text":"the farthest blazar detected so far is at z = 5.47,","Functions Label":0}
{"Functions Text":"From 2008\u20132009 INTEGRAL data, Beckmann & Do Cao (2010) report a cut-off of \u223c80 keV with a hard photon index, but these results are not confirmed by NuSTAR","Functions Label":1}
{"Functions Text":"Studies of orbit composition of B\/PS bulges and X-structures in different numerical and analytical models","Functions Label":0}
{"Functions Text":"showed that an X-shape is observed in these models due to a tendency of a star to spend more time near turning points of its trajectory.","Functions Label":0}
{"Functions Text":"This is indeed the case for the realistic bar potential","Functions Label":0}
{"Functions Text":"In contrast to the Lempo system, all other known triples in the Solar system have their orbits almost regularly spaced, with one component much smaller than the others, with the most distant component being the largest","Functions Label":6}
{"Functions Text":"With the goal of identifying new exotic pulsar systems or highly stable MSPs suitable for PTA studies, the SPAN512 pulsar survey","Functions Label":3}
{"Functions Text":"was conducted between 2012 and 2018 at the NRT.","Functions Label":3}
{"Functions Text":"CS approaches based on constrained optimization problems, solved via convex optimization techniques, have been applied broadly in RI imaging","Functions Label":0}
{"Functions Text":"These techniques have shown promising results, with improvements in terms of image fidelity and flexibility compared to traditional approaches such as clean-based methods and MEM.","Functions Label":1}
{"Functions Text":"This approximation works well, even for evolved density fields, while deviations from Gaussianity can also be taken into account","Functions Label":1}
{"Functions Text":"and possible alternative explanations of the changing-look behaviour are","Functions Label":1}
{"Functions Text":"transient events, e.g. tidal disruption of a star by the central black hole (e.g.","Functions Label":1}
{"Functions Text":"Stripping and star formation consume the available gas and galaxies first appear as truncated disks","Functions Label":0}
{"Functions Text":"Optical ionised gas has been observed by","Functions Label":0}
{"Functions Text":"next to the black hole in a field of view1 of 5\u2032\u2032 \u00d7 3.5\u2032\u2032, but this emission is weak.","Functions Label":0}
{"Functions Text":"Initially the core size of a galaxy was determined by fitting the so-called \u2018Nuker-profile\u2019","Functions Label":0}
{"Functions Text":"to the surface brightness profile, a method that however depends sensitively on the radial fitting range and yields unreliable results when fit to surface brightness profiles with a large radial extent (e.g.","Functions Label":0}
{"Functions Text":"In these radiative envelopes, the transport of chemical elements on a macroscopic scale is ascribed to","Functions Label":0}
{"Functions Text":"or internal gravity waves (IGWs, e.g.,","Functions Label":0}
{"Functions Text":"The problem of accretion on to an SMBH has been studied via hydrodynamical simulations (e.g.","Functions Label":0}
{"Functions Text":"More recently, the emission-line OMEGA-OSIRIS survey provided similar results","Functions Label":0}
{"Functions Text":"Many simulations consider either an intermediate-mass BH (e.g.","Functions Label":0}
{"Functions Text":"Accordingly, it is informative to investigate the shape of the probability distribution of the matter density field and its evolution","Functions Label":3}
{"Functions Text":"However, it is worth noting that the gA-values obtained by the latter authors were deduced from the combination of branching ratio measurements with available experimental lifetimes for the 3d74p z5F, z5D, z5G levels","Functions Label":0}
{"Functions Text":"but also with estimated lifetimes for the z3G, z3F and z3D levels from the measurement of total intensity of all lines of each of these levels under the assumption of almost equal population.","Functions Label":0}
{"Functions Text":"In this scenario, depending on the misalignment angle, the outer disk image will show narrow shadow lanes (e.g.,","Functions Label":1}
{"Functions Text":"The reason that high-velocity features are interesting to investigate in connection with blueshifted Na\u2009i D features is that there are suggestions that the high-velocity Ca\u2009ii features may be at least partially due to ejecta\u2013CSM interaction (e.g.","Functions Label":3}
{"Functions Text":"Therefore, if a link between these quantities was identified, it would provide evidence that blueshifted Na\u2009i D features are due to CSM also rather than contamination.","Functions Label":3}
{"Functions Text":"CMEs have been observed to occur often having spatial and temporal relation with solar flares, eruptive prominences","Functions Label":0}
{"Functions Text":"In order to produce a steep gravitational potential at low |z|, there could be a breathing mode in the stellar disk","Functions Label":2}
{"Functions Text":"which is currently in its most compressed state.","Functions Label":2}
{"Functions Text":"Indeed, other studies confirm that abiotic buildup of ozone is possible (e.g.,","Functions Label":5}
{"Functions Text":"The input of dust from the inner disc triggers a streaming instability in the outer disc","Functions Label":2}
{"Functions Text":"lasting \u22480.1 Myr and concentrating pebbles and fractals sticking to pebbles into filaments where the comet nucleus collapses by gravity at speeds 1 m s\u22121 into a randomly packed","Functions Label":2}
{"Functions Text":"aggregate of cm-sized pebbles, with the fractals stored in the voids among the pebbles","Functions Label":2}
{"Functions Text":"In addition to morphological disturbances, galaxy mergers can trigger vigorous galactic outflows associated with feedback from the enhanced star formation (e.g.","Functions Label":0}
{"Functions Text":"Similar conclusions can be reached for the","Functions Label":5}
{"Functions Text":"sample where they adopt the same analysis as in Nestor et al. (2013).","Functions Label":5}
{"Functions Text":"For example, star count observations in the solar neighbourhood","Functions Label":0}
{"Functions Text":"followed by its characterization as the old \u03b1-enhanced population in the double sequence exhibited by the solar neighbourhood stars in the [\u03b1\/Fe] versus [Fe\/H] plane","Functions Label":0}
{"Functions Text":"Following Paper I, we have also adopted a 0.2 dex difference in metallicity between G2 and G1, and assumed 12 and 10 Gyrs for the ages of G1 and G2, respectively, with the same population ratio for the two RCs","Functions Label":2}
{"Functions Text":"Each deformable mirror uses 672 actuators that routinely correct 400 modes and provide Strehl ratios exceeding 80%, 95%, and 99% at 1.6\u00e2\u0080\u0089\u00ce\u00bcm, 3.8\u00e2\u0080\u0089\u00ce\u00bcm, and 10\u00e2\u0080\u0089\u00ce\u00bcm, respectively","Functions Label":0}
{"Functions Text":"In our second work","Functions Label":0}
{"Functions Text":"S19 hereafter), we used a complementary approach and looked for evidence of the lack of star formation as seen in the sub-millimetre regime to confirm the passive classification of the high-z candidates selected in GOODS-S.","Functions Label":0}
{"Functions Text":"At high nb the density profile inside the WS cell extends towards the edge of the cell, pointing out that the WS approximation may be close to its limits of validity","Functions Label":2}
{"Functions Text":"This matter replenishment may be channeled from within the cloud itself through molecular filaments","Functions Label":0}
{"Functions Text":"or toward hubs","Functions Label":0}
{"Functions Text":"Dry minor or intermediate mergers contribute little to the mass growth but promote substantial size growth (the accreted stars tend to be deposited mostly in the external regions), making spheroidal galaxies less compact and likely also less concentrated","Functions Label":0}
{"Functions Text":"Theoretical models have found that CO should be the dominant carbon-bearing molecule for hydrogen-dominated atmospheres above 1000 K","Functions Label":1}
{"Functions Text":"and CO has been detected at high resolution in hot Jupiter atmospheres (e.g.","Functions Label":1}
{"Functions Text":"In addition, technical development offers a new and barely explored perspective: a panchromatic, more detailed view of the universe through the use of narrowband filter systems, such as those from the J-PLUS and J-PAS surveys","Functions Label":0}
{"Functions Text":"The discovery of snail shells in the phase-space distribution of MW disk stars","Functions Label":0}
{"Functions Text":"has inspired debates about their origin:","Functions Label":0}
{"Functions Text":"Another model for their formation is by increasing their spin rates due to incident and remitted solar photons, known as the Yarkovsky\u2013O'Keefe\u2013Radzievskii\u2013Paddack (YORP) effect. The YORP effect on contact binary asteroids has been studied","Functions Label":0}
{"Functions Text":"A sample that contains 120 angular size measurements in intermediate-luminosity quasars from the very long baseline interferometry (VLBI) observations","Functions Label":0}
{"Functions Text":"has become an effective standard ruler, which have been extensively applied to test cosmological models","Functions Label":0}
{"Functions Text":"In the last decades, KAWs have received considerable attention due to their possible role in a normal mode description of turbulence. Indeed, theoretical studies (e.g.,","Functions Label":0}
{"Functions Text":"have shown that the turbulent cascade in magnetized plasma tends to develop mainly in directions perpendicular to B0.","Functions Label":0}
{"Functions Text":"The linear stability analysis of these idealized configurations","Functions Label":5}
{"Functions Text":"as well as the corresponding non-linear solutions (e.g.","Functions Label":5}
{"Functions Text":"confirms this view.","Functions Label":5}
{"Functions Text":"These properties can also be explained by the locations of resonances","Functions Label":1}
{"Functions Text":"Varying star densities can affect the results (e.g.","Functions Label":2}
{"Functions Text":"In this section we therefore explore the sensitivity of the shear measurement bias to various assumptions and simplifications made in the simulations.","Functions Label":2}
{"Functions Text":"Most DSFGs are discovered in wide-area observations using single-dish far-IR (FIR)\/millimeter instruments such as","Functions Label":0}
{"Functions Text":"the Herschel Space Observatory","Functions Label":0}
{"Functions Text":"In addition, we also included fgas estimates derived from the (median) stacked FIR spectral energy distributions of ETGs at","Functions Label":2}
{"Functions Text":"z\u2004\u223c\u20041.2, z\u2004\u223c\u20040.8, and z\u2004\u223c\u20040.5 (1394, 1536, and 563 galaxies, respectively;","Functions Label":2}
{"Functions Text":"hereafter M20","Functions Label":2}
{"Functions Text":"Increasing numbers of LAEs are being observed by surveys including narrow-band imaging (e.g.,","Functions Label":0}
{"Functions Text":"Recent work also finds that transient spiral structure","Functions Label":0}
{"Functions Text":"may lead to the formation of moving groups, as well as perturbations due to spiral arms in the MW","Functions Label":0}
{"Functions Text":"As a consequence, only large or massive planets are detected around the classical evolved stars","Functions Label":1}
{"Functions Text":"and references therein","Functions Label":1}
{"Functions Text":"The atmosphere above the Canary Islands, and especially the western islands Tenerife and La Palma, has been extensively characterized over the past 50 yr","Functions Label":0}
{"Functions Text":"(54 509) was the first asteroid for which the effect of YORP has been observed","Functions Label":0}
{"Functions Text":"There is indeed evidence for a potentially large population of heavily obscured, possibly Compton-thick AGN, among the WISE population (e.g.","Functions Label":0}
{"Functions Text":"Alternatively, the jet could be (ii) structured, with a fast and energetic inner core surrounded by a slower, less energetic layer\/sheath\/cocoon (first proposed for long GRBs","Functions Label":2}
{"Functions Text":"In particular, there are two intermittent quasi-periodicities for both NGC 5408 X-1 and M81 X-6, suggesting that the quasi-periods are changing or evolving. They resemble some Galactic X-ray binaries that show similar behaviour (e.g. Cyg X\u20132 and SMC X\u20131;","Functions Label":5}
{"Functions Text":"These characteristics resemble closest the behavior often observed in (luminous) red novae","Functions Label":0}
{"Functions Text":"a modern category of eruptive stars known from our and other galaxies (e.g.","Functions Label":0}
{"Functions Text":"J04221332+1934392 (a~7 AU,","Functions Label":2}
{"Functions Text":"chose the propagating direction averaged over the whole CME derived by the polarization ratio technique to correct the radial speed in the 2D maps, but the key information along the LOS is still lacking.","Functions Label":1}
{"Functions Text":"Some recent investigations showed that the mass-transfer process in the lobe-filling BH binaries is more stable than previously expected (e.g.,","Functions Label":2}
{"Functions Text":"; the maximal mass ratio of the donor star to the BH for stable mass transfer can reach as high as \u223c6. Hence only a few BH\u2013He XRBs with orbital periods of \u22721 day are produced in our calculations.","Functions Label":2}
{"Functions Text":"However, their emissivities can be computed based on specific energy absorbed in each grid cell and assuming that the emissivity is the function of the mean intensity of the radiation field, which approximates the spectral shape to the first order","Functions Label":2}
{"Functions Text":"In this context we promoted the ESO-VLT Multi-Instrument Kinematic Survey (hereafter the MIKiS survey;","Functions Label":3}
{"Functions Text":"a project specifically designed to characterize the kinematical properties of a sample of GGCs in different dynamical evolutionary stages from the radial velocities (RVs) of hundreds of individual stars distributed over the entire radial range of each stellar system.","Functions Label":3}
{"Functions Text":"observed a clear trend that AGNs, including the Seyfert composite galaxy NGC 1068, tend to show higher HCN\/HCO+ and\/or HCN\/CS than in SB galaxies as long as the observations were at high enough spatial resolutions to separate energetically discrete regions.","Functions Label":0}
{"Functions Text":"The luminosity in these FIR lines generally exhibits a deficit in the most FIR luminous galaxies compared to the trend expected from lower luminosity galaxies (e.g.","Functions Label":1}
{"Functions Text":"The concentration parameter is defined as the ratio of the surface brightness within 0.1 R500 to the surface brightness within R500","Functions Label":2}
{"Functions Text":"Note that there is some degeneracy between broken power-law break frequency","Functions Label":1}
{"Functions Text":"and extinction, which could lead to inference of grey dust for some instances","Functions Label":1}
{"Functions Text":"The reason is probably that the asteroids classified by Bus & Binzel (2002) as members of this taxonomic class include objects that belong to the old F-class, originally proposed by","Functions Label":1}
{"Functions Text":"and included in the Tholen taxonomy, due to its flat spectrum and low albedo;","Functions Label":1}
{"Functions Text":"Although it appears that small-scale flux ropes tend to contract or merge predominantly incompressibly in discussions of particle simulations (e.g.,","Functions Label":1}
{"Functions Text":"In fact, it is commonly believed that dynamical interactions in GCs facilitate the formation of close binary systems and exotic objects such as cataclysmic variables (CVs), low-mass X-ray binaries (LMXBs), millisecond pulsars (MSPs), and blue straggler stars (BSSs) (e.g.,","Functions Label":0}
{"Functions Text":"However, the measured solar disk emission flux was about a factor of seven higher than that predicted about this disk component by a \u201cnominal\u201d model","Functions Label":6}
{"Functions Text":"In the past, the limited observations showed that precursor activities of solar eruptions can come in various forms,","Functions Label":0}
{"Functions Text":"as well as nonthermal processes in microwave or hard X-ray wavelength","Functions Label":0}
{"Functions Text":"are most common ones.","Functions Label":0}
{"Functions Text":"Moreover, these disc-sources are confirmed to be binaries and show orbital periods between 100 and 2000 d","Functions Label":1}
{"Functions Text":"The literature on indirect evidence of the presence of planets is now becoming very rich, and nearby young stars surrounded by gas-rich disks are intensively studied for this purpose. In most cases, available data cannot fully eliminate alternative hypotheses, or the data have ambiguous interpretations (see, e.g.,","Functions Label":0}
{"Functions Text":"The hole-like structure may result from the expansion of a large-scale supershell produced by a supernova in the Per OB2 association that compresses the Taurus cloud from the far side","Functions Label":0}
{"Functions Text":"The most likely candidates for this task, given their reasonable agreement with observations and numerical simulations of cosmic-ray diffusion coefficients, are the quasilinear theory (QLT) of Jokipii (1966), the weakly nonlinear theory (WNLT) of Shalchi et al. (2004b), and the nonlinear guiding center theory (NLGC; or one of its variants; see, e.g.,","Functions Label":1}
{"Functions Text":"The global fits included","Functions Label":2}
{"Functions Text":"29 lines from","Functions Label":2}
{"Functions Text":"The majority of extremely metal-poor stars shows overabundances of carbon, [C\/Fe] > 0.7, and it appears that carbon-enhanced metal-poor (CEMP) stars split into two groups, with dramatically different carbon abundances (see, e.g.,","Functions Label":1}
{"Functions Text":"Based on this behaviour, it becomes possible to form hot Jupiters on retrograde orbits by combining the eccentric ZLK effect and tidal friction","Functions Label":0}
{"Functions Text":"Those blended emission lines can be easily detected at the position of the flare ribbon, including known and unknown emission lines, such as the C i line at 1354.29 \u212b, the Fe ii lines at 1353.02 \u212b, 1354.01 \u212b, and 1354.75 \u212b, the Si ii lines at 1352.64 \u212b and 1353.72 \u212b, and the unidentified lines at 1353.32 \u212b and 1353.39 \u212b (e.g.,","Functions Label":0}
{"Functions Text":"The timing of the coronal-hole-originated solar wind observation aligned well with the PSP orbit. PSP started passing through the leading edge of the high-speed stream, continued as the high-speed stream corotates over the spacecraft, and ended passing the trailing edge of the stream as seen in Figure 3, standing as a perfect classic CIR\/SIR event","Functions Label":3}
{"Functions Text":"Furthermore, in galactic nuclei with a high X-ray flux we would expect to see an increase in the dust temperature and infrared luminosity","Functions Label":2}
{"Functions Text":"Therefore in galactic nuclei, and in particular in AGNs, we expect a reduction in [C\u2009ii] emission relative to FIR\/IR emission depending on the relative contribution of different ISM components to the [C\u2009ii] luminosity.","Functions Label":2}
{"Functions Text":"The conversion factor depends on the physical conditions of the gas in the ISM (temperature, surface density, dynamics, and metallicity), as well as the star formation and associated feedback","Functions Label":1}
{"Functions Text":"For example, the enhanced close binary fraction of metal-poor solar-type stars substantially strengthens the conclusion that the shaping of PN morphologies is the result of binary interactions","Functions Label":5}
{"Functions Text":"These explanations can be very roughly divided into two main categories:","Functions Label":0}
{"Functions Text":"and mergers due to dynamical interactions (e.g.,","Functions Label":0}
{"Functions Text":"Adam optimization, compared to other gradient-based optimization, is very suitable for noisy and sparse gradients, and for simulated data that show very large scatter with respect to a given quantity of parameter","Functions Label":1}
{"Functions Text":"The Rayleigh\u2013Jeans dust continuum emission has been used to estimate dust and gas masses, assuming an average emissivity and dust temperature for the dominant cold dust component and a constant dust-to-gas ratio","Functions Label":0}
{"Functions Text":"In the regime of stability, the normal modes are undamped oscillation modes in absence of lateral streaming","Functions Label":2}
{"Functions Text":"If the particle is too small to be detected by the GDS system, it may be detected by the IS sensor only (IS particles): in this case the particle momentum is converted to the mass assuming the mean value of the velocities of the GDS+IS particles in the same momentum bin, or assuming the velocities predicted by tail models","Functions Label":2}
{"Functions Text":"if Ngds+is = 0 in that mass bin.","Functions Label":2}
{"Functions Text":"This method and its variants","Functions Label":0}
{"Functions Text":"have been used to estimate","Functions Label":0}
{"Functions Text":"as well as the power spectrum of H\u2009i distribution in nearby galaxies","Functions Label":0}
{"Functions Text":"These works propagate the uncertainties in each visibility estimate and combine that with the sample variance error in measuring the power spectrum to quote uncertainties in the power spectrum estimates.","Functions Label":0}
{"Functions Text":"Observational calibrations of the virial factor also tend to support this conclusion (e.g.,","Functions Label":5}
{"Functions Text":"according to diffusive shock acceleration (DSA; e.g.,","Functions Label":2}
{"Functions Text":"The radial variation of the stellar surface density of the high $\\mathrm{[ \\alpha \\mathrm{\/Fe]}}$ mono-age populations is found to have insignificant breaks, and they are better fit by a single exponential in this disc region. As these populations are the oldest, this may be a sign of the disc evolution washing out the density peak over time, or may point to a different formation scenario for high $\\mathrm{[ \\alpha \\mathrm{\/Fe]}}$ stars, where no density peak ever existed. These findings are in good agreement with earlier studies of MAPs","Functions Label":5}
{"Functions Text":"The origin of this large scatter is usually explained as a combination of the time variability of the SFR during the course of cloud evolution and intrinsic scatter of SFEs due to the diversity of GMC properties","Functions Label":0}
{"Functions Text":"To estimate the positions of the snow lines in observed disks, the temperature profile is often assumed to be a simple power law","Functions Label":2}
{"Functions Text":"which is broken if the disk has shadows on the disk surface","Functions Label":2}
{"Functions Text":"The last column in Table 1 reports the number of OB stars minus the \u201cdiffuse\u201d population estimated from their density in the Reference field (22.5 stars per square degree): as is immediately seen, the M-star statistics is much larger than the OB star statistics. This can hardly be considered surprising, if an ordinary IMF (e.g., that from","Functions Label":2}
{"Functions Text":"is assumed for the star-formation region.","Functions Label":2}
{"Functions Text":"The spectrum of He seems harder than that of H as indicated by many spectral studies, implying, e.g. time-dependent particle acceleration","Functions Label":1}
{"Functions Text":"or more efficient He injection in the shock acceleration process","Functions Label":1}
{"Functions Text":"The turning point of increased relative production of carbon from massive stars takes place at A(O) ~ 8.7 dex (see Fig. 2 of","Functions Label":2}
{"Functions Text":"which equals to [O\/H] ~ 0.0 dex.","Functions Label":2}
{"Functions Text":"This observed behaviour of [C\/O] is in contrast to the steady increase of [C\/O] up to [Fe\/H] ~ 0.3 dex found, for example, by Franchini et al. (2021).","Functions Label":6}
{"Functions Text":"In the simulations, hydrodynamics and neutrino transfer in general relativity are solved simultaneously","Functions Label":2}
{"Functions Text":"Alone, the energy released by jetted outflows appears to be on the same order as the energy needed to offset cooling (e.g.","Functions Label":2}
{"Functions Text":"therefore suggesting that AGN feedback is a good candidate for solving the cooling flow problem.","Functions Label":2}
{"Functions Text":"Other proposed solutions include","Functions Label":0}
{"Functions Text":"or through dynamical feedback driven by starbursts or active galactic nuclei","Functions Label":0}
{"Functions Text":"For example, GRBs that are highly offset from their hosts may have afterglows with much lower luminosities, making precise localization (and therefore host identification) difficult","Functions Label":1}
{"Functions Text":"The starting point is the \u201chybrid Vlasov\u2013Maxwell\u201d (HVM) code","Functions Label":2}
{"Functions Text":"which is already equipped with a fluid model in which electrons are described as an isotropic, isothermal fluid with finite inertia. The HVM code has recently been upgraded in order to implement a more sophisticated model for the electron fluid. This includes evolution equations for the anisotropic (gyrotropic) electron pressures, p\u2225,\u2006e and p\u22a5,\u2006e (where \u2225 and \u22a5 refer to the local magnetic-field direction, b\u2004=\u2004B\/|B|), and a Landau-fluid (LF) closure for the parallel transport of the gyrotropic electron thermal energy along field lines (i.e., parallel heat fluxes, q\u2225,\u2006e and q\u22a5,\u2006e).","Functions Label":0}
{"Functions Text":"We showed that molecular gas is falling in and slowly rotating with sub-Keplerian velocities down to radii of 500 au from the central star, where we measured a mass infall rate of 6 \u00d7 10\u22124 M\u2299 yr\u22121","Functions Label":0}
{"Functions Text":"their Fig. 5).","Functions Label":0}
{"Functions Text":"while short GRBs are consistent with null or negligible intrinsic spectral lag and are therefore an ideal tool to measure the LIV effect","Functions Label":3}
{"Functions Text":"also denoted $X^N_{2m}$ in","Functions Label":0}
{"Functions Text":"Similarly, stronger-than-expected 21-cm signals can arise if the cosmic radio background has contributions other than the CMB","Functions Label":3}
{"Functions Text":"The existence of MPs in Pal 13 supports the statement that this phenomenon is not unique in Galactic GCs formed in situ (e.g.,","Functions Label":5}
{"Functions Text":"More generally, in the case of strong shocks, the velocity u is identified as the velocity of the shock, as it is precisely the velocity jump at the shock discontinuity which drives the acceleration of the particles via the DSA mechanism (e.g.","Functions Label":0}
{"Functions Text":"After convolving our models with a 10\u2033 FWHM Gaussian kernel to simulate the data analysis presented in Lef\u00e8vre et al. (2014) and following the","Functions Label":2}
{"Functions Text":"prescription to take into account the part of the ISRF+CM light that can be transmitted through the cloud3, we compute the synthetic photometry for each pixel along a radial cut through our model clouds. The results are shown in Figs. 10a and b, which present the coreshine ratio as a function of the 3.6 \u03bcm intensity for the 21 starless cores of Lef\u00e8vre et al. (2014) and in Fig. 10c and d, which displays the near- to mid-IR ratio as a function of the coreshine ratio for the Taurus-Perseus and L183\/L134 regions.","Functions Label":2}
{"Functions Text":"Inspired by the new observations of this GW event at 3.3 yr after the initial merger","Functions Label":3}
{"Functions Text":"in this paper, we extend the synchrotron model presented in Fraija et al. (2021a), including the continuous energy injection from the central engine (either a spinning magnetized NS or BH remnant) into the blast wave through a numerical approach and analytic arguments.","Functions Label":3}
{"Functions Text":"We primarily used the OGLE catalogues for RR Lyrae stars","Functions Label":2}
{"Functions Text":"but we also used RR Lyrae stars by CTRS","Functions Label":2}
{"Functions Text":"These cross-matches returned a list of 88 578 known RR Lyrae stars in our sample of 140 784 stars.","Functions Label":2}
{"Functions Text":"This up-gradient transport into the jet can result from Rossby waves, coupled Rossby\u2013Kelvin waves, mixed Rossby\u2013gravity waves, wave\u2013jet resonance, barotropic instability, or baroclinic instability","Functions Label":0}
{"Functions Text":"This property enables the creation of steep phase ramps that efficiently diffract light into a single order without scattering","Functions Label":2}
{"Functions Text":"The problem of the balance between driving and decay for magnetized turbulence is most acute in molecular clouds. Since these have linewidths indicating the presence of supersonic flow, the fast dissipation of turbulence found by these simulations necessitates a mechanism to reinject the energy equally quickly. A number of candidates have been proposed, including","Functions Label":0}
{"Functions Text":"or protostellar outflows","Functions Label":0}
{"Functions Text":"Despite this only six radio pulsars have been discovered within half a degree of Sgr A*","Functions Label":0}
{"Functions Text":"For MR Del, we revised the absolute parameters using its full light curve and the published radial velocities, which are similar to those published previously","Functions Label":5}
{"Functions Text":"Many near-infrared observations have revealed the same feature on the blue wing part of the CO absorption feature","Functions Label":5}
{"Functions Text":"which was suggested as an absorption feature of XCN ice.","Functions Label":0}
{"Functions Text":"According to","Functions Label":2}
{"Functions Text":", the Poisson noise is 200 e\u2212 for a typical detector with a gain of a few e\u2212 ADU\u22121 and the flat illumination level is of 20 000 ADU pixel\u22121 = 40 000 e\u2212 pixel\u22121. Thus, a typical photometric aperture with a radius of 3 pixels contributes \u223c1 mmag photon noise.","Functions Label":2}
{"Functions Text":"This complex environment is multiphase and has been observed in numerous surveys","Functions Label":0}
{"Functions Text":"at low redshift.","Functions Label":0}
{"Functions Text":"Hence, to reduce the number of 24 free parameters and the values they can take, we use prior knowledge about the pulsation spectrum of the star that was acquired during","Functions Label":2}
{"Functions Text":"For a collision at a velocity \u223c108\u2009cm\u2009s\u22121, which is a typical velocity scale for young SNR shocks, the cross-section is \u223c10\u221213\u2009cm2, giving a reaction rate \u223c10\u22125\u2009cm3 s\u22121 (e.g.","Functions Label":2}
{"Functions Text":"Thus, if the density is \u223c106\u2009cm\u22123, the collisional depopulation becomes important.","Functions Label":2}
{"Functions Text":"In OMC-1, the low- and high-velocity outflows from BN\/KL plunge into the ambient molecular cloud","Functions Label":2}
{"Functions Text":"producing hot (from Tk \u2243 200\u20132000 K) and dense (up to n(H2) \u2243 106\u2013107 cm\u22123) post-shocked gas in H2 Peaks 1 and 2","Functions Label":2}
{"Functions Text":"Theoretical work suggests major mergers can provide the torque to displace such an overwhelming fraction of the angular momentum of the gas, allowing for the highest accretion rates on to the central black hole whilst transforming the galaxy morphology","Functions Label":0}
{"Functions Text":"As already noted, the companions are generally significantly fainter than the exploding star, although this is frequently not the case for stripped SN progenitors \u2013 for Type Ibc SNe, it should not be surprising to find that the binary companion is more visually luminous than the SN progenitor. This point is of considerable importance for the one candidate Type Ib progenitor iPTF13bvn","Functions Label":0}
{"Functions Text":"In order to estimate a temperature for the dust, we have fitted a modified blackbody to the available photometry at wavelengths longer than 10 \u00b5m (AKARI, WISE, IRAS, Herschel)3 and the new ALMA photometry using the emcee Affine Invariant Markov chain Monte Carlo Ensemble sampler implementation","Functions Label":2}
{"Functions Text":"Graham (2001) analysed a sample of 86 face-on disc-dominated galaxies previously selected by","Functions Label":2}
{"Functions Text":"hus, both survival and replenishment of galaxies should be expected over the time, and two important factors come into play: (i) the accretion rate of galaxies; and (ii) the orbital dependence of galaxy properties (e.g.","Functions Label":2}
{"Functions Text":"The disk of an AGN provides a natural environment for stars and compact objects to accrete materials and to migrate within it (e.g.,","Functions Label":0}
{"Functions Text":"Recently,","Functions Label":5}
{"Functions Text":"claimed that the mass of XTE J1859+226 is perhaps in between 6.58 and 8.84\u2009M\u2299 which is similar to the prediction of Shaposhnikov & Titarchuk (2009)","Functions Label":5}
{"Functions Text":"although the lower mass limit is estimated as 5.4\u2009M\u2299 by Corral-Santana et al. (2011).","Functions Label":6}
{"Functions Text":"Also shown in Fig. 12 (with a black [gray] solid line for the low [high] dust content) is the proposed analytic solution for fesc by","Functions Label":2}
{"Functions Text":"(18)\\begin{equation} f_{\\rm esc}^{\\rm HO06} = 1\/{\\rm cosh}(\\!\\sqrt{2 N_{\\cl}\\epsilon}), \\label{eq:fescHO06} \\end{equation}fescHO06=1\/cosh(2Ncl\u03f5),where for Ncl we used Eq. (8)(with (a1,b1) = (3\/2, 2) as found in Sect. 4.1) and for the clump albedo (i.e., the fraction of incoming photons that are reflected) \u03f5, we adopted a value of c1(1\u2212e\u2212 \u03c4d,cl) with c1 = 1.6 [c1 = 0.06] to match the NHI,cl = 1022 cm-2 data points for \u03c4d,cl = 10-4 [\u03c4d,cl = 1].","Functions Label":2}
{"Functions Text":"Early studies concentrated on measurements of higher order correlation hierarchy in the angular space due to small survey size","Functions Label":0}
{"Functions Text":"On the other hand, the Minkowski functionals (MFs) are extremely useful tools in quantitatively describing the morphology because, in principle, they contain information on all the higher-order moments.","Functions Label":0}
{"Functions Text":"Since then they have been extensively employed to study the morphology of the large-scale structure of the universe and the cosmic web","Functions Label":0}
{"Functions Text":"Next, we adopt the position of 3FGL J1640.4-4634c provisionally provided by the 3FGL catalog","Functions Label":2}
{"Functions Text":"This is illustrated in Fig. 5, where thick blue and red data points show mild high-energy excesses of the electron spectra derived by","Functions Label":2}
{"Functions Text":"Kerszberg et al. (2017), Kerszberg (2017) over broken power-law models derived from the fits to lower energy data.","Functions Label":2}
{"Functions Text":"Other global 21-cm experiments, including the Large-Aperture Experiment to Detect the Dark Ages","Functions Label":0}
{"Functions Text":"provide upper limits on the signal from Cosmic Dawn and the Epoch of Reionization (EoR), ruling out some extreme astrophysical scenarios.","Functions Label":0}
{"Functions Text":"It was soon realized that these frequencies are probably related to oscillations of the neutron star, and several groups tried to identify them as","Functions Label":0}
{"Functions Text":"Alfv\u00e9n oscillations","Functions Label":0}
{"Functions Text":"The data were manually calibrated by the EA ARC node using the Common Astronomy Software Applications (CASA) of the version 5.1.1","Functions Label":2}
{"Functions Text":"Recent measurements of the LMC abundances based on the X-ray spectral analysis of SNRs","Functions Label":6}
{"Functions Text":"suggest \u223c50% lower LMC abundance values for O, Ne, Mg, and Fe than the previously estimated values","Functions Label":6}
{"Functions Text":"Our derived shock parameters are consistent (within statistical uncertainties), assuming either set of these LMC abundances in tbnew.","Functions Label":6}
{"Functions Text":"The B\/T ratio is an important indicator of galaxy structure and is well correlated with several other physical quantities of interest in studies of galaxy evolution, such as","Functions Label":0}
{"Functions Text":"stellar mass, and star formation rate","Functions Label":0}
{"Functions Text":"In this scenario SMBHs have to begin growing even earlier than the very first stars are assumed to have appeared (see discussion in","Functions Label":2}
{"Functions Text":"Studies based on both observations and simulations have shown that galaxy collisions and mergers can dramatically affect the galaxies undergoing the interaction, by, e.g.","Functions Label":0}
{"Functions Text":"disrupting morphologies (e.g.","Functions Label":0}
{"Functions Text":"A whole host of ions, atoms, and molecules have been detected through a variety of, often complementary, techniques,","Functions Label":0}
{"Functions Text":"and high resolution spectroscopic techniques (e.g.","Functions Label":0}
{"Functions Text":"To date, several candidate jet\u2013ISM interaction sites have been identified;","Functions Label":0}
{"Functions Text":"XTE J1550\u2013564","Functions Label":0}
{"Functions Text":"From these past works, it is clear that finding and confirming interaction sites can be incredibly difficult and often observationally expensive (e.g. requiring deep, wide-field radio continuum observations).","Functions Label":0}
{"Functions Text":"However, the depth of the feature is \u0394T21 \u223c 0.5 K ($99{{\\ \\rm per\\ cent}}$ confidence level), which is two to three times stronger and considerably wider (\u0394\u03bd \u223c 19 MHz) than that predicted by the most optimistic astrophysical models (e.g.","Functions Label":6}
{"Functions Text":"V\u00e1zquez-Semadeni, Gonz\u00e1lez-Samaniego & Col\u00edn (2017) have recently shown that the simulations of Col\u00edn et al. (2013) in fact produce stellar age histograms highly resemblant of the observed ones","Functions Label":5}
{"Functions Text":"Moreover, in massive galaxies, the role of AGNs in influencing galaxy evolution and quenching SF is supported by several observations","Functions Label":0}
{"Functions Text":"On the other side, we have the tidal (gravitational) mechanisms occurring","Functions Label":0}
{"Functions Text":"or among neighbour galaxies","Functions Label":0}
{"Functions Text":"In fact, homologous jets, continuing for hours at a time, have been commonly observed (e.g.,","Functions Label":0}
{"Functions Text":"More evolved disks do not show a degree of linear polarization larger than 0.5%","Functions Label":0}
{"Functions Text":"and a similar phenomenon has also been observed in the case of","Functions Label":5}
{"Functions Text":"CB 3","Functions Label":5}
{"Functions Text":"Since cool core clusters have short radiative cooling time-scales on the order of 108 yr in their centres (e.g.","Functions Label":2}
{"Functions Text":"starbursts are expected to be common at the centre of such clusters.","Functions Label":2}
{"Functions Text":"Comparison of 1D marginal posterior distributions over the parameters S8 \u2261 \u03c38(\u03a9m\/0.3)0.5, \u03c38 and \u03a9m, from DES Y3 data as well as other experiments, and consistency tests for this work (in blue).","Functions Label":1}
{"Functions Text":"Constraints from other weak lensing surveys, namely HSC Y1","Functions Label":1}
{"Functions Text":"are shown in grey","Functions Label":1}
{"Functions Text":"They have shown that the ionised phase appears to be an ideal tracer of stripped gas in dense regions: approximately 50% of late-type galaxies show extended (~50 kpc) tails of ionised gas with surface brightness \u03a3(H\u03b1) of approximately a few 10\u221218 erg s\u22121 cm\u22122 arcsec\u22122","Functions Label":0}
{"Functions Text":"while only a handful of galaxies have extended cold or hot gaseous tails","Functions Label":0}
{"Functions Text":"Since relxillDCp considers the thermal Comptonization model nthComp","Functions Label":2}
{"Functions Text":"as the irradiating (primary) continuum, we replaced the zpowerlw continuum with nthComp.","Functions Label":2}
{"Functions Text":"For this paper, \u03ba is taken to be equal to 1, in agreement with numerical simulations of decaying turbulence","Functions Label":2}
{"Functions Text":"Observationally, the bulk Lorentz factor of the jet in the low\/hard state of X-ray binaries can be restricted in a relatively narrow range and the velocity of the jet is mildly relativistic, i.e. \u0393jet \u2272 2. More strictly, the bulk Lorentz factor is restricted to be as \u0393jet \u2272 1.67","Functions Label":0}
{"Functions Text":"and \u0393jet \u2272 1.2","Functions Label":0}
{"Functions Text":"A similar effect is also found in measurements of the propagation velocity of travelling waves","Functions Label":0}
{"Functions Text":"In particular, it has been demonstrated repeatedly that the power spectral density (PSD) of blazar light curves is, in general, of a power-law form","Functions Label":0}
{"Functions Text":"For solar-type stars k2 \u223c 0.035","Functions Label":2}
{"Functions Text":"This kind of weak anti-correlation between the activity cycle and the meridional flow has been found in solar observations","Functions Label":5}
{"Functions Text":"The reasons for studying the dynamic properties of small-scale magnetic fields in the quiet photosphere are manifold. Firstly, magnetic fields provide an opportunity to probe","Functions Label":3}
{"Functions Text":"and energy propagation to the upper atmospheric layers (see, e.g.","Functions Label":3}
{"Functions Text":"that cannot be addressed otherwise from an observational point of view.","Functions Label":3}
{"Functions Text":"In particular, the analysis of CMB data, most notably from the Wilkinson Microwave Anisotropy Probe","Functions Label":0}
{"Functions Text":"and Planck","Functions Label":0}
{"Functions Text":"experiments, has not yet provided conclusive evidence for the hypothesis of Cosmological Isotropy","Functions Label":0}
{"Functions Text":"Several works have pointed out that AGN activity coincides with a recent starburst, with the AGN having significant accretion events at least \u223c200\u2009Myr after the starburst has occurred","Functions Label":0}
{"Functions Text":"giving the neutral material time to propagate out to the impact parameters probed by COS-AGN","Functions Label":0}
{"Functions Text":"Stars with brighter K-band absolute magnitudes tend to have higher [N\/Fe] and lower [C\/Fe] (middle and bottom panels of Figure 8), which is consistent with extra-mixing theory and observation","Functions Label":5}
{"Functions Text":"Higher angular resolution observations of the (3,\u20093) NH3\u2009absorption line (0\\hbox{$\\farcs$}.\u030b3 beamsize) showed signatures of rotation within 2000 AU based on a position-velocity (pv) diagram","Functions Label":0}
{"Functions Text":"Here, for instance, the presence of a magnetic field leads to the formation of early outflows. These reduce the radiation pressure, which allows the protostar mass to grow further","Functions Label":0}
{"Functions Text":"Here we adopted an intermediate value between the solar and supersolar G\/Ds used in","Functions Label":2}
{"Functions Text":"and we increased the error bars of these points to include both the solar and supersolar confidence estimates.","Functions Label":2}
{"Functions Text":"Although hotspots located at the foot of accretion streams can affect RV measurements mimicking the signal of an orbiting body","Functions Label":2}
{"Functions Text":"Johns-Krull et al. (2016) specifically looked for these signals and found no evidence that hotspots produced the RV signals seen in photospheric absorption lines.","Functions Label":2}
{"Functions Text":"As for the density profile, simulations of the FHSC stage show a flat inner region, corresponding to the FHSC structure and extending up to \u223c10 au","Functions Label":1}
{"Functions Text":"Some of the recent observations and studies","Functions Label":0}
{"Functions Text":"indicate that the CGM can account for a good fraction of the baryons in these galaxies.","Functions Label":0}
{"Functions Text":"From power spectrum analysis, significant periodicities ranging from about 1.4 to 10 yr were found in PSR B1540\u221206, PSR B1642\u221203, PSR B1818\u221204, PSR B1826\u221217, PSR B1828\u221211, and PSR B2148+63","Functions Label":2}
{"Functions Text":"In all cases, we consider a solar metallicity for the main SF episode and, according to the results of","Functions Label":2}
{"Functions Text":"a subsolar metallicity (Z = 0.004) for the later one.","Functions Label":2}
{"Functions Text":"If the carbene is formed in its first excited singlet state (a1A1), the insertion is barrierless","Functions Label":2}
{"Functions Text":"Using these indicators, a number of studies have found that the color or SFR transition of galaxies is associated with the consumption of their gas content (e.g.,","Functions Label":0}
{"Functions Text":"As shown by comparisons to dark moon observations only particle events are recorded in the stow position","Functions Label":0}
{"Functions Text":"The cool molecular envelope exhibits ice and dust absorption bands","Functions Label":0}
{"Functions Text":"Sagittarius A* (Sgr A*) is inferred to be accreting at a rate of 10\u22123 to $10^{-2}\\ \\dot{M}_{\\rm B}$ (e.g.","Functions Label":2}
{"Functions Text":"In more detail, the existence of a \u201cblue\u201d and possibly also a \u201cpurple\u201d component in the AT 2017gfo emission further indicated that the merger product of the GW170817 event is very likely to be a hypermassive NS, which lasted for at least a few hundred milliseconds, as an immediately formed black hole can only be associated with a \u201cred\u201d kilonova1","Functions Label":0}
{"Functions Text":"The origin of this correlation is puzzling, as stellar clustering is expected to affect mostly the outer part of planetary systems in very dense environments","Functions Label":1}
{"Functions Text":"which is one of the commonly used methods of mass determination in galaxy clusters (see e.g.","Functions Label":0}
{"Functions Text":"This new estimate is consistent with the ratio expected between the aGg\u2032 and gGg\u2032 conformers under thermal equilibrium conditions at 300\u2009K, the excitation temperature of glycolaldehyde derived in IRAS 16293","Functions Label":5}
{"Functions Text":"see equations 3 in","Functions Label":0}
{"Functions Text":"these are based on the vector eccentricity and the vector inclination.","Functions Label":0}
{"Functions Text":"The initial condition is the Orszag\u2013Tang vortex (OTV) (e.g.,","Functions Label":2}
{"Functions Text":"also, \u2018convergence\u2019 is meant in the sense that the Lp norm of the difference between the actual solution and the ZKBP function tends to zero as t\u2004\u2192\u2004\u221e faster than a negative power of the time with an exponent which is a function of n, m, and p (e.g. \u22121\/3 for n\u2004=\u20042 and m\u2004=\u20043 in the L2 norm; see details in the book by","Functions Label":0}
{"Functions Text":"The CO photodesorption yield reaches its highest value when this ice is deposited at low temperatures (down to 7\u2009K, the lowest temperature studied experimentally) and decreases gradually at higher deposition temperatures","Functions Label":0}
{"Functions Text":"The explanation for this phenomenon motivated further research.","Functions Label":3}
{"Functions Text":"On the other hand, if the torus is made of a collection of clouds, each cloud is heated to \u223c300 K to emit MIR emission while absorbing the background light when the foreground cloud is cooler than the one behind. The radiation transfer effect among the clouds significantly reduces the net silicate absorption even when the torus is seen edge-on","Functions Label":6}
{"Functions Text":"The first three LoTSS Deep Fields are the European Large-Area ISO Survey-North 1 (ELAIS-N1","Functions Label":0}
{"Functions Text":"Lockman Hole, and Bo\u00f6tes","Functions Label":0}
{"Functions Text":"these were chosen to have extensive multi-wavelength coverage from past and ongoing deep, wide-area surveys sampling the X-ray","Functions Label":0}
{"Functions Text":"and to infrared (IR; e.g.","Functions Label":0}
{"Functions Text":"wavelengths","Functions Label":0}
{"Functions Text":"Several observations have shown that properties of galaxies such as star formation, gas content, and colour are affected by the cluster environment at large clustercentric distances (e.g.","Functions Label":0}
{"Functions Text":"This proved to be a useful distinction and an excellent predictor of several trends","Functions Label":1}
{"Functions Text":"but recent results, including our present and previous analysis","Functions Label":1}
{"Functions Text":"show that the demarcation between starburst and main-sequence galaxies is more blurred that we previously considered.","Functions Label":1}
{"Functions Text":"Metallicity gradients in units of dex kpc-1 determine tight correlations with the global properties of galaxies such as the stellar mass or the size, which are erased when normalised by a characteristics radius such as the half-mass radius (e.g.","Functions Label":0}
{"Functions Text":"For example, it was observed that a single emission line at around 14 keV can fit two features around 10 and 20 keV for","Functions Label":2}
{"Functions Text":"Her X-1","Functions Label":2}
{"Functions Text":"In the case of GRO J2058+42, an introduction of a single Gaussian emission line in this range of energies could not appropriately fit the spectrum.","Functions Label":1}
{"Functions Text":"In this context \u2018scale-free\u2019 cosmological models, in which both the expansion law and the power spectrum characterizing the initial fluctuations are simple power laws, have the advantage of relative simplicity, and they have for this reason been studied quite extensively in the literature (see e.g.","Functions Label":0}
{"Functions Text":"Extreme geomagnetic storms can cause widespread interference and damage to technological systems","Functions Label":0}
{"Functions Text":"and then lead to significant economic loss (e.g.,","Functions Label":0}
{"Functions Text":"Our upper limit on the Fopt\/Fx for the PSR J0633+0632 PWN is above the values obtained for the other PWNe, which are typically \u223c 0.02\u20130.04, apart from the Crab PWN which has an Fopt\/Fx \u223c 2","Functions Label":6}
{"Functions Text":"This is also the case for the PSR J1124\u22125916 PWN","Functions Label":1}
{"Functions Text":"Also the dependence of the IMF on the SFR is nowadays observationally well established","Functions Label":0}
{"Functions Text":"but see also a noticeable exception in","Functions Label":6}
{"Functions Text":"An interesting implication is that, if BHs settle into the disk, they interact dynamically and form BH\u2013BH binaries efficiently, and frequent dynamical interactions and gas effects drive the BHs to merger, producing gravitational waves (GWs) detectable by LIGO, VIRGO, and KAGRA","Functions Label":0}
{"Functions Text":"The fact that simulations usually produce anti-solar differential rotation for the solar rotation rate could indicate that the Sun is in a transitional regime (e.g.,","Functions Label":1}
{"Functions Text":"or could also mean that simulations still cannot fully capture the true rotational influence on turbulent convection in the Sun.","Functions Label":1}
{"Functions Text":"But there is no well-resolved system that matches the theoretical expectations (see, e.g.,","Functions Label":3}
{"Functions Text":"Nevertheless, it still faces numerous challenges on galaxy scales. Among these, the most important ones are","Functions Label":3}
{"Functions Text":"for dwarf galaxies, the tightness of the baryonic Tully\u2013Fisher relation","Functions Label":3}
{"Functions Text":"The comparison sample is compiled from the literature up to z \u223c 3","Functions Label":2}
{"Functions Text":"There have been searches for a periodic signal in the prompt emission of GRBs with a number of instruments with no success, for example:","Functions Label":0}
{"Functions Text":"and Burst Alert Telescope (BAT) GRBs","Functions Label":0}
{"Functions Text":"At certain geocentric velocities the cometary [O i] 6300 \u212b emission sits on top of a strong telluric absorption, and at high airmass inaccurate removal of this feature can result in a decrease in the measured flux and therefore production rate. This was observed for C\/2012 S1 (ISON)","Functions Label":1}
{"Functions Text":"Several observations have shown that properties of galaxies such as star formation, gas content, and colour are affected by the cluster environment at large clustercentric distances (e.g.","Functions Label":3}
{"Functions Text":"Here, Ai,j are the entropic functions of the particles","Functions Label":2}
{"Functions Text":"A cold-phase of the CGM at \u2248104 K has also been observed, but its origins are less clear","Functions Label":3}
{"Functions Text":"It was the first source identified as a hot corino","Functions Label":0}
{"Functions Text":"based on the detection of Complex Organic Molecules (COMs) in the source, which was later supported by follow-up studies","Functions Label":0}
{"Functions Text":"Turbulence on scales less than the scale height of the warm\u2013cold ISM likely originates primarily due to the feedback from young stars","Functions Label":0}
{"Functions Text":"To model mechanical feedback, we adopt a phenomenological model proposed by Ostriker et al. (2010), while radiative feedback is treated by adopting the standard and slim disc model","Functions Label":2}
{"Functions Text":"As reported in","Functions Label":0}
{"Functions Text":", the intensity of H2O in the coma dominated the overall signal, with maxima in the H2O signal every ~6 h, about twice during a rotation.","Functions Label":0}
{"Functions Text":"Interestingly, however, CO2 and CO displayed a separate additional maximum when the H2O signal was near its minimum. This independent maximum in CO2 and CO only occurred at negative observing latitudes that are associated with a particular \u201cview\u201d of Rosetta at 67P, with the larger lobe blocking out the neck and head.","Functions Label":3}
{"Functions Text":"According to the time-lag analysis,","Functions Label":0}
{"Functions Text":"found that the disc thermal emission (\u223c0.3\u20130.7 keV, soft band) leads the power-law variations (\u223c0.7\u20131.5 keV, hard band) on long timescales (> 1s).","Functions Label":0}
{"Functions Text":"The propeller regime has been investigated both analytically","Functions Label":0}
{"Functions Text":"In this paper, we adopt Mpi = 20 M\u2295 and Mpf = 10 M\u2295 nominally (close to the standard model adopted in","Functions Label":5}
{"Functions Text":"Negative radial metallicity gradients have been widely observed in the low-redshift galaxy population (e.g.","Functions Label":0}
{"Functions Text":"Gravitational interactions in the perturbed disc drive turbulence causing the disc to self-regulate in a marginally stable state with Q \u2272 1","Functions Label":0}
{"Functions Text":"that can last for more than a Gyr so long as the accretion is not interrupted.","Functions Label":0}
{"Functions Text":"Apart from cosmological simulations, dedicated zoom-in simulations","Functions Label":0}
{"Functions Text":"have revealed that dry mergers that dominate the passive evolution of ETGs below z \u2248 2 could make the total density profile shallower than isothermal","Functions Label":0}
{"Functions Text":"We calculate the GW amplitudes A(f) of NS\u2013WD binaries using the phenomenological (PhenomA) waveform model in the Fourier domain","Functions Label":2}
{"Functions Text":"According to the review of the leptonic model (see, e.g.,","Functions Label":2}
{"Functions Text":"the electrons injected into PWNe are accelerated by the pulsar magnetosphere and the termination shock. Therefore, the relativistic particles injected into the PWNe are also assumed as two different power-law components from the pulsar magnetosphere and shock acceleration, respectively.","Functions Label":2}
{"Functions Text":"and a comparison with the other EoSs of the BSk family","Functions Label":7}
{"Functions Text":"and the RMF family","Functions Label":7}
{"Functions Text":"shall be left for future study.","Functions Label":7}
{"Functions Text":"Intermittency is related to the scale-dependent shape of the probability distribution function of the increments \u0394\u03d5","Functions Label":0}
{"Functions Text":"This, additionally, implies the existence of nonvanishing odd moments.","Functions Label":0}
{"Functions Text":"whereas radio relics are apparently associated with localized, post-merger shock-fronts","Functions Label":0}
{"Functions Text":"and the Coma cluster","Functions Label":0}
{"Functions Text":"an apparent link is seen between radio galaxies and radio relics.","Functions Label":0}
{"Functions Text":"Although","Functions Label":6}
{"Functions Text":"concluded that WR 130 could have alone created the observed structure, it is important to note that they did not take into account the molecular mass present in the shell, which considerably increases the kinetic shell energy.","Functions Label":6}
{"Functions Text":"Linking purely gravitational interactions to symmetries such as defined in equation (3) suggests deeper physics and constitutes a motivation for viewing MOND as much more than a mere phenomenological description of galactic dynamics","Functions Label":1}
{"Functions Text":"Although period-folding improves performance","Functions Label":1}
{"Functions Text":"Becker et al. (2020)\u2019s time-space RNN does not require the period to be calculated, and is thus less computationally expensive in terms of preprocessing.","Functions Label":1}
{"Functions Text":"This representative value for our AGN is in line but not as low as previous work targeting extremely powerful sources (e.g., Mgas,\u2006mol\/M*\u2004\u20040.05 in","Functions Label":1}
{"Functions Text":"As a result, when the power spectrum is observed as a function of (k\u2225, k\u22a5), the foreground emission remains concentrated near the low k\u2225, inside the \u2018wedge\u2019","Functions Label":2}
{"Functions Text":"Another problem is the use of time-dependent mixing-length formalisms","Functions Label":0}
{"Functions Text":"to account for modal surface effects (e.g.,","Functions Label":0}
{"Functions Text":"Strong gravitational lensing systems are a powerful tool for cosmology. They have been used to study how dark matter is distributed in galaxies and clusters","Functions Label":0}
{"Functions Text":"and are uniquely suited to probe the low end of the dark matter mass function and test the prediction of the cold dark matter (CDM) model beyond the local universe (e.g.,","Functions Label":0}
{"Functions Text":"A way to possibly explain this polarization change is to view it as a mode-coupling phenomenon, the process by which the rays reverse their original sense of polarization while passing through a quasi-transverse field region along the line of sight from the radiation source to the observer, depending on the degree of mode coupling there","Functions Label":1}
{"Functions Text":"In addition, we argue that the Galaxy is the azimuthally asymmetric spiral system (cf.","Functions Label":6}
{"Functions Text":"The charge transfer inefficiency (CTE) correction for the ACS data was performed by the pipeline, whereas CTE losses in WFC3\/UVIS","Functions Label":2}
{"Functions Text":"were treated manually using the tools supplied by STScI.","Functions Label":2}
{"Functions Text":"t is worth pointing out that clumpy galaxy fractions are highly sensitive to methodology and clump definition and vary widely in the literature (e.g.,","Functions Label":1}
{"Functions Text":"so we should not expect complete agreement.","Functions Label":1}
{"Functions Text":"Here, we use the new formalism presented in","Functions Label":2}
{"Functions Text":"who showed that the Newtonian potential is exactly reproduced by using an intermediate scalar function \u210b, namely \\hbox{$\\Phi = \\partial_{xy}^2 {\\cal H}$}\u03a6=\u2202xy2\u210b. In 3D, this hyperpotential is written as (12)\\begin{equation} {\\cal H}(x,y,z) = -G \\iiint_{\\Omega'}{\\rho(x',y',z')} \\kappa^{xy}(X,Y,Z){\\rm d}x'{\\rm d}y'{\\rm d}z' , \\end{equation}\u210b(x,y,z)=\u2212G$\u03a9\u2032\u03c1(x\u2032,y\u2032,z\u2032)\u03baxy(X,Y,Z)dx\u2032dy\u2032dz\u2032,with X = x\u2212x\u2032, Y = y\u2212y\u2032 and Z = z\u2212z\u2032.","Functions Label":2}
{"Functions Text":"However, the repulsive nature of lensing by a large and deep underdense region (i.e., cosmic voids) as described by the rigorously derived but simply implemented embedded lens formalism did not appear until","Functions Label":0}
{"Functions Text":"Indeed, other studies confirm that abiotic buildup of ozone is possible","Functions Label":0}
{"Functions Text":"however, detectable levels are unlikely if liquid water is abundant, as e.g. rainout of oxidized species would keep atmospheric O2 and O3 low","Functions Label":0}
{"Functions Text":", unless the CO2 concentration is high and both H2 and CH4 emissions are low","Functions Label":0}
{"Functions Text":"For instance,","Functions Label":0}
{"Functions Text":"and RFs are associated with energy conversion from electromagnetic fields to particles","Functions Label":0}
{"Functions Text":"This accounts for the bias due to contaminating galaxies that are physically associated with the centrals but are not satellites (i.e., the 2-halo term of the correlation function; see","Functions Label":2}
{"Functions Text":"Even modest changes in direction (e.g.,","Functions Label":0}
{"Functions Text":"have long been recognized as one way to produce significant changes in the flux and polarization","Functions Label":0}
{"Functions Text":"Vacuum birefringence dramatically increases the linear polarization of the observed radiation, from a level of a few \u2009per\u2009cent up to even \u223c100\u2009per\u2009cent, depending on the viewing geometry and the surface emission mechanism","Functions Label":0}
{"Functions Text":"In addition,","Functions Label":0}
{"Functions Text":"recalled several issues that should be taken into account when considering the Si\u2009iv\/O\u2009iv density diagnostic. The main ones were: (1) O\u2009iv and Si\u2009iv ions are formed at quite different temperatures in equilibrium and hence a change in the O\u2009iv\/Si\u2009iv ratio could imply a change in the temperature rather than in the plasma density (2) the chemical abundances of O and Si are not known with any great accuracy and could be varying during the observed events (3) density effects on the ion populations could increase the Si\u2009iv\/O\u2009iv relative intensities by a factor of roughly three to four.","Functions Label":0}
{"Functions Text":"So-called Type-C low-frequency QPOs","Functions Label":0}
{"Functions Text":"are believed to originate from the inner accretion flow\/corona that is associated with the Comptonized power-law component of the X-ray spectrum, as this component shows a much larger variability amplitude than the blackbody disc component","Functions Label":0}
{"Functions Text":"This latter assumption does not perfectly reflect spacecraft observations of the same","Functions Label":1}
{"Functions Text":", but leads to relatively simple, tractable expressions for the parallel and perpendicular MFPs.","Functions Label":1}
{"Functions Text":"Non-chondrite meteorites (including achondrites) also originate from differentiated asteroids and planets, e.g. from Moon, Mars, and Vesta, and the angrite and ureilite parent bodies","Functions Label":0}
{"Functions Text":"This result strengthens the notion that metallicity may not play an important role in deciding theresulting SN type, in agreement with other works based on SN environments","Functions Label":5}
{"Functions Text":"Here, $\\widetilde{v}_r$ and $\\widetilde{v}_\\varphi$ are the amplitudes of the radial and tangential wave motions that depend weakly on the Galactocentric distance r, and \u03d5 is the phase of the wave","Functions Label":2}
{"Functions Text":", annexure B therein","Functions Label":2}
{"Functions Text":"Indeed, Terzan 5 hosts the largest population of MSPs among all Galactic GCs","Functions Label":3}
{"Functions Text":"Still, in four dimensions, hairy BHs have been described in different theories of gravity, such as Einstein\u2013Yang\u2013Mills","Functions Label":0}
{"Functions Text":"Originally it was proposed that due to mutual gravitational interactions that all black holes would have been ejected from globular clusters","Functions Label":0}
{"Functions Text":"These differences","Functions Label":0}
{"Functions Text":"do not seem to be related to unaccounted variation in the CO-to-H2 conversion factor","Functions Label":0}
{"Functions Text":"but has been interpreted as evidence that SiO disappears from the gas phase at high densities to be incorporated into dust grains","Functions Label":1}
{"Functions Text":"This method has been intensively implemented with updated observations","Functions Label":0}
{"Functions Text":"To limit the ISGRI calibration uncertainties","Functions Label":2}
{"Functions Text":"This is within the range of the equipartition magnetic fields of 17 HFP radio sources","Functions Label":5}
{"Functions Text":"and 5 HFPs at 0.084\u2004 \u2004z\u2004 \u20041.887 (18\u2013160 mG","Functions Label":5}
{"Functions Text":"These values are in very good agreement with those measured from the average long-term Swift\/BAT (Burst Alert Telescope) spectrum","Functions Label":5}
{"Functions Text":"As shown in greater detail in Stritzinger et al. (2020, hereafter Paper I), the ILRT subtype is well represented by NGC 300-2008-OT and SN 2008S, and has been linked to asymptotic giant branch (S-AGB) stars","Functions Label":0}
{"Functions Text":"that die as electron-capture supernovae","Functions Label":0}
{"Functions Text":"In this paper, the data from DC to 2 MHz are discussed. These measurements are obtained from the potentials of the four antennas, V1 through V4, that are located in the plane perpendicular to the Sun\u2013satellite line. They produce E12 = (V1\u2212V2)\/3.5 and E34 = (V3\u2212V4)\/3.5, which are then rotated into the spacecraft coordinate system to produce EX and EY. The direction, X, is perpendicular to the Sun\u2013spacecraft line, in the ecliptic plane, and pointing in the direction of solar rotation (against the ram direction), Y is perpendicular to the ecliptic plane, pointing southward, and Z points toward the Sun. The numerical factor, 3.5, is the effective antenna length","Functions Label":2}
{"Functions Text":"No Compton reflection hump has been detected with","Functions Label":1}
{"Functions Text":"or NuSTAR","Functions Label":1}
{"Functions Text":"despite the presence of a complex Fe K\u03b1 line.","Functions Label":1}
{"Functions Text":"The initial dispersion of the LUV\u2005\u2212\u2005LX relation is relatively large (\u03b4\u2004\u223c\u20040.35\u22120.4,","Functions Label":1}
{"Functions Text":"but after a detailed study, Lusso & Risaliti (2016) suggest that most of the observed dispersion is not intrinsic, but it is rather due to observational effects.","Functions Label":1}
{"Functions Text":"We use an \u03b1 approximation for the turbulent viscosity","Functions Label":2}
{"Functions Text":"when the (r\u03c6) component of the stress tensor tr\u03c6 is written as (5)\\begin{equation} t_{r\\phi}=\\alpha\\, P, \\label{trphi} \\end{equation}tr\u03c6=\u03b1\u2009P,where the phenomenological non-dimensional parameter \u03b1 \u2264 1.","Functions Label":2}
{"Functions Text":"Early on, the MUSE Guaranteed Time Observations (GTO) team established surveys including MUSE-QuBES","Functions Label":0}
{"Functions Text":"to relate gas traced by absorbers to galaxies.","Functions Label":0}
{"Functions Text":"Topological estimators such as the Minkowski functionals (MFs) are also important diagnostics in this direction as they carry information at all orders. The MFs have been extensively developed as a statistical tool in a cosmological setting for both two-dimensional (2D; projected) and 3D (redshift) surveys. The MFs have analytically known results for a Gaussian random field, making them suitable for studies of non-Gaussianity. Examples of such studies include CMB data","Functions Label":0}
{"Functions Text":"These microlensing magnification estimates are calculated after subtracting the emission line flux ratios, which are little affected by microlensing (see, e.g.,","Functions Label":2}
{"Functions Text":"from the continuum flux ratios, and are therefore virtually free from extinction, substructure, and macro model effects (as these affect the line and continuum flux ratios equally).","Functions Label":2}
{"Functions Text":"Furthermore, well-defined large samples of white dwarfs are an extremely useful starting point for identifying rare white dwarf types like","Functions Label":3}
{"Functions Text":"or white dwarfs with dusty or gaseous planetary debris discs","Functions Label":3}
{"Functions Text":"Observations have shown that the AGN fraction does increase with decreasing distance between two merging galaxies","Functions Label":0}
{"Functions Text":"but this has not been well tested at the very centers of merger-remnant galaxies because of the observational difficulty of detecting and resolving two AGNs with separations 10 kpc.","Functions Label":3}
{"Functions Text":"Moreover, c-C3HD and c-C3D2 have been surveyed in a sample of low-mass prestellar and protostellar cores","Functions Label":0}
{"Functions Text":"finding that the corresponding isotopic ratios are relatively uniform, within a factor of a few, and similar to those in L1544 and L483.","Functions Label":0}
{"Functions Text":"However, differences in the yields produced in the He detonation can in part be attributed to the slightly different setups of Model M2a (and therefore Model M2a_pp) and Model M10_05_1 at the beginning of the relaxation simulation, with the differences in the total and shell masses being less than 1% (see","Functions Label":6}
{"Functions Text":"for an explanation of the difference).","Functions Label":6}
{"Functions Text":"This results in different spatial distributions in which tiny grains are present at the disk surfaces","Functions Label":1}
{"Functions Text":"and in the cavity or gaps from which the pebbles are missing (e.g.","Functions Label":1}
{"Functions Text":"We expect the centroid of a blended source to be determined with poor accuracy (see e.g.","Functions Label":2}
{"Functions Text":"For this reason as a further test we plotted the distribution of distances in arcsec of the VMC sources cross-matched with the OGLE IV RRLs.","Functions Label":2}
{"Functions Text":"In some cases, the mergers eventually devoid their entire neighbourhood, leaving behind a single elliptical galaxy of group-scale mass, called a fossil group galaxy","Functions Label":0}
{"Functions Text":"Using their spectroscopic catalog with radial velocities measured with an external accuracy of 7\u201310 km\u2009s-1 and applying photometric parallax relations, the SDSS teams have traced K\u2013M dwarfs in the distance range up to ~2 kpc, thus providing valuable information on the spatial, velocity, and metallicity distributions with respect to vertical distance from the Galactic plane","Functions Label":0}
{"Functions Text":"as well as on the luminosity and mass functions of low-mass dwarfs in the Galactic disk","Functions Label":0}
{"Functions Text":"Second, our calculations neglect the effects of binary star systems. Mass transfers and mergers between binary companions can extend the period over which ionizing photons are produced by the stellar population, which would harden the time-integrated spectrum","Functions Label":1}
{"Functions Text":"Then, as this polarization propagates, it is further modified by Faraday effects, important for depolarizing accretion flows down to observed levels and generating the observed rotation measure","Functions Label":0}
{"Functions Text":"Following OSO-7, a series of spacecraft (Skylab, Helios, P78-1 Solwind, SOHO, Coriolis, and STEREO, etc.) have observed thousands of CMEs leading to a vast literature","Functions Label":0}
{"Functions Text":"detected INV during three nights out of three using C- and F-tests (a total monitoring duration of 16 h in the R-band).","Functions Label":1}
{"Functions Text":"Fornasier et al. (2015) obtained results for the 67P nucleus surface reflectivity applying a HG-type phase function","Functions Label":2}
{"Functions Text":"with a best-fitting G of \u22120.13. Fig. 5 shows the phase angle-corrected af\u03c1 values of 67P for the various phase function solutions.","Functions Label":2}
{"Functions Text":"Asymmetric inflow reconnection has also been investigated in","Functions Label":0}
{"Functions Text":"laboratory experiments","Functions Label":0}
{"Functions Text":"The LMC star cluster formation history is believed to be three-staged, including a period of rapid cluster star formation in the early universe (\u03c4 \u2273 10 Gyr), followed by a long quiescent period between \u223c10 and \u223c2\u20134 Gyr ago and then by a period of rapid star cluster formation extending to the present day, potentially due to the interaction between the LMC and SMC","Functions Label":0}
{"Functions Text":"Hydrodynamic simulations using the code HYADES","Functions Label":2}
{"Functions Text":"developed a classification scheme based on a disk+power law fit, to be applied to ULX spectra, according to which the spectral state of an ULX source can be defined by the disk temperature, the power-law slope, and the ratio between the flux contribution of the two spectral components in the 0.3\u22121 keV band.","Functions Label":0}
{"Functions Text":"The X-ray luminosity of GRBs is given by the energy input from the electromagnetic and gravitational waves into the surrounding medium","Functions Label":2}
{"Functions Text":"Therefore, in order to standardize GRBs as standard candles through the Dainotti relation, it is recommended that X-ray plateaus caused by the same physical mechanism are used (electromagnetic dipole radiation or gravitational waves).","Functions Label":2}
{"Functions Text":"For the three first cases, we assumed ISM[M\/H](R\u2299) = 0.0 to estimate Rbirth from the stellar metallicity. However,","Functions Label":6}
{"Functions Text":"have their own zero point, defined as: [Fe\/H]\u2004=\u2004\u22120.06\u2005*\u2005Rg\u2005+\u20050.57, with a clear shift in the relation compared to the other ones assumed in this work.","Functions Label":6}
{"Functions Text":"Single-case studies reported some EIT waves covering a whole solar hemisphere","Functions Label":0}
{"Functions Text":"For the Bernard-Salas et al. (2009),","Functions Label":2}
{"Functions Text":"and the GOALS samples, we excluded all the composite starburst-AGN objects identified as those with a detection of [NeV] either at 14.3 or 24.3 \u03bcm.","Functions Label":2}
{"Functions Text":"A cool spot at a higher latitude would reduce the amplitude of the NIR wide-band flux modulations; a quenching of the convective shifts or the Zeeman effect also do not appear to be viable explanations because they increase the effect of a cool spot on the RV at NIR wavelengths","Functions Label":2}
{"Functions Text":"The most rapid changes of surface temperature occur early,","Functions Label":0}
{"Functions Text":"and then when the temperature drops below the critical temperature for core neutrons to become superfluid, which activates the efficient neutrino emission process of Cooper pair formation and breaking","Functions Label":0}
{"Functions Text":"For PN in O-rich AGB atmospheres, the disagreement between the observed abundances, (1\u20132) \u00d7 10\u22128","Functions Label":6}
{"Functions Text":"and the calculated maximum chemical equilibrium abundance is almost three orders of magnitude.","Functions Label":6}
{"Functions Text":"Compact starbursts containing hot O stars offer an alternative explanation for the relative intensities of LINER emission lines","Functions Label":1}
{"Functions Text":", but have difficulty explaining the broad Balmer emission wings often seen in LINER spectra","Functions Label":1}
{"Functions Text":", since this would require long-lived supernova remnants.","Functions Label":1}
{"Functions Text":"The H\u03b1 line of V410 Tau can grow much stronger and broader during a flare, and also show asymmetries; however, the observed asymmetries seen during flares do not show excess emission with apparent peaks shifted out to greater than \u00b1200 km s\u22121","Functions Label":1}
{"Functions Text":"as seen here in PTFO 8-8695.","Functions Label":1}
{"Functions Text":"L.A. Cosmic","Functions Label":2}
{"Functions Text":"was used to clear the image of cosmic rays to produce the final H\u03b1 and final R image.","Functions Label":2}
{"Functions Text":"Several attempts have been made to infer clusters dynamical state, using both observational data and simulations, by analysing the images of the emission in optical","Functions Label":0}
{"Functions Text":"and in the X-ray band (see e.g.","Functions Label":0}
{"Functions Text":"A relaxed, dynamically old group or cluster should be characterized by a central galaxy which is the brightest (most massive) member by a significant margin (e.g.","Functions Label":0}
{"Functions Text":"Different column densities of para-H2CO only weakly affect derived kinetic temperatures (see Fig. 3 in","Functions Label":2}
{"Functions Text":"as long as all lines are optically thin.","Functions Label":2}
{"Functions Text":"The spectra of the AGNs to be compared are taken from those of the IR galaxies observed by Spitzer\/IRS","Functions Label":2}
{"Functions Text":"As mentioned previously, magnetars have been identified in many studies as promising candidates for the acceleration of cosmic rays and the production of secondary high-energy neutrinos, for instance Blasi et al. (2000), Fang et al. (2012, 2013), Lemoine et al. (2015),","Functions Label":3}
{"Functions Text":"We estimated the optical depths of the AGNs of Stierwalt et al. (2013), Wu et al. (2010), and Roussel et al. (2006) by ourselves in the same manner as was performed for LEDA 1712304 with the method defined by","Functions Label":2}
{"Functions Text":"and continue to attract much attention in the quest for unraveling quantum effects such as the geometric phase (GP) in chemical reactions","Functions Label":0}
{"Functions Text":"Using Bayesian analysis to fit a distribution function to full 6D phase-space data (globular clusters, satellites, and halo stars) has been a recent popular choice among many works","Functions Label":0}
{"Functions Text":"The ascending of a filament can go on high into the corona (successful eruptions) and gives rise to a coronal mass ejection (CME) or can stop at some greater height in the corona (confined or failed eruptions)","Functions Label":0}
{"Functions Text":"Accounting for the ramp up of the driver and scaling the values, this corresponds to an energy injection rate of \u22485.6 \u00d7 1023 erg s\u22121 at the maximum driving speed. During the quasi-steady phase, this injection is balanced by losses to numerical diffusion and equates to roughly the free energy available for heating the plasma. Even after accounting for the unrealistically fast driving speed (see below), this energy release rate compares well with the observed values of 1023\u20131024 erg s\u22121 for bright points","Functions Label":5}
{"Functions Text":"A possible fix of this proposal is to introduce rapidly spinning magnetars born from binary neutron star (BNS) mergers","Functions Label":0}
{"Functions Text":"Recently, several works have attempted to estimate the expected coalescence time for binary BHs by post-processing cosmological simulations, finding time-scales on the order of 100s of Myr to Gyr for the binary coalescence time (e.g.","Functions Label":0}
{"Functions Text":"For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm\u22123 is assumed","Functions Label":2}
{"Functions Text":"Generally, the spectrum hardens when the flux increases","Functions Label":0}
{"Functions Text":"but photon indices can saturate at higher fluxes","Functions Label":0}
{"Functions Text":"It is not yet clear which process is the dominant source of the elements in the early Universe (see discussions by, e.g.,","Functions Label":3}
{"Functions Text":"As a consequence, mergers are also expected to play a significant role in driving the evolution of galaxy properties, for example,","Functions Label":0}
{"Functions Text":"star formation in the host galaxy or by driving its morphological evolution (e.g.","Functions Label":0}
{"Functions Text":"At the centre of the debate is the strength of the surface dipole field and any multipolar component. Should the dipole field strength be similar to that of Galactic HMXBs (1012 G \u2013 e.g.","Functions Label":3}
{"Functions Text":"then it is quite plausible that the flow will be supercritical ($\\dot{m}\/\\dot{m}_{\\rm Edd} \\gt $ 1 where $\\dot{m}_{\\rm Edd}$ is the Eddington accretion rate) at radii greater than the magnetospheric truncation radius (rM).","Functions Label":3}
{"Functions Text":"We have now access to the size evolution up to z ~ 10 from the deepest HST imaging data","Functions Label":0}
{"Functions Text":"There is a debate about the extent to which DIG affects measurements of gas-phase metallicity and its radial slope","Functions Label":3}
{"Functions Text":"as some observations indicate lower metallicity (up to 1 dex) in DIG compared to nearby H ii regions.","Functions Label":3}
{"Functions Text":"For example, if G1.75-0.08 follows the line width\u2013size relation in the central molecular zone, or CMZ, which for HCN is found to be \u03c3 \u221d R0.62","Functions Label":1}
{"Functions Text":", the aforementioned HCN(1 \u2013 0) line width would be expected to be only ~2.5 km s\u22121 on the ~0.1 pc scale, which is a typical inner width (FWHM) of filamentary molecular clouds","Functions Label":1}
{"Functions Text":"In particular, classification by ML (e.g.,","Functions Label":7}
{"Functions Text":"can avoid time-consuming visual inspections and will be helpful for the visual classification of galaxy\u2212galaxy interactions from the forthcoming large surveys.","Functions Label":7}
{"Functions Text":"We stress that our SOFIA\/FORCAST images do not detect the outer polar rings seen in Spitzer IRAC images","Functions Label":6}
{"Functions Text":"For the sake of simplicity, the specific heat capacity c was assumed constant, c\u2004=\u2004560 J kg\u22121 K\u22121, and the regolith grain density obtained for C-type meteorites was used, \u03c1\u2004=\u20043.11 g cm\u22123 (both from","Functions Label":2}
{"Functions Text":"We collect the total radio flux density from literature","Functions Label":2}
{"Functions Text":"We estimate the fluxes Fx (see Table 1) of LHS and HIMS of the 1999 outburst of the source","Functions Label":2}
{"Functions Text":"There are examples of merging clusters that show presence of X-ray\u2013SZ offsets, such as","Functions Label":0}
{"Functions Text":"and Bullet cluster","Functions Label":0}
{"Functions Text":"For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm\u22123 is assumed","Functions Label":2}
{"Functions Text":"A novel aspect of the search here presented is the inclusion in the data analysis chain of the uncertainty that possible unknown parameters, related to the characteristic activity of the central engine, can introduce in the neutrino flux evaluation. This is crucial in order to correctly interpret the validity of model-dependent results, in terms of upper limits set by non-detections of neutrinos in coincidence with GRBs","Functions Label":1}
{"Functions Text":"Analogously to previous ANTARES searches","Functions Label":1}
{"Functions Text":"MC simulations of the signal predicted by NeuCosmA were performed, while the respective background was estimated directly from off-source data collected by ANTARES.","Functions Label":1}
{"Functions Text":"Following Rosdahl et al. (2018), we have calibrated the SN feedback in order to reproduce the high-redshift stellar mass\u2013halo mass relation from abundance matching","Functions Label":2}
{"Functions Text":"The same source was followed up and consistently localized at other wavelengths (e.g.,","Functions Label":0}
{"Functions Text":"On the one hand, it is more energetically favorable for the system to populate new degrees of freedom, such as hyperons","Functions Label":1}
{"Functions Text":"in order to lower its Fermi energy (starting at about two times the saturation density).","Functions Label":1}
{"Functions Text":"Such studies are dependent on the observations of a handful of storms that have approached or rivalled the Carrington geomagnetic storm in observed\/inferred intensity and\/or auroral extent. These include great storms in","Functions Label":0}
{"Functions Text":"May 1921","Functions Label":0}
{"Functions Text":"For consistency, we adopt the translation of this to the absolute velocities of cluster galaxies normalized by their respective galaxy cluster velocity dispersions into the range $0.3 \\lt |\\Delta \\mathrm{V}|\/\\sigma _{r_{200}} \\lt 0.5$ as deduced by","Functions Label":2}
{"Functions Text":"With ALMA and NOEMA, ground-based observations of the [C\u202fII] 158 \u03bcm line in high redshift galaxies have come into reach and such data are routinely used to infer SFRs","Functions Label":0}
{"Functions Text":"based upon validations of this relationship in the nearby Universe","Functions Label":0}
{"Functions Text":"A common interpretation of the MS is that the location of galaxies relative to the MS follows a different time evolution of SFR","Functions Label":0}
{"Functions Text":"Several studies have already measured the distance ratios (e.g.","Functions Label":0}
{"Functions Text":"though they are afflicted by several systematics such as, uncertainties in modelling cluster profiles and cosmic variance in the case of multiple strong lens systems, and photometric redshift uncertainties as well as imaging systematics that cause a redshift-dependent shear calibration in the case of weak lensing.","Functions Label":6}
{"Functions Text":"The ESPRESSO DFS concept","Functions Label":0}
{"Functions Text":"was conceived during its preliminary design phases with the goal of maximizing operational efficiency, flexibility, and scientific output while complying with the standard Paranal Observatory operational scheme.","Functions Label":0}
{"Functions Text":"A neutron-star merger consists of several stages starting from the late inspiral, where accurate numerical waveforms are needed to calibrate analytical models for waveforms, through merger","Functions Label":3}
{"Functions Text":"which requires sophisticated microphysics in terms of finite-temperature equations of state (EOS) satisfying recent observational constraints","Functions Label":3}
{"Functions Text":"Indeed, the H\u03b2","Functions Label":2}
{"Functions Text":"and Mg\u202fII lines seem to arise from the same part of the BLR in various quasars (e.g.,","Functions Label":2}
{"Functions Text":"and should both yield similar sizes; whereas the Fe\u202fII line is thought to arise from a larger part of the BLR","Functions Label":2}
{"Functions Text":"Therefore, the combination of the two signals modelled as a single BLR emission could broaden our measurement and induce its slight bi-modality.","Functions Label":2}
{"Functions Text":"In the solar wind, the evaluation of turbulence is well described by magnetohydrodynamic (MHD) theory","Functions Label":0}
{"Functions Text":"and the turbulence transport throughout the heliosphere has been studied over the years (e.g.,","Functions Label":0}
{"Functions Text":"As mentioned above, after its discovery in 2010, V2492 underwent a long-lasting period of strong activity with intermittent burst and fading events","Functions Label":0}
{"Functions Text":"and reached its maximum recorded brightness in 2017","Functions Label":0}
{"Functions Text":"This equation, usually referred to as the Landau\u2013Lifshitz (LL) equation, has important consequences: it is of the second order, does not violate the principle of inertia, and the self-force vanishes in the absence of the external (Lorentz) force","Functions Label":0}
{"Functions Text":"Many computational works have so far focused on a few important astrochemical species like H, H2, N, O, CO, and CO2, in which BEs are calculated on periodic\/cluster models of crystalline\/amorphous structural states using different computational techniques (e.g.,","Functions Label":0}
{"Functions Text":"For some Cepheids (OGL0434, OGL0501, OGL0510, OGL0512, OGL0528, OGL0545, OGL0590, OGL0712, OGL0757, OGL0966, and OGL0992), we also included V-band light curves from the","Functions Label":2}
{"Functions Text":"and\/or ASAS-SN survey","Functions Label":2}
{"Functions Text":"to increase the baseline coverage.","Functions Label":2}
{"Functions Text":"This model can naturally fit the observational positive relationships between \u03b1OX and \u03bbO as well as \u0393 and \u03bbO in RQAGNs","Functions Label":1}
{"Functions Text":"In observations, RLAGNs appear to have different properties than RQAGNs, for instance the positive relationships listed above in RQAGNs have not been found in RLAGNs","Functions Label":1}
{"Functions Text":"This crude selection of cluster member candidates is obviously prone to contamination by interlopers. So, we further refine it using the shifting gapper method","Functions Label":2}
{"Functions Text":"which uses velocity and spatial information on the candidates simultaneously. The shifting gapper method spatially distributes the candidates according to their clustercentric distance in radial bins. The mean velocity of the candidates within each bin is calculated, and those candidates with velocities that are too far from the others are rejected. As unrelaxed clusters are more likely to have a broader spatial distribution, this procedure naturally allows candidates at larger distances to be identified as cluster members for these systems. These two steps are, thus, essential to guarantee that our cluster membership algorithm implicitly takes into account the dynamical state of the systems and does not bias the measurement of their total luminosity, while minimizing contamination by interlopers at the same time.","Functions Label":0}
{"Functions Text":"The observed ratios of the infrared fine-structure ionic lines (Ne ii, Ar iii, and S iv;","Functions Label":2}
{"Functions Text":"indicate that at least eight O7.5V stars are necessary to account for the ionization of the region.","Functions Label":2}
{"Functions Text":"With the large number of newly discovered exoplanets expected in the next 10 years by ground-based surveys such as","Functions Label":0}
{"Functions Text":"as well as the ongoing Transiting Exoplanet Survey Satellite (TESS) space survey","Functions Label":0}
{"Functions Text":"a rapid characterization scheme of the interior structure of these planets will become increasingly necessary to further our understanding of planetary populations.","Functions Label":3}
{"Functions Text":"To take the contribution of f\u2013f and f\u2013b radiations into account and estimate the corresponding spectra, we used the\u2009chianti package","Functions Label":2}
{"Functions Text":"The Largest Linear Sizes (LLS) and radio powers of relics are correlated, as well as the integrated spectral index and the radio power","Functions Label":0}
{"Functions Text":"Since the light curve inversion produced convex shape models only, then shadowing and self-heating effects inside global-scale concavities (see","Functions Label":6}
{"Functions Text":") were not possible to model.","Functions Label":6}
{"Functions Text":"Through the work of \u0160vestka & Fritzov\u00e1-\u0160vestkov\u00e1 (1974), Kahler et al. (1978, 1984)","Functions Label":0}
{"Functions Text":"(1982","Functions Label":0}
{"Functions Text":"1983b), Cane & Stone (1984), Klecker et al. (1984), Mason et al. (1984, 1986), Meyer (1985), Reames et al. (1985, 1994, 1996), Cane et al. (1986, 1988), Luhn et al. (1987), Reames (1990, 1999), Kahler (1992, 1994), Gosling (1993), and others, involving various comparisons of SEP events with flare electromagnetic emissions and coronal mass ejections (CMEs), as well as considerations of SEP composition, charge states, and the longitude distribution of SEP-associated flares, the two-class picture of SEP acceleration presciently proposed by Wild et al. (1963) became established.","Functions Label":0}
{"Functions Text":"At the supranuclear densities of the outer core, the Fermi energy for protons and neutrons is well above the typical temperature of a mature neutron star, and both the neutrons and protons are expected to condense into Bardeen\u2013Cooper\u2013Schrieffer superfluids, with 3PF2 and 1S0 Cooper pairing, respectively","Functions Label":2}
{"Functions Text":"where \u03a6mad \u2248 50\u03a6mad,1.7 is the saturated magnetic flux","Functions Label":2}