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+,Functions Text,Functions Label
+0,Several modelling works on this comet have shown that ion composition in the coma varies based on the sublimation rate of the nucleus,0
+1,as well as strong AGN/QSO and Supernova feedback that will heat and expel the gas (e.g.,0
+2,"Indeed, large atomic gas reservoirs, together with low molecular gas masses",1
+3,and stellar masses,1
+4,indicate that GRB hosts are preferentially galaxies that have very recently started a star formation episode.,1
+5,"J04414489+2301513 (a~15 AU,",2
+6,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,2
+7,"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.",3
+8,We now extend the original formalism,4
+9,in another direction.,4
+10,"Consequently, the image separation distribution is consistent with the SDSS measured stellar VDF",5
+11,and the Second Southern Sky Redshift Survey (SSRS2) inferred stellar VDF,5
+12,although the two stellar VDFs are significantly different from each other concerning their corresponding parameter values.,1
+13,"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",0
+14,"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",2
+15,We derived AV(s) by adopting a simplified model of the local distribution of the interstellar dust density,2
+16,"expressed by the relation ρ = ρ0·sech2(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.",2
+17,"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—all of these small-scale magnetic activities contribute greatly to coronal heating",0
+18,NaCl was first investigated using a chirped-pulse Fourier transform microwave (CP-FTMW) spectrometer with a laser ablation source,0
+19,operating between 6.0 and 12.0 GHz to sample swiftly the rotational spectra of the different species present in the supersonic expansion.,0
+20,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,3
+21,"Then, observations of oscillation modes in",0
+22,and in B-type stars,0
+23,provided us new Rosetta stones to constrain the transport of angular momentum in the whole Hertzsprung-Russell diagram.,0
+24,"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",5
+25,Many reports on the eruption of filaments are concerned with torus instability or/and kink instability,0
+26,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,0
+27,"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",2
+28,"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",1
+29,and the activity of OJ 287 from the end of 2015 to the middle of 2017,1
+30,"More recently, other surveys also revealed that the fraction of high-EW Ly α emitters increases towards fainter UV magnitudes",0
+31,We used a compensated filter to eliminate the small wavelength modes linked with such numerical noise,2
+32,The behavior for the low- and high-dust contents is quite different.,6
+33,"On the one hand, the escape fractions versus NHI,cl scales for τd,cl = 1 (filled symbols in Fig. 12) as predicted by",5
+34,in their “surface scatter” approximation,5
+35,"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.",6
+36,Mrk 421 is a very hard spectrum γ-ray source with a photon index of ≈1.77 and its semiminor and semimajor axes at 68 per cent confidence are of 0$_{.}^{\circ}$0067 as derived in,2
+37,"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 “megamasers”) 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",3
+38,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 keV,0
+39,"The temperature Tcl of each cloud is determined as the result of a one-zone calculation (for details, see",2
+40,"Indeed, only lower limits to the high-energy cut-off have been found with NuSTAR (210 keV",1
+41,"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",2
+42,"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.",0
+43,"Also, metals have been detected, using UV/optical absorption lines, around",0
+44,"and HD 32297 (Na i,",0
+45,The initially low polarization levels often rise during the plateau phase,0
+46,with a polarization angle that typically remains nearly fixed throughout (e.g.,0
+47,"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 vi",0
+48,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,2
+49,The modelfit program fits image-plane model components to the visibilities in the uv plane.,0
+50,"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.",1
+51,We used electron collisional excitation and ionization rates from the quantum mechanical computations of,2
+52,for the energy levels of up to 5s (2S).,2
+53,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,0
+54,"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",2
+55,for the details of the implementation).,2
+56,"Once the existence of a relationship between age and chemical clocks was established (see, e.g.,",0
+57,"In the equation above, Plin(k) is the linear matter power spectrum computed using the Boltzmann code CLASS",2
+58,assuming the Planck 2015 (Ade et al. 2016) fiducial cosmology.,2
+59,Numerous attempts to calibrate SZ masses have been made in the literature using,0
+60,SPT clusters,0
+61,"Andromeda hosts both very little gas and very little star formation, while the black hole is basically quiet and has some murmurs",0
+62,"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 ∼ 10−3",2
+63,The case of solar pulsational stability has been studied in detail,0
+64,while the space missions,0
+65,and Kepler,0
+66,have provided high-quality seismic data for stars of different flavours against which we can test models and further our understanding of stellar pulsations.,0
+67,"In this scenario, depending on the misalignment angle, the outer disk image will show narrow shadow lanes (e.g.,",0
+68,"Quasi-periodic oscillations (QPOs) have been detected from many Be binaries, such as",0
+69,4U 0115+63,0
+70,Yang et al. (2013) showed that at 2:1 and 6:1 resonances with a static/slab ocean (see Section 2.2.2 of,0
+71,"), 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.",0
+72,The Sun is situated at the inner edge of the Orion arm,0
+73,"Here, for each of the terms we use the sign conventions given in the source code for the pulsar timing software tempo21",2
+74,Frequently a major issue in these applications is the use of formulations derived assuming isotropy in turbulence that is actually anisotropic,1
+75,", this being the typical case for solar wind and magnetosheath turbulence.",1
+76,and found no Class II CH3OH masers in the sources of our sample,2
+77,Simulations and theory together suggest that the magnetic field plays an important role in collimating the particles and giving them a jet like shape,0
+78,A common mitigation strategy is to model the data as a Gaussian mixture of inlier and outlier distributions with differing variance,2
+79,In,0
+80,", 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.",0
+81,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,2
+82,"The latter is longer by roughly the mass ratio of Mars to Titan, which can be understood from Eq. (2) of",2
+83,"Unlike the subgrid recipes which involve kinetically prescribed decoupled winds and cooling-suppressed blastwaves, the FIRE simulations solve the ‘overcooling’ problem by explicitly modelling the radiation pressure, stellar winds, and ionizing feedback from young stars as taken directly from the population synthesis code starburst99",2
+84,"The galaxies presented by Bernard-Salas et al. (2009) have instead an average redshift of 0.0074, while the sample by",1
+85,has an average redshift of 0.0044.,1
+86,"From studies on the optical–IR colour–magnitude diagram, it is known that FSRQs in general show an RWB trend, which is attributed to them having a luminous accretion disc",1
+87,Mass transfer will continue for ≈1 Myr at a rate exceeding 10−9 M⊙ yr−1 until hydrogen shell burning is finished and the star contracts to become a carbon–oxygen WD with a thick helium layer and a small residual layer of hydrogen. The high accretion rate will heat the accreting WD significantly,0
+88,It was found that the complex dielectric function from,2
+89,"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 μm features, so this component was included in the models.",2
+90,"For example, studies of young clusters embedded in moderate-mass MCs (∼104M⊙)",0
+91,"have shown that their age histograms contain a large majority of young (1–2 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",0
+92,"The Blandford–McKee blast wave of the ultrarelativistic shock moving into a medium of uniform external density ρ0 has radius R ≃ 2cT Γ2/(1 + $z$) and explosion energy per unit solid angle E/Ω ≃ ρ0R3Γ2c2, which gives Γ ≃ 9(Eiso, 53/n0)1/8(T/[(1 + $z$)day])−3/8, where $E=10^{53}\, \mbox{erg}(\Omega /4\pi)E_{iso,53}$ and n0 is the external density in cm−3",2
+93,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,5
+94,"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 “EIT waves” or “EUV waves”) are in close empirical correlation with type II radio bursts",0
+95,"In other words, the velocity equivalent of the observed line width, Wobs = c × Δλ/λ, 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×Δλλ2=Winstrumental2+WDoppler2+Wturbulence2,assuming that all three line broadening components have a Gaussian profile (Eq. (4.17) of",2
+96,"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",2
+97,The pexrav model assumes an exponentially cutoff power-law spectrum reflected from neutral material,2
+98,"n0 is limited between 10−5 and 100 cm−3, in line with what has been found in these sources",2
+99,"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 ±35 G",2
+100,"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.",1
+101,"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",1
+102,are typically a few times shorter than the age of the remnant.,1
+103,"However, the latest observations by Planck",3
+104,indicate that there may be some problems with such an inflationary scenario,3
+105,Their simulation results also reveal that the bipolar pulses reported in the Enceladus plume by,1
+106,and Pickett et al. (2015) could most probably be ion holes.,1
+107,The analytical expressions for the Sérsic model are taken from Prugniel & Simien (1997) (see also,2
+108,"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",0
+109,down to those that have only weak CSM interaction and faster decline rates that are difficult to distinguish from radioactive decay or light echoes.,0
+110,Recent works have studied lensing effects in the existing LIGO/Virgo O1 and O2 events,0
+111,In fact observations show either no or positive relationships between star formation rates and SMBH accretion rates but no negative trends are seen,3
+112,The third Fermi–LAT catalogue (3FGL catalogue:,2
+113,has been used to include the contributions of sources inside the ROI.,2
+114,Aside from electron dissociative recombination of C4H3NH+,1
+115,neutral production of CH3C3N can occur in a few ways,1
+116,"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.",2
+117,"Recently, quasars observed with multiple measurements, another potential cosmological probe with a higher redshift range that reaches to z ∼ 5, is becoming popular to constrain cosmological models in the largely unexplored portion of redshift range from z ∼ 2 to z ∼ 5. A sample that contains 120 angular size measurements in intermediate-luminosity quasars from the very long baseline interferometry (VLBI) observations",0
+118,"has become an effective standard ruler, which have been extensively applied to test cosmological models",0
+119,"An alternative scenario, such as dust formation in the KN that could also explain such a blue-red evolution, has been ruled out",0
+120,The authors used their new results together with the available literature results covering up to z = 1.3,2
+121,to further solidify the evidence supporting passive evolution and a formation redshift zform ≈ 2.,1
+122,"The upcoming LoTSS catalogs, covering a large sky area, will help us to explore further regarding",7
+123,and the current puzzling dipole signal observed with radio catalogs,7
+124,In case of lamp-post models,1
+125,general-relativistic effects will rotate the polarization position angle along null geodesics from the corona towards the disc,1
+126,"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.",1
+127,While spatially extended optical jets and bipolar CO molecular outflows have been observed in numerous Class 0/I protostars,0
+128,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.,0
+129,XRD of their sample obtained from heating boehmite to 1173 K,1
+130,"suggests δ-alumina to be present, though some amounts of θ-alumina and α-alumina are present, as they deduce from XRD and infrared and NMR spectroscopy.",1
+131,"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.",0
+132,It has been shown that the fraction of AGN in mergers tends to increase as the separation between the two galaxies decreases,0
+133,"On the other hand, a positive correlation exists between the average Φ and the average Fidx with the linear PCC = 0.65 (refer to Figure 5(b)). Such correlation of Φ with flaring activity in individual ARs has been reported in many previous studies (e.g.,",5
+134,We have compared to N-body simulations the well-known GSM,1
+135,"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 ∼5 h−1 Mpc over the range of redshifts covered by future surveys.",6
+136,"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: 0.1–1 Gyr",1
+137,The background Alfvén or slow continuum can be due to the variation of the plasma density,0
+138,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,0
+139,"In particular, the SPS approach has been applied to observations of various Galactic and extragalactic environments (e.g.,",0
+140,"Internally, the ejecta release their energy through",0
+141,"or photospheric dissipation (e.g.,",0
+142,and produce the prompt gamma-ray emission of GRBs.,0
+143,"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",7
+144,"In the obtained size distribution, erosive collisions are more important than catastrophic collisions (see Fig. 10 of",2
+145,"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 km0.96R2.5 au4.18where sp is the size of planetesimals, R is the radius of the planetesimal belt, and e is the eccentricity of planetesimals.",2
+146,"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",1
+147,"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",2
+148,"see also Bisnovatyi-Kogan (2011), to calculate the transient disk structure.",2
+149,The heating by jets propagating through the galaxies could prevent gas from cooling and cut-off the gas supply for further star formation,0
+150,"With such a bin width of ∼0.03 dex, any biases in ξ are less than $5{{\ \rm per\ cent}}$ of the observational uncertainty for a BOSS CMASS-like sample (see",2
+151,"As they pass by, they modify the transverse magnetic field and velocity components but, do not alter the gas pressure or the mass density",0
+152,at least in the linear limit and in a homogeneous background plasma.,0
+153,Power asymmetry from CMB data has also been a matter of intense debate and scrutiny,0
+154,Although thermochemical equilibrium models predict the formation of condensate clouds with various composition in these hot atmospheres,1
+155,"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",1
+156,Equation (16) describes turbulent fluctuations from a Lagrangian point of view,2
+157,"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",0
+158,"The masses of the condensations are around 0.01−0.1 M⊙, comparable to or larger than the local Jeans mass.",0
+159,"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",0
+160,"Large uncertainties in VCME restrict further improvements to the TT prediction of the shock. Possible solutions to this restriction could include adopting the CME’s radial speed, which is derived from models (such as cone models) based on single spacecraft observations",1
+161,The influence of tidal truncation is therefore limited to stellar multiples,0
+162,or during the decay of higher order multiplicity,0
+163,Many stars in the solar neighbourhood are born in regions where UV fields are sufficient to significantly shorten disc lifetimes,0
+164,"However, in Tomaru et al. (2019, hereafter Paper I) we show instead that thermally driven winds can explain this switch (see also",0
+165,"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",1
+166,"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",5
+167,"This strengthened earlier results based on smaller samples (e.g.,",5
+168,"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.,",0
+169,"In this regard, the upcoming ADITYA-L1 mission",7
+170,with the Visible Emission Line Coronagraph,7
+171,will provide much better data and hence will help in arriving at much stronger conclusions on the evolution of CME legs.,7
+172,We then used the phases determined in,2
+173,"during our last observing season as starting values,",2
+174,Recent high-resolution hydrodynamical simulations of ‘zoomed’ 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,1
+175,"Interaction of CRs with molecular clouds is accompanied by various processes generating observable radiation signatures, such as",0
+176,"as well as production of neutral pions whose decay generates gamma-rays in the GeV (e.g.,",0
+177,"The distance to GoHam is not known precisely, but a value d = 250 ± 50 pc is required to satisfy all the existing observational constraints",2
+178,We here adopt this value with the uncertainty.,2
+179,"Figure 13a shows that this evolution exhibits three distinct phases: (i) the early phase (between t = 0 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 = 250 and 665 s, where the growth rate is slower compared to the linear phase, which is called the Rutherford regime",2
+180,"and (iii) the final phase, which starts at t = 665 s, where the instability suddenly develops in an explosive way, and finally saturates at a later time, which we call the post-Rutherford regime.",2
+181,This model was successfully applied to explain several observed core distances,1
+182,however it is not able to explain all observations,1
+183,"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",5
+184,Other mechanisms proposed are,0
+185,spiral shocks associated with very young binary systems orbiting within a circumbinary disc,0
+186,Recent studies increasing the statistics of sources with detection of molecular outflows have widened the range of measured energetics (e.g.,0
+187,While the Loison et al. (2015) CH3C3N model corroborates the upper atmospheric abundance of C4H3N inferred by,5
+188,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.,6
+189,"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",0
+190,"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.",0
+191,"Even more interestingly, the detection of multi-periodic brightness variations in low-mass WDs",0
+192,"has brought about new classes of pulsating stars known as ELMVs and pre-ELMVs, respectively (ELM and pre-ELM variables, respectively).",0
+193,"Overall, we find that constraints on tides, radius, possible p–g instabilities",5
+194,and the EoS from GW190425 are consistent with those obtained from GW170817,5
+195,For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm−3 is assumed,2
+196,"To convert from surface brightness to density, we use the following widely used approach",2
+197,"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",0
+198,This is consistent with ongoing/recent star formation within the central molecular zone,5
+199,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.,5
+200,"Furthermore, our photometric data also constrain the long-term variability of DES17X1boj to a level below what was seen in SN2009ip",1
+201,and SN2016bdu,1
+202,in the years before the brightest event (MV in range −13 to −14).,1
+203,"The orbit has a period of ∼10 days (typical value of Kepler planets), and it is sufficiently close to the central star to be subject to significant photo-evaporation effect",2
+204,"Using the J0740 proper motion value from Table 1, the Sun’s Galactocentric velocity and the distance (240 km s−1 and 8.34 kpc, respectively;",2
+205,"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.",2
+206,"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",0
+207,suites. These simulations have box sizes ranging from ∼50 to ∼300 Mpc and baryonic mass resolutions ranging from ∼105 to 107 M⊙.,0
+208,"In addition, the linear polarization P.A.s across pulse phase can constrain the beam size and inclination angles, with respect to the pulsar’s rotation axis and our line of sight (LoS). For example, the rotating vector model (RVM) predicts a smooth ‘S’-shape, due to the projected vectors of the magnetic field lines as they sweep across our LoS (e.g.",0
+209,"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.",5
+210,BCGs constitute a special category of objects with peculiar star formation histories (SFHs) seen from both observations,0
+211,and models,0
+212,Studies of SMGs over the past few tens of years have provided valuable insights into their properties. These include,0
+213,merger incidence (e.g.,0
+214,"From the median values of $\bar{\mathcal {R}}_{190814}=7\rm \, Gpc^{-3}\, yr^{-1}$",2
+215,"$\bar{\mathcal {R}}_{\rm 170817}=760\rm \, Gpc^{-3}\, yr^{-1}$, and $\bar{\mathcal {R}}_{\rm 190425}=460\rm \, Gpc^{-3}\, yr^{-1}$",2
+216,we obtain the effective surveyed space–time volumes $VT=1.2/\bar{\mathcal {R}}$ for each of these three events (‘1.2’ is the median of $\mathrm{d}P/\mathrm{d}\mathcal {N}$).,2
+217,"Alternatively, such a change in the PA can be obtained due to magnetic reconnection, e.g. in the ICMART model",1
+218,"where the local magnetic field orientation, which is orthogonal to the wave vector of the emitted photon, itself changes by 90○ as the field lines are destroyed and reconnected in the emission region",1
+219,We used dmcopy tool in CIAO: Chandra's data analysis system,2
+220,"to restrict the energy range to 0.7−7 keV for both imaging and spectral analysis in all of the four data product files: event file, blank-sky observation, RMF and ARF.",2
+221,"Perhaps more customary today, and equivalently, is to introduce a hierarchy of formally independent time variables (e.g.,",2
+222,", so that",2
+223,"In addition, there are no dust condensations along the direction of isolated synchrones, which could have indicated short bursts of activity",1
+224,"or several separated short bursts, as in the case of P/2013 P5",1
+225,The prompt emission of GRB 090709A possibly showed evidence of a periodic signal,1
+226,"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",1
+227,"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.",1
+228,Transit observations with Spitzer,3
+229,"have found a +208 ± 110 ppm difference between the 3.6 and 4.2 μm bands, suggesting CO2 absorption.",0
+230,"While kink waves, both propagating and standing, are routinely observed in the corona (e.g.,",0
+231,The investigations developed by Marcus et al. (2010) and,0
+232,"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.",0
+233,"The use of Planck and WISE data resulted in the discovery of the brightest known, dusty starburst galaxy at z > 1, the “Cosmic Eyebrow”",0
+234,which has also been independently recovered as one of the LPs presented in this survey work.,5
+235,Classical bulges might have formed as a result of,0
+236,multiple minor mergers,0
+237,"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",5
+238,median size – flux relation (black solid lines on the right).,5
+239,"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",0
+240,"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",2
+241,The accretion of gas and the dynamical evolution of BSBHs are likely to be coupled,0
+242,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;,0
+243,The,0
+244,BOSS project,0
+245,obtained additional imaging data of about 3000 deg2,0
+246,"These authors compute the collisional rate coefficients for collisions with electrons, either using perturbation methods such as those used by",2
+247,utilizing the same halo finder as,5
+248,"In this scenario, the present γ-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 ‘leptonic’ models (see also",0
+249,"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 per cent of the diffuse gas luminosity for these high-mass galaxies (see",2
+250,Infrared and submilimetre observations of,0
+251,SN 1987A,0
+252,"confirm the presence of ∼0.1–1.0 M⊙ of dust, indicating that a substantial fraction of refractory elements in their ejecta went to dust grains.",0
+253,"The use of the geodesic equation for a quasi-particle must be questioned, if this particle associates with pure quantum fluctuations",1
+254,While this approach initially appeared to work remarkably well in the case of starburst galaxies,1
+255,"there is now ample evidence that there is no tight universal relation between the UV slope and the attenuation (e.g.,",1
+256,"The LPT for dark matter fluctuations in MG was developed in Aviles & Cervantes-Cota (2017), and further studies for biased tracers in",4
+257,"Among the rich variety of low-frequency waves observed in the Sun’s atmosphere, flare-related quasi-periodic fast propagating wave trains have received much attention",0
+258,Their quasi-periods usually range from 25 to 400 s. These wave trains were,0
+259,and extensively observed in images acquired with the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory (SDO/AIA;,0
+260,"In Table 3 we provide the coordinates, radial velocities, and the sum of the equivalent widths for the cluster member stars, both measured (“m”) and corrected (“c”) to the system of",2
+261,"In this paper, we consider an analysis of the PDF at redshift z = 1 in a survey volume of V = 100(Gpc h−1)3, which is smaller than the effective volume of upcoming surveys such as Spherex with Veff ≈ 150(Gpc h−1)3 and somewhat larger than existing surveys such as BOSS with Veff ≈ 55(Gpc h−1)3",1
+262,"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",0
+263,"At present, data from large-scale spectroscopic surveys",0
+264,"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.",0
+265,"Some studies have indicated that not only [C II] emission is deficient in some sources, but other FIR cooling lines ([O I], [O III], [N II]), as well (e.g.,",0
+266,"In particular, two major categories of MR have been proposed: the steady state model with a single X line and the outflow approaching the Alfvén speed",0
+267,"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˝ = 64) with the help of the Loomis-Wood-type plot technique from the AABS package",7
+268,and SP-FIT/SPCAT program suite,7
+269,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.,3
+270,High velocity outflows from AGN host galaxies have been reported in numerous studies in the literature,0
+271,using optical spectroscopy,0
+272,"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.,",0
+273,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’s Trojan asteroids.,0
+274,Following the method presented in,2
+275,"In L1544, the 14N/15N ratio of several different molecules has been measured:",2
+276,CN/C15N = 500 ± 75,2
+277,"The crystallization age of EC 002 also predates all those of the other dated achondrites, such as",1
+278,and NWA 7325,1
+279,"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",1
+280,"For comparison, to obtain the Hubble Ultra Deep Field (UDF) image, ∼400 hr of actual observation time (∼1 yr in real time) was needed",0
+281,"A tight relationship between O/H and N/O abundances is indeed observed in both H ii regions and local galaxies, especially at M⋆ ≳ 109.5M⊙",5
+282,"Other works report, however, that LiRG can be randomly located in the HRD",6
+283,"The distinction is crucial to understanding the processes that may provide an explanation for the phenomenon,",3
+284,"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.,",0
+285,"Using the relatively strong neutral lines (i.e., “O i” 1355.60 Å and “S i” 1401.51 Å), we also perform an absolute wavelength calibration for the spectra at the “O i” and “Si iv” windows, respectively",2
+286,"Newer, alternate cosmological probes could help alleviate this issue. Recent examples of such probes include",3
+287,QSO angular size measurements that reach to z ∼ 2.7,0
+288,"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 +10216 is large",2
+289,"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",0
+290,"The mean speed of network jets is very similar, as reported in previous works (e.g.,",5
+291,"Theoretical stellar libraries like, e.g.",1
+292,or PHOENIX,1
+293,"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.",1
+294,"The transverse velocities of pulsars (based on proper motion and distance estimates) are particularly large, with a mean close to 310 km s−1",0
+295,"Since for this present UM, the estimation of H0 from CMB alone is compatible with the local estimation of H0 by",1
+296,"thus, we can safely add both the data sets to see whether we could have something interesting.",1
+297,"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.,",3
+298,", which makes these sources good tracers for finding galaxy clusters.",3
+299,"significantly increased the size of LAEs samples used by stacking ≈2000 and ≈4500 LAEs at redshift z ≃ 3 and 2.2 ≤ z ≤ 6.6, respectively.",0
+300,found typical Lyα halo exponential scale lengths of 5–10 physical kpc.,0
+301,"The line force is exerted mainly by the radiation flux in the UV band (200–3200  Å), because the metal lines are densely distributed (e.g.",0
+302,Other studies have used similar methods for budgeting oxygen,0
+303,"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.",0
+304,The dynamics of the cyclotron line was shown to be dependent on the luminosity state of XRPs (see,0
+305,for review).,0
+306,The term φi + 1/2 is the so-called flux limiter,2
+307,"A large proportion of the spiders, whether BWs or RBs, have been observed to exhibit (quasi-)periodic eclipses of the pulsars’ radio emission (e.g.",0
+308,that are generally attributed to excess material in the orbits,0
+309,interfering with the propagation of the radio emission.,0
+310,"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.",3
+311,This basic idea has allowed the development of global “Enthalpy-Based Thermal Evolution of Loops” (EBTEL) models that describe the evolution of the average temperature and density in the coronal part of the loops;,0
+312,these models are generally in good agreement with one-dimensional hydrodynamic simulations,5
+313,"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.",1
+314,"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–Heitler (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.",1
+315,whereas KEPLER was used to evolve the star along zero age main sequence and calculate nucleosynthesis yields and light curves,2
+316,"The observational analysis of PDRs, H II regions, and IBLs has improved considerably since the availability of far-infrared spectroscopic data from the Herschel Space Observatory (see",0
+317,"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",1
+318,An individual star-forming galaxy is expected to evolve along the relation of star-forming galaxies in the mass–size plane,0
+319,while the average size of the population as a whole increases with decreasing redshift due to processes such as mergers,0
+320,and ’puffing up’ due to strong active galactic nuclei (AGNs) feedback,0
+321,but also new galaxies forming with larger radii,0
+322,These outflows can explain the nearly constant temperatures inferred from the spectrum of optically bright TDEs,5
+323,There is evidence for a few additional smaller shock fronts throughout the cluster volume,0
+324,"In support, observations of V404 Cyg do indicate the source",5
+325,and was enshrouded by rapidly varying Compton-thick outflowing material,5
+326,We segmented the sky into equal-area pixels using the HEALPix scheme,2
+327,"The derived central engine parameters are sometimes ad hoc or inconsistent. For instance, the analyses",1
+328,and for GRB 130427A,1
+329,"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.",1
+330,"Conversely,",6
+331,observe two sequences in the inner regions.,6
+332,The thermal emission from the aligned dust grains is then polarized with polarization segments perpendicular to the field lines,2
+333,The two coherent emission mechanisms are,0
+334,and electron cyclotron maser (ECM) emissions,0
+335,"Nevertheless, there are examples of weakly magnetized WD pulsars, which can be explained even in the GR framework, e.g.",1
+336,and AR Scorpii,1
+337,where magnetic fields hardly affect their mass–radius relations.,1
+338,"Both categories of method have been applied to large stellar spectroscopic surveys, including",0
+339,RAVE,0
+340,"A similar decrease of eZ,rel,int with increasing mass is found for the bulk metal content of Solar System giants",5
+341,"where the mass where eZ,rel,int reaches 1 is extrapolated to be at about 11 MJup.",5
+342,The scaling laws derived from the numerical simulations of downward overshooting,5
+343,agree well with Zahn’s analytical model.,5
+344,"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",1
+345,The resulting gas density probability distribution function,2
+346,with an additional few per cent of the mass in a power-law tail at high density,2
+347,This discrepancy in results might originate in the nature of the collisions studied in these different experiments:,1
+348,"and Higa et al. (1996) performed collisions of a particle with a flat surface, while Heißelmann et al. (2010) observed particle-particle collisions in a free-floating environment.",1
+349,The minimum gap-opening mass depends on the viscosity and scale-height of the disc,0
+350,or even Earth-mass planets,0
+351,could produce detectable gaps.,0
+352,"We confirmed that this is indeed negligible for [O i] 6300 Å 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 Å measurements were consistent with values determined using other methods",5
+353,Among the better recent claims of QPOs in the gamma-ray band are of,1
+354,and of ∼71 d in the blazar B2 1520+31,1
+355,found as part of a continuing analysis of blazar Fermi–LAT observations.,0
+356,"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−1 to coincide with observations",0
+357,Previous studies have considered the implications of structure models,0
+358,on the shape of the afterglow light curve,0
+359,coronal dissipation fraction fc ≈ 0.45,2
+360,"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",1
+361,"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.",1
+362,According to recent theoretical analyses of gap structure around a planet,0
+363,"the depth and width of the gap are controlled by the planetary mass, the turbulent viscosity, and the gas temperature.",0
+364,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),0
+365,MBHBs are in fact expected to emit a large amount of EM radiation in different bands,0
+366,and possibly even through pre-merger signals,0
+367,The distance of this source is around d ∼ 11 kpc,2
+368,Many studies suggest that BH growth precedes spheroid assembly,1
+369,"however, other studies find no significant evolution with redshift (e.g.",1
+370,Electrostatic solitary waves have been observed in Saturn’s magnetosphere,0
+371,"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",7
+372,the direct comparison of bulge stars with similarly metal-rich GCs on the Na–O plane would require further spectroscopic observations for such GCs in the bulge.,7
+373,"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",0
+374,"Vázquez-Semadeni, González-Samaniego & Colín (2017) have recently shown that the simulations of Colín et al. (2013) in fact produce stellar age histograms highly resemblant of the observed ones",5
+375,"On the other hand, the discovery of isolated L dwarfs in young clusters",0
+376,"and very cold very nearby Y dwarf objects (e.g.,",0
+377,show that very low-mass isolated brown dwarfs exist and overlap with the planetary masses.,0
+378,Alternative mechanisms such as,0
+379,shocks from supernova remnants,0
+380,are often invoked.,0
+381,"Based on this evidence, Troja et al. (2017) suggested that a structured jet model (e.g.",2
+382,"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",2
+383,"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.,",3
+384,X-ray reverberation in black hole X-ray binaries was first robustly detected in GX 339–4 by,0
+385,when the source was in its hard state.,0
+386,and fit Kurucz ATLAS9 stellar atmosphere models,2
+387,Such mini-outbursts or night-side activities have been observed before at,0
+388,and comet 103P/Hartley 2 by the EPOXI mission,0
+389,"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",2
+390,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,1
+391,"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 ≈ 107°) with a full-width at half-maximum (FWHM) size of roughly 0.8 × 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 × 1.1 pc and elongated along PA ≈ 46°",0
+392,and in the seeding of large-scale magnetic fields in the universe (e.g.,0
+393,"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",5
+394,The properties that make RR Lyrae standard candles are,0
+395,the period–luminosity relation in the near-infrared (NIR) filters and in particular in the K 2.2 μm band (see e.g.,0
+396,"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",7
+397,"This is basically consistent with the detection rate and the distance distribution of BH–NS merger candidates detected during LVC O3 (e.g.,",5
+398,"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;",0
+399,Even though arguments,6
+400,microlensing,6
+401,"exist that favour a compact corona, we used extended coronae.",6
+402,Stringent non-detections in radio,0
+403,observations exclude nearby CSM at high significance.,0
+404,"Mid-IR (MIR) and far-IR (FIR) observations have revealed bright atomic lines from H ii regions ([S iii], [Ne iii], [Ne ii], [O iii], etc.) and PDRs ([C ii], [O i]) (e.g.,",0
+405,"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 Å, the Fe ii lines at 1353.02 Å, 1354.01 Å, and 1354.75 Å, the Si ii lines at 1352.64 Å and 1353.72 Å, and the unidentified lines at 1353.32 Å and 1353.39 Å (e.g.,",0
+406,"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",0
+407,For the regression the mpfit library,2
+408,"was used, with the variable errors handled according to York (1966) in the implementation of Tellinghuisen (2020).",2
+409,"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",0
+410,"We use a fully coupled ocean model because alongside atmospheric heat transport, ocean heat transport plays a vital role in the climate of Earth",2
+411,"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",1
+412,"The first identified phosphorus compound in the ISM was PN through observations of its rotational transitions in Orion-KL, W51M, and Sgr B2",0
+413,"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",5
+414,"For the X-ray data, we use",2
+415,the Chandra 4 Ms source catalog in the CDFS field,2
+416,The typical sensitivity limits of these X-ray data are,2
+417,∼10−17 to 10−16 erg cm −2 s−1 for the CDFS and HDFN fields.,2
+418,"However, the virialization of dark matter perturbations in the non-linear regime cannot be independent from the properties of DE",2
+419,This correlates with the analysis,1
+420,"which demonstrated that the preliminary track annealing led to unpredictable changes in track lengths, resulting in a lower accuracy of nuclear charge determination.",1
+421,"For SIBEC-DM given by the field Lagrangian in Eq. (1), the self-interaction is constrained to Rc  1 kpc, otherwise an early radiation-like period and a large comoving Jeans’ length washes out too much structure to be consistent with observations",1
+422,This stochastic acceleration process typically causes the particle distributions to have a pronounced curvature in the energy spectrum,2
+423,see fig. 5 from,2
+424,"Due to its simplicity and in order to allow comparison with previous work (e.g.,",1
+425,"), we used the cutoffpl model for all subsequent analysis.",1
+426,"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)",0
+427,"The dashed blue line is the limit above which a halo must grow in order to overwhelm the impact of LW radiation, Mmin, LW",2
+428,Using Eq. (1) from,2
+429,", we derived the precession time of T ≈ 530 yr.",2
+430,This value is quite large for the wiggling waves that we see.,1
+431,"Such a gap could be opened by a super-Neptune-mass planet, depending on the parameters of the disk, such as the turbulent viscosity",1
+432,"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.,",3
+433,"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",0
+434,"If there is no break in the spectrum, the energy budget for these particles would be untenable",1
+435,This electric field is generated by the density gradient and different mobilities of electrons and ions,2
+436,"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",3
+437,", leading to a lower critical dose in the case of mixed hydrogen and helium exposure",3
+438,"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.",0
+439,interferometric observations in the (sub)millmetre domain,0
+440,"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 10−25 to 10−15 nG",1
+441,"From observations, field stars in dwarf galaxies do exhibit different abundance ratios from MW field stars, e.g. lower [α/Fe] ratios and variations in neutron-capture element ratios at intermediate metallicities. However, these typically do not show up until [Fe/H] ∼ −1.5",0
+442,"Since 2006, it has been suspected that mergers of compact objects could also produce the so-called long–short 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",0
+443,"Interesting explorations on the origin of PCEB (and specifically sdB+MS/BD) circumbinary planets can be found in Zorotovic & Schreiber (2013),",0
+444,"Bear & Soker (2014), and Völschow et al. (2016).",0
+445,"In fact, the E0 distribution for the high κ solution is qualitatively similar to the FIDO one",5
+446,which according to,2
+447,is about of 0.5−1 Gyr after the merger,2
+448,"Secondly, there is growing evidence that the mass of any classical bulge, if present in the Milky Way, must be small",0
+449,"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).",3
+450,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.,0
+451,"In our MHD simulations, βrot is adopted to be 0.4% based on the observational estimates of the core mass of ∼1 M and the angular speed of the core rotation of 4 × 10−14 s−1. The angular speed was estimated based on the global velocity gradient along the major axis of the dense core observed with single-dish telescopes",2
+452,"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",1
+453,Theorem 18.29,1
+454,The Artificial Neural Networks (ANNs) have found application in not only the traditional tasks in extragalactic astronomy,0
+455,but also in more specialized problems such as,0
+456,estimation of star formation properties,0
+457,"In the visual passband, the luminosity L depends on Z in the form of the so-called RR Lyrae luminosity–metallicity relation (see e.g.",0
+458,"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",1
+459,"We approximate the NS as a polytropic star of index n = 0.5 (e.g.,",2
+460,The turning point of increased relative production of carbon from massive stars takes place at A(O) ~ 8.7 dex (see Fig. 2 of,1
+461,which equals to [O/H] ~ 0.0 dex.,1
+462,"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).",6
+463,"and that of the gamma-ray emission about the hadronic process have been also investigated (see, e.g.,",0
+464,"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.",3
+465,The JAGUAR catalogue provides emission line fluxes and EWs for the main lines based on modelling with the beagle code,2
+466,"Toward this goal, conventionally, new summary statistics that can only be measured with imaging have been proposed. These include the three-point correlation function",0
+467,"Direct detection of progenitor stars is still elusive for SNe Ic, which prevents us from further testing the theoretical evolution of massive stars",0
+468,FTD models driven only by the Babcock–Leighton mechanism,5
+469,currently have the best agreement with observations,5
+470,because the length of the simulated overlap is short and it occurs only during the minimum at low latitudes.,5
+471,"In some sources it has been found that coronae can have extremely high energy cut-off (e.g. NGC 5506,",0
+472,"and therefore thermal energy, which is inferred by measuring the curvature of NuSTAR spectra at high energy and in this context K–N effects cannot be neglected.",0
+473,"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",3
+474,"Therefore, they can be considered as better candidates for the formation of complex organic molecules with longer carbon chains.",3
+475,"As of today, many more mass ejection channels have been discussed: matter that becomes unbound on secular time-scales (∼1 s) from the post-merger accretion torus",0
+476,and do not fully rule out a spatially non-flat Universe,1
+477,"Meanwhile, enormous efforts have been made to refine the reaction rates of key BBN reactions in the past 20 yr",0
+478,but the probability of solving or alleviating the 7Li problem by improving our knowledge of relevant nuclear reaction rates still cannot be eliminated.,3
+479,The comet's surface revealed a wide diversity in morphology such as layering,0
+480,The morphology resulting from this particular type of wind–binary interaction is shown in Fig. 3 in,0
+481,"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.,",0
+482,"The key achievement of LPF was placing two gold-platinum cubes known as “test masses” into a freefall so pure that it was characterized by accelerations at the femto-g level (e.g.,",0
+483,the level required to detect the minute disturbances caused by passing gravitational waves.,0
+484,"Grillo, Lombardi & Bertin (2008) introduced a methodology to estimate cosmological parameters using strong-lensing systems (SLS; see also",0
+485,"However, if a single stellar loop were flaring, the cooling time of the confined plasma would be proportional to the loop length",2
+486,"However, the discovery of ubiquitous propagating transverse oscillations with CoMP",0
+487,and SDO,0
+488,"led to the possibility of continuous diagnostics in time, i.e., dynamic coronal seismology.",0
+489,"Because of the faintness of the transient and its proximity to the larger, brighter main source, an automated detection algorithm such as SExtractor",2
+490,"implemented in GAIA36 2016A, was unsuccessful in deblending the two sources.",1
+491,"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.",0
+492,Simultaneous observations were made with,2
+493,the Swift UV/Optical Telescope (UVOT;,2
+494,with the u filter applied.,2
+495,Especially for late M dwarfs the cut-off at 4.545 μm leads to non-negligible loss in incoming radiation of up to ≈5% (see also,2
+496,"Hence, HZ boundaries obtained with the models lie closer to the star than would be expected when accounting for this missing portion of irradiation.",2
+497,"Particles up to gigaelectronvolt energies are accelerated by strong shocks driven by CMEs of very high speeds (∼2000 km s−1) and intense, soft X-ray flares (see",0
+498,"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",0
+499,"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.,",3
+500,"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",2
+501,"In Table 3 we provide the coordinates, radial velocities, and the sum of the equivalent widths for the cluster member stars, both measured (“m”) and corrected (“c”) to the system of",2
+502,This type of geometric configurations for the BBH–disk accretion systems has been revealed by many numerical simulations and analysis,0
+503,Local thermodynamic equilibrium (LTE) is a good approximation for the H2CO level populations under optically thin and high-density conditions,2
+504,"For comparison, we show in Fig. 13 the predictions of the most recent one",1
+505,where the updated nuclear reaction network was used.,0
+506,"This is consistent with the ${\approx } 30\, {{\rm per\, cent}}$ amplitude modulations observed in the source at 3 GHz",5
+507,being caused by refractive interstellar scintillation in the Milky Way interstellar medium,5
+508,The previously reported anti-correlation between tdepl and sSFR,5
+509,"is also further supported by our galaxies at z = 4.4 − 5.9 (Fig. 6, middle panel).",5
+510,"Our numerical experiments, however, do not seem to support claims of the steepening of the R ∝ Mα relation for CGs towards values α ≳ 1",6
+511,"Our results appear to stand apart from similar studies in full spherical shells (e.g.,",6
+512,in that the differential rotation is strongly quenched as a function of the magnetic Reynolds number.,6
+513,We calculate this by using the slug stellar population synthesis code,2
+514,We use the $\mathcal {N}_\mathrm{LyC}$ for each H ii region as determined from the radio observations outlined in Table  2 (i.e.,2
+515,and solve for the direct radiation pressure using equation (4).,2
+516,"However, uncertainties on the observational and theoretical sides mean that the true level of disagreement is unclear. For example, while",1
+517,"derived a PN abundance of 10−8 relative to H2 in IK Tau, De Beck et al. (2013) and Velilla Prieto et al. (2017) derived higher abundances, (3–7) × 10−7, in this source.",1
+518,"Then, we consider the REFLKERR where the hard X-ray Comptonisation spectrum is computed with the COMPPS model",2
+519,which appears to be a better description of thermal Comptonisation when compared to Monte Carlo simulations,1
+520,"We derive a ratio ∼0.05, which is very similar to the average ratio derived in the disc of M 31 (see e.g.",5
+521,Supervised learning has been used,0
+522,and to determine the redshift of galaxies,0
+523,"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",0
+524,The left-hand panel of Fig. 2 shows sources from Gaia’s DR2 LPV catalogue,2
+525,chosen to lie within a 15° aperture of the LMC.,2
+526,Recent results from solar flares observed from space,0
+527,demonstrate an NUV spectrum originating largely from Hydrogen Balmer continuum emission.,0
+528,"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",1
+529,"Note that the minimum value of the drag parameters we used here is 1 × 10−9 km s−1, which was revealed as the lowest possible value",2
+530,"Nevertheless, an early ROSAT observation of the old open cluster M 67, which lies at ∼840 pc",0
+531,Earlier observations of the physical sizes of SMGs by CO detection and 1.4 GHz imaging suggest larger sizes (e.g.,1
+532,These low ratios are consistent with the values found for several other stars with strong chromospheric activity,5
+533,"For instance, shallow gradient in metallicity is seen in SBS 0335−052 (",1
+534,while no significant variations were seen in Mrk 35,1
+535,"However, our result is consistent with other NLFFF results",5
+536,"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.",0
+537,"Although the current corotation radius is rco ≈ 2.25 RJ, Jupiter at its time of formation was much larger than it is today",2
+538,"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.",2
+539,TDSs are also expected along the Parker Solar Probe orbit,0
+540,The consideration of ambipolar diffusion processes in solar physics started many decades ago,3
+541,but it has undergone a true explosion in terms of its use in large numerical models (e.g.,3
+542,"Such numerical calculations often encounter a problem: given the comparatively high values of χa 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 ηa.",3
+543,"For this reason, we obtained a considerable amount of biases (150−300 frames) and twilight flat-fields (25−100 frames) each night to reduce the Poisson noise to less than 0.2 mmag",2
+544,"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",0
+545,Most studies to date find that cusp-core transformations are challenging at the likely mass-scale of UFDs (M200c ∼ 109 M⊙; M* ∼ 105 M⊙; e.g.,1
+546,"However, different works used different mono-energetic bins to represent this channel, e.g.,",6
+547,2.5 GV,6
+548,This is probably ram pressure caused by the relative motion of galaxies with respect to the ICM,0
+549,"The influence of tidal truncation is therefore limited to stellar multiples, either in bound systems",0
+550,"The fitted radio spectral index α1 from this study is −0.53 ± 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 −0.58 (e.g.",5
+551,"Along with an increasing number of observational cases, the study of fast kink oscillations in coronal loops has been significantly advanced",0
+552,see Figure 8 for a comparison of the arc redshift distributions adopted by the pre-HFF and new HFF+ lensing models;,2
+553,We also used some observational data obtained within several other programmes,2
+554,It has only recently become widespread to model the formation of galaxies ab initio (e.g.,0
+555,"Currently, a limited number of observations",0
+556,"are available to explore the environment dependence of the metallicity, and most of our current understandings are based on simulations",0
+557,"Several solutions have been successfully proposed in order to deal with stellar oscillations and granulation phenomena, such as:",0
+558,"using daytime spectra of the Sun in order to measure the solar oscillations (e.g.,",0
+559,"This picture is consistent with the observed low temperature, large radius, and super-Eddington luminosity (see",5
+560,"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",1
+561,"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",0
+562,This image reconstruction problem inspired several computational approaches like,0
+563,and machine learning,0
+564,Interstellar scintillation (ISS) is difficult to distinguish from intrinsic variability without fully time-resolved data (see e.g.,1
+565,"and references therein), and can coexist with it",1
+566,"However, to obtain precise photometric transit and spot parameters, we recommend the use of a planetary pixel radius between 15 and 50 pixels",2
+567,From the IPAC forced-photometry service,2
+568,"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 σpix on the background at the pixel on which the SN is located.",2
+569,A large number of kinematic arches with various morphologies not known prior to Gaia were found,0
+570,"In parallel, theoretical works and simulations have tried to explain the physical mechanisms that reproduce the measured global properties",0
+571,"In Equation (3), ΔE 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−1 as measured by Voyager 2, whereas uR = 40 km s−1 for the heliosheath in the Voyager 1 direction",2
+572,Solar wind velocity distribution moments are described in,0
+573,"The constant, 4.64, is the r-band magnitude of the Sun in the AB system",2
+574,Assuming the width of the gaps corresponds to 4RHill,2
+575,"On the contrary, ground-based telescopes usually have instruments which can cover several spectral lines simultaneously, e.g.",1
+576,Gregor/GRIS,1
+577,"One of the major error sources is the uncertainty in ξ in various studies, including ours, based on spectra at different wavelengths",2
+578,to the H band,2
+579,"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",0
+580,"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 KROME",2
+581,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,2
+582,we conclude that the star-spot signal cannot be originating on the secondary component.,2
+583,"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",0
+584,"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 Myr of Solar system history",1
+585,"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 km and above the detection limit.",1
+586,The first study to determine masses for a sample of metal-poor halo giants with both seismic information,0
+587,and chemistry from high-resolution APOGEE,0
+588,"spectra, was by",0
+589,The authors used scaling relations at face value and reported masses larger (M >  1 M⊙) than what would be expected for a typical old population.,0
+590,"Similar results were obtained by Casey et al. (2018), also using scaling relations for three metal-poor stars.",5
+591,These findings led to the need for further tests of the use of asteroseismology in the low metallicity regime.,0
+592,"Theoretical stellar libraries like, e.g. BaSeL",1
+593,"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.",1
+594,"However, since such diagnostics usually involve the [N ii]/[O ii] or the [N ii]/[S ii] 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",1
+595,"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),",2
+596,", Kerszberg (2017) over broken power-law models derived from the fits to lower energy data.",2
+597,"NATs, which are especially common in clusters, (e.g.,",0
+598,"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.",0
+599,"The number of convincing dual AGN systems, mostly detected by X-ray and radio observations (e.g.,",6
+600,are relatively few compared to the theoretically predicted abundance,6
+601,Mass–radius relation is employed to estimate radius in case of white dwarfs and neutron stars (see e.g.,2
+602,We convert the ASAS-SN distributions into estimates of the true luminosity function using the V/Vmax method,2
+603,Subsequent studies found the same trend of [α/Fe] with mass,0
+604,"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 α 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.",0
+605,"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",0
+606,The quasar survey data are also used for studies to constrain cosmological parameters,0
+607,"We make the simplifying assumption that the cloud temperature does not vary with radius; for solar composition, photoionization equilibrium is achieved at temperatures T ∼ 104 K across a wide range of ionization parameter (equation 5), and the gas temperature will therefore vary weakly with radius (e.g.",2
+608,or parametric equations tuned by direct comparison with the outcome of numerical simulations of collisions of live galaxy pairs (e.g.,0
+609,"Regarding the radiation-hydrodynamic evolution, the conservation equation $\Delta_\alpha T^{\alpha \beta }_{\rm (total)}=0$ is solved using the piecewise parabolic method",2
+610,Other sources of dark energy include scalar fields such as,0
+611,and phantom fields,0
+612,"Usually, the downstream sheath regions have larger density, temperature, mean magnetic intensity, and compressibility, and higher plasma β, as compared to the upstream solar wind",0
+613,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.,1
+614,"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.,",1
+615,"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.",1
+616,The sample of,1
+617,"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.",1
+618,The dimensionless accretion rate,2
+619,and black hole mass of the source are $\log (\dot{\mathscr {M}})$ = $2.63^{+0.16}_{-0.67}$ and log (MBH/M⊙) = $6.78^{+0.31}_{-0.06}$ with the reverberation mapping technique,2
+620,"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.",2
+621,"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",1
+622,"Then, interestingly, it followed by the quadruple radiation of the standing accretion shock instability",5
+623,"signal, which was suggested to be seen in the GW data",5
+624,"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",0
+625,", motivated by the knowledge of surface brightness dimming (1 + z)4.",0
+626,"In empirical methods this application is more straightforward, since algorithms are constructed such that it is not difficult to add extra input parameters.",3
+627,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,2
+628,"For βapp and δvar we used the fastest measured radial, non-accelerating apparent jet speed from the MOJAVE kinematic analysis",2
+629,"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.",0
+630,"Since CVs are intrinsically rather faint (typically, MV > 4 mag; e.g.",2
+631,", in general the correction for the interstellar extinction will represent an upper limit.",2
+632,"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−1), reported in at least ∼36% of AGNs",1
+633,"see also, e.g.,",1
+634,"Along the dust lane of the elliptical galaxy, there is a molecular gas component of mass ∼109 M⊙ as probed by various molecular lines",0
+635,"Note that the perpendicular heating rate is a nonnegligible fraction of that observed in the solar wind, where",2
+636,"If f > fm, the index of the power-law relation between A(f) and f changes",2
+637,and is beyond the scope of this study.,7
+638,Entire sample is shown in Toomre Diagram of rotational velocity (VLSR) and sum of quadrature of radial and vertical velocities ([$\rm {\it U}_{\rm LSR}^2 + {\it W}_{\rm LSR}^2]^{1/2}$),2
+639,"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.",0
+640,"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",1
+641,"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 Å) is determined by averaging the line centers of the Fe XXI profiles which were used in the previous IRIS observations",2
+642,", while the rest wavelengths for the C i and Si iv lines, i.e., 1354.29 Å and 1402.77 Å, respectively, are determined from their quiet-Sun spectra",2
+643,"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.",0
+644,"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 (≥10 M⊙) and is therefore nearly independent of the evolution of LIMS, the progenitor stars of PNs",0
+645,"Assumption of the thermal blackbody radiation could overestimate the emissivity of ionizing photons at Z ∼ Z⊙ owing to the line-blanketing effect, especially for stars with M* ∼ 10 M⊙ (e.g.",2
+646,"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;",0
+647,"Such surveys also provide key spectral and orbital characterisation data for known exoplanets (e.g.,",0
+648,"were used as inputs for the turbulence quantities (e.g.,",0
+649,"Furthermore, mean free paths such as those discussed have,",5
+650,"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",1
+651,"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",1
+652,"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",5
+653,the study of binary systems such as eccentric MSPs like PSRs J1903+0327,3
+654,which are interesting due to their peculiar binary evolution,3
+655,"To confirm the importance of VO, water and an inversion layer",0
+656,obtained repeated HST observations of the transmission spectrum and the secondary eclipse using the STIS and WFC 3 instruments.,0
+657,"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× to 30× 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.",1
+658,This resulted in,0
+659,"formation of globally unstable disks, and radial gas transport by dynamical friction",0
+660,"A tight relationship between O/H and N/O abundances is indeed observed in both H ii regions and local galaxies,",2
+661,"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 ‘secondary’ nitrogen production mechanism,",2
+662,"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",3
+663,We predict the noise in the Planck lensing map assuming the detector sensitivity and beam sizes listed in the Planck Bluebook,2
+664,The FNm can be written explicitly as an integral over the eccentric anomaly,2
+665,"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.",2
+666,"The second issue is the pseudo- versus classical bulge argument – 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",1
+667,"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.,",0
+668,"The luminosity during the 2020 giant outburst reached a record high, which was significantly higher than the critical luminosity",0
+669,"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 γ measurements",0
+670,Cepheids have also been found to show additional complications that include cycle-to-cycle variations in their light and radial velocity curves (see,3
+671,"It is of importance to planned future surveys to investigate suitable strategies for source-finding in linear polarization with interferometers such as LOFAR,",0
+672,and with the ability to make precise Faraday rotation measurements,0
+673,"Specifically, we use m* values computed from Bruzual & Charlot (2003) models in the same fashion as described in previous SPT publications",5
+674,"The warm Neptune GJ436b, which is the lowest mass planet found evaporating to date",0
+675,"), shows transit absorption depths up to 60% in the Ly-α line.",0
+676,"Semi-analytic modelling is a particular simulation method which is optimized to connect the observed properties of the galaxy population – abundances, scaling relations, clustering and their evolution with redshift – to the astrophysical processes that drive the formation and evolution of individual galaxies (e.g.",0
+677,Minima and transition states (TSs) were optimized using the DL-FIND,2
+678,program of the ChemShell suite,2
+679,"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",0
+680,"which suggests that at least some FRBs originate from magnetars born from the core collapse of massive stars (e.g.,",3
+681,"Approaches of this type are widely used in astronomy, for example to infer star formation histories or stellar mass distributions from observed colour–magnitude diagrams (CMDs; e.g.",0
+682,Infalling and rotational motions on scales from 100 to 3000 au have been observed in molecular lines with single-dish telescopes and interferometers,0
+683,This must typically be done with a numerical Poisson solver,2
+684,discussed four estimators which attempted to correct for biasing in the degree of linear polarisation in the presence of low signal-to-noise ratios.,0
+685,"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.,",1
+686,Three events (Swift J1644+57;,1
+687,have isotropic ∼5 GHz luminosities of between 1040 and 1042 erg s−1 whereas the rest,1
+688,"have luminosities in the range 1037 to 1039 erg s−1 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.",1
+689,The sequence of dwarf and giants from,2
+690,"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)",2
+691,"Given this deficit, we provide only a simplified estimate using radial velocities of OBA-type stars from",2
+692,"Since they belong to the same young population, we assume that they have a similar distance distribution and kinematics as the Cepheids.",1
+693,"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",0
+694,"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",2
+695,"Velocity fluctuations have been studied thoroughly (see, e.g.,",0
+696,"although the kinetic scales still remain quite unexplored for instrumental limitations, most notably in the sampling time resolution.",7
+697,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,5
+698,Orbiting SMBHBs produce a,0
+699,and transient GW bursts,0
+700,The relevant methodology is straightforward and well established. One needs to calculate the likelihood function of the data given the model – namely the probability of the occurrence of the data within the framework of the assumed model,2
+701,"However, an optimal metric – expressed as an entropy functional – is not known in advance and therefore needs to be chosen individually",2
+702,"For the SPT-SMGs, we used the sizes of",2
+703,"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 (6–10 K for olivine grains)",0
+704,In the magnetically arrested disk,1
+705,"scenario, the MRI and subsequent turbulence in the inner accretion disk are suppressed due to large-scale magnetic flux (see, e.g.,",1
+706,Plenty of simulation works,0
+707,"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.",0
+708,"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 ‘thermal’ events and rarer relativistic jets. Three events (Swift J1644+57",0
+709,have isotropic ∼5 GHz luminosities of between 1040 and 1042 erg s−1,0
+710,"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.",0
+711,"On the other hand, long-duration gamma-ray bursts (lGRBs",0
+712,are associated with the core collapse (CC) of dying massive stars,0
+713,leading to supernovae (SNe;,0
+714,Recent advances in understanding the properties of magnetohydrodynamic (MHD) turbulence,3
+715,stimulate a renewed investigation on density statistics,3
+716,Many studies of individual galaxies,0
+717,"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 = 1−0.",0
+718,The fewer radio studies of RQ AGN,3
+719,"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.",3
+720,The estimated continuum slope is consistent but somewhat flatter than the typical slope of luminous quasars,1
+721,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,0
+722,Recent data from the Gaia mission,3
+723,"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.,",3
+724,The full particle simulations are performed using,2
+725,and NPIC code,2
+726,"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.",0
+727,"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.",5
+728,"Dynamic ocean heat transport on completely ocean-covered worlds (i.e., no continents) leads to warmer global mean temperatures and a reduction in day–night temperature differences on synchronously rotating planets",3
+729,"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.",7
+730,"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",2
+731,"The geometrical thickness of the disk scales with the radius R following a (slightly) different relation; it is proportional to R−21/20 in the inner Thomson scattering-dominated, regions and to R−9/8 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 Ṁin and assuming the same value for α in both equations. We found Rjump between 3 × 104 RG and 7 × 104 RG in all the epochs considered.",2
+732,"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",0
+733,"using various radiative transfer codes, such as",0
+734,MARCS,0
+735,"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",0
+736,"supporting instead the idea of possible central star formation, it seems unlikely it can develop such steep profiles.",5
+737,"Traditionally, bulges were thought to invariably form early-on via",0
+738,or mergers,0
+739,with the disk gradually building up around them.,0
+740,"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.",1
+741,In transition regions from diffuse ISM to dense clouds,0
+742,"\hbox{$0.7 \leqslant A_{V} \leqslant 1.2$}0.7 ⩽ AV⩽ 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 → 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.",0
+743,"They exploit the maps with different apertures and efficiencies and are applied individually or combined together, even with different weights (see e.g.",1
+744,The authors used their new results together with,0
+745,and low-redshift reference data for the Coma cluster,0
+746,to further solidify the evidence supporting passive evolution and a formation redshift zform ≈ 2.,0
+747,"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.,",0
+748,which provide the initial condition of star formation.,0
+749,"Such transition might well imply an imminent increase of the SFR, driving the object in the realm of starbursts",1
+750,"or its cessation, bringing the system back onto or even below the main sequence",1
+751,with the CO properties potentially able to distinguish between these two scenarios.,7
+752,and the magnetic field can exceed 0.15 T in both the intranetwork and the network quiet region,2
+753,While the universality of the latter finding is in doubt,3
+754,it certainly introduces very important subtleties to the old paradigm,3
+755,The most recent spectroscopic study is from,0
+756,who reinvestigated the internal rotation measurements and also determined hyperfine coupling parameters due to the nitrogen quadrupole,0
+757,"Gas masses can also be estimated with an empirically calibrated relation between single-band dust continuum flux at the Rayleigh–Jeans (R-J) tail and gas mass (e.g.,",0
+758,"These scaling relations are calibrated with local galaxies or with local galaxies and SMGs up to z ∼ 2. In this method, the gas-to-dust mass ratio is included in the conversion factor, and therefore does not need to be considered.",0
+759,It remains unclear whether the empirical calibration methods are applicable to galaxies at z > 3 or how much scatter there is in the relationships.,1
+760,"The catalogue explores a wide range of linear diameters and masses, from sub-parsec (≤ 0.1 pc) to parsec scale (1−5 pc) with masses from 1 M⊙ to 105M⊙. 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",2
+761,Compact BH jets show an LX–LR correlation across ∼eight orders of magnitude in X-ray luminosity,0
+762,"a subset of sources follows a radio-bright correlation with a power-law slope of β ≈ 0.6 (where $L_R \propto L_X^{\beta }$, while others follow a steeper correlation with β ≳ 1 at high X-ray luminosities, before re-joining the other track around LX ≈ 1035 erg s−1 (e.g.",0
+763,"This is not the Kozai–Lidov resonance; in this case, the Kozai–Lidov domain (domain II in",1
+764,is characterized by libration around $\omega _{\rm r}=0{^\circ }$ (or 180°) which is only briefly observed at the end of the backwards integrations,1
+765,see Fig. 6,2
+766,"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",2
+767,"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.",0
+768,"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",1
+769,"To illustrate this, we show examples of calibration vectors for SDSS",2
+770,eBOSS DR14,2
+771,We also plot the results of previous blank-field surveys,2
+772,"For example, Chen et al. (2016) and",0
+773,have produced filament catalogues in the SDSS,0
+774,This ‘funnel’ accretion scenario is also found in other simulations with a spherical-like distribution of rotationally accreting material,5
+775,"At later times, the spectrum depends on the seed photon spectra, but it can roughly be estimated to be a flat spectrum from ∼1 eV to ∼0.1 TeV, while the supernova emission continues, which is expected based on more detailed calculations (e.g.,",2
+776,"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",0
+777,"Recently, Fernández-Martín et al. (2017) reported a slope of −0.108 ± 0.006 dex kpc−1 using optical spectra for H  ii regions located at RG between 5 and 17 kpc. That value of the slope is considerably much steeper than our determination and other previous estimates from the literature (e.g.",6
+778,"In view of the fact that the limiting magnitude of the follow-up wide-field survey projects is almost ≲21 mag (e.g.,",2
+779,"the maximum detectable distance for BH–NS kilonovae would be ≲200 Mpc, which can hardly cover the horizon of GW-triggered BH–NS merger events that O3 found (as shown in Figure 10).",2
+780,"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",0
+781,"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.,",0
+782,"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.",3
+783,"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",5
+784,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).,5
+785,"The dispersion relation of strong electromagnetic waves is altered due to the effective electron mass increased by the relativistic effect (e.g.,",2
+786,"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",0
+787,It is worth noting that the “head-to-tail” scenario seems to support the idea that the filament is supported by sheared arcades,1
+788,"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.",0
+789,The quantitative estimation of the radiated flare energy partition suggested about,0
+790,"and 55%–80% in WL for stellar flares (e.g.,",0
+791,"The nuclear semi-relativistic phase and the galaxy-scale molecular phase have been observed simultaneously in less than a dozen sources, with varied results:",0
+792,in other cases data suggest momentum driven flows (e.g.,0
+793,The growth of dust grains through accretion in the ISM has been proposed as a solution (e.g.,0
+794,"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",1
+795,"Efforts have been made in quantifying mass, star formation rates, gas composition, and kinematics, as well as other LAE properties (e.g.,",0
+796,"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 1138−262 from this point of view as well",3
+797,"As a result, optical studies have produced the largest number (∼1200) 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 ii]/H α > 0.4–0.5",0
+798,"This calibration is relatively insensitive to changes in gas pressure or ionization parameter, and we adopted it as fiducial approach in this paper (see",0
+799,", for a discussion).",0
+800,"Of course, care has to be taken to avoid combinations of biosignature molecules which can be generated abiotically together (see e.g.",0
+801,short-term Fourier transform,0
+802,are methods to infer DR.,0
+803,"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.,",1
+804,without any serious contamination in the line of sight.,1
+805,"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",1
+806,and theoretically supported through detailed hydrodynamic simulations (e.g.,1
+807,"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",0
+808,The 70 μm band luminosities (from,0
+809,is a good example of such a huge scatter in the FIR luminosity of elliptical galaxies.,0
+810,"The spectral synthesis match was performed using the Stellar Parameters Classification tool (SPC,",2
+811,"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.",2
+812,"Our Galaxy, however, contributes",2
+813,"from its interstellar medium and a presumed ${\rm DM}_{\rm Halo}\sim 50 \, {\rm pc \, cm^{-3}}$ from its halo",2
+814,"On the one hand, it is more energetically favorable for the system to populate new degrees of freedom, such as hyperons",3
+815,"For a cosmic void, embedding requires the underdense interior to be “compensated” by an overdense bounding ridge, i.e., a compensated void",0
+816,"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.",2
+817,A soft excess below 1.5 keV is also present,0
+818,"In all four cases of different initial amplitude, ρIA, the phase speed decreases slighty (consistent with observations; see",5
+819,"In the microquasar Cygnus X-1, radio emission has been measured with a flat spectrum, i.e. α = −0.06 ± 0.05 and α = 0.07 ± 0.04",5
+820,"Larger data sets of star-forming clumps, identified as gaseous protoclusters, also exhibit a mass-size relation.",1
+821,"compiled the observations of Shirley et al. (2003), Faúndez et al. (2004), and Fontani et al. (2005) in their Fig. 1, and found via least-squares regression the relation R ∝ M0.38.",1
+822,"Meanwhile, both studies exhibit mass scatter of about 1 dex and are compatible with constant gas surface density, that is, R ∝ M0.5.",1
+823,Other examples of AGN with at least two variable phases of the X-ray winds are,0
+824,IRAS 17020+4544,0
+825,Previous studies include,0
+826,and magnetohydrodynamic (MHD) shocks,0
+827,magnetic helicity flux from anisotropy of the turbulence produced by differential rotation,0
+828,USSRH are a prediction of turbulent re-acceleration models,0
+829,"However, about half of our most massive clumps migrate radially outwards.",1
+830,but requires either large torques or steep surface density gradients,1
+831,"Nevertheless, Swift J1834.9−0846 has some interesting characteristics that are not shared with the entire magnetar population. First, the environment of Swift J1834.9−0846 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",1
+832,There are two main formation channels that are thought to compete in NSC formation:,0
+833,or via orbital segregation and merger of massive star clusters that migrate towards the galactic centre via dynamical friction,0
+834,"The explosions, however, leave imprints in the interstellar medium that can remain visible at radio wavelengths for 10 − 100 kyr",0
+835,thereby allowing the association of pulsars with supernova remnants (SNRs).,0
+836,"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.",3
+837,Models that have been contemplated in this sense include for example,0
+838,extended or exotic DM and/or dark energy (DE) models and interactions,0
+839,"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 “critical luminosity” Lcrit, which strongly depends on the magnetic field of the NS",0
+840,"Unfortunately, in the case of the M 81 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",1
+841,The fast solar winds emanate from coronal holes at higher heliolatitudes,2
+842,"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",2
+843,with a bandwidth equal to 1.5 times the bin size.,2
+844,"Among the fibers, f1 is clearly tracing the central-densest part of the dust ridge well known from previous dust-continuum observations",2
+845,"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 ‘mini-discs’ in the literature,",0
+846,as a consequence of the non-axisymmetric and time-dependent potential of the binary.,0
+847,"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",3
+848,The values of the para-H2CO column density were obtained with APEX data (beam size ~30″;,2
+849,AGNs with predominant radio emission from jet deviate from radio–IR correlation by showing radio-excess,2
+850,"Therefore, we examine if our NLS1s show radio-excess in the radio–IR correlation.",2
+851,"For an analytical expression of the poloidal magnetic field, we follow the practice of",2
+852,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=−∂At∂xr⊥r⊥+∂At∂r⊥+Atr⊥x.,2
+853,"Various values of β in MCs have been derived by several authors, ranging from β ∼ 0.38",1
+854,to β = 0.6 ± 0.3,1
+855,"More interestingly, there are hints suggesting that the impacts of projection effects extend beyond richness misidentification.",3
+856,"Secondly, when More et al. (2016) reported a detection of the so-called ‘splashback’ 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",3
+857,for a similar detection).,3
+858,Aperture photometry was performed with the DAOPHOT,2
+859,package,2
+860,"Nevertheless, early attempts (e.g.,",0
+861,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.,0
+862,"For this work, we used two reference spectra:",2
+863,and the spectrum of NGC 4387,2
+864,an elliptical galaxy showing strong absorptions.,2
+865,It has been classified as having a cometary-like morphology with an integrated subsolar metallicity of 12 + log(O/H) = 7.73–7.78,0
+866,"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) ≤ 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⊙",0
+867,"Subsequently,",1
+868,"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.",1
+869,"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.",1
+870,"On the other hand, many fewer studies, all recent, were devoted to the full mass spectrum, using optical photometry",0
+871,The magnetic fields in the low solar atmosphere could be very strong,2
+872,"Mid-IR (MIR) and far-IR (FIR) observations have revealed bright atomic lines from H ii regions ([S iii], [Ne iii], [Ne ii], [O iii], etc.) and PDRs ([C ii], [O i]) (e.g.,",0
+873,"It is important to do so because different processes, e.g.",3
+874,pristine accretion,3
+875,are surely contributing to the same system,3
+876,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,1
+877,", causing its heating via inelastic collisions with the ambient plasma via a hydrodynamic response",1
+878,and a comparison with the other EoSs of the BSk family,7
+879,shall be left for future study.,7
+880,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.,3
+881,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.,3
+882,"Since the star-formation histories of galaxies (ETGs included, e.g.",2
+883,"can be stochastic and include multiple bursts, we also verify the full-spectrum fitting capabilities to retrieve more complex SFHs.",2
+884,Current cosmological hydrodynamic simulations of galaxy formation employ a variety of subgrid models (e.g.,0
+885,"that artificially launch galactic winds, but the results are sensitive to numerical resolution and the exact subgrid model employed",0
+886,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,0
+887,The high-twist region in our result is also in agreement with the,5
+888,and the location of the flare ribbons,5
+889,We scan each trial of data and the on-source window in the 30–1000 Hz frequency band using a predefined bank of waveform templates,2
+890,Previous studies of intermediate-age star clusters with eMSTOs usually showed tight SGBs throughout,6
+891,but see,6
+892,"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",0
+893,"where P0, T0, and Λ values are listed in Table 1, s is the depth from the nucleus surface, $f(s) = 1 - (1 - {s \over R})^4$ for s ≤ R, f(s) = 1 elsewhere, r ≈ 50 nm and R ≈ 5 mm are the radii of the grains of which cometary dust consists",2
+894,and of the pebbles of which cometary nuclei,2
+895,Three-dimensional simulations that include all three non-ideal MHD effects are also performed,0
+896,"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",2
+897,to reach the total sample of 196 galaxies with IR line fluxes in the 5.5 − 35 μm interval in which an AGN component is not detected.,2
+898,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,0
+899,"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",6
+900,"and Hezaveh et al. 2016), but we hope that our work can help make substructure lensing more reproducible.",6
+901,"In the regions we investigated, the Hapi region displays the lowest spectral slopes 8–11%/100 nm (see also",1
+902,together with the isolated bright features (IBFs) and the clustered bright features in the Imhotep region.,1
+903,We introduce a method to search for signatures of DM annihilation from a Galactic subhalo population using the non-Poissonian template fitting (NPTF) framework,2
+904,"Our model consists of four zones; an inner disk (zone 1, as in",2
+905,Several predictions for planet(s) shaping the disk of SAO 206462 have been proposed,0
+906,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,1
+907,Uncertainties in stellar radius estimates from photometric Kepler observations prevented a detailed assessment of the intrinsic planet size distribution,0
+908,The calculations of LS,0
+909,are the two EoS tables in more widespread use for astrophysical simulations.,0
+910,varying within an order of magnitude over decades of observations,0
+911,The [C II]–FIR luminosity ratios of these quasar hosts range from 10−4 to a few ×10−3,1
+912,following the trend of decreasing [C II]–FIR ratio with increasing FIR luminosities found with the IR luminous star-forming systems,1
+913,The column density is estimated from the fitted line profile by assuming local thermodynamic equilibrium (LTE),2
+914,"In Equation (3), ΔE 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−1 as measured by Voyager 2, whereas uR = 40 km s−1 for the heliosheath in the Voyager 1 direction",2
+915,In low-density regions (according to,0
+916,"\hbox{$A_{V} \leqslant 0.7$}AV⩽ 0.7 for the standard ISRF), UV photons are responsible for causing the photo-dissociation of CH bonds, a-C:H → a-C.",0
+917,"However, Lyα emission is known to be extended beyond the continuum",1
+918,and fluxes based on the TDOSE spectra would therefore be biased.,1
+919,"Methanethiol (or methyl mercaptan, CH3SH) was detected in the Sagittarius B2 (Sgr B2) region of the center of our Galaxy",0
+920,"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-β",0
+921,"In the FS (BS), the 2D velocity map between the current and the previous (next) frame is constructed with almost the same method as",2
+922,"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.,",0
+923,"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.,",1
+924,"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 σ = 400 eV, in accordance with what literature papers (e.g.",2
+925,"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.",3
+926,"Therefore, methods with more advanced mathematical algorithms were introduced.",0
+927,Coronal Hole Identification via Multi-thermal Emission Recognition Algorithm (CHIMERA),0
+928,"have been found to be very effective and are widely used in online solar data visualization tools1$^,$ .2",0
+929,Narrow-band imaging can efficiently detect LAHs at targeted redshifts through stacking,0
+930,"and narrow-band surveys enable ultradeep, blind samples of LAHs around distant galaxies",0
+931,Examples of r-process sites that have been proposed and investigated by theoretical studies include (i) neutrino-driven winds from proto-neutron stars (NSs;,0
+932,"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.,",0
+933,for a review),0
+934,"During the past two decades, several Type IIb SNe with such interesting features have been monitored and studied well, e.g.,",0
+935,SN 2011fu,0
+936,Although shown to be too simplistic by the first X-ray studies of clusters,1
+937,the self-similar relations allow us to investigate if astrophysical processes are less significant in more massive clusters or at higher redshift.,1
+938,Further observations revealed a transition in average densities at planet sizes ∼1.5 R⊕,0
+939,with smaller planets having densities consistent with rocky compositions while larger planets having lower densities indicating significant H/He envelopes.,0
+940,The colour information is considered an important feature to find lenses (see e.g.,2
+941,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.,2
+942,"At redshifts above z ∼ 1, it is nearly impossible to detect weak auroral lines for directly determining metallicity (but see",1
+943,"Therefore, GRB afterglows are good probes of burst environment and the interstellar dust and gas in distant, star-forming galaxies",3
+944,"At the same time, gas accretion rates were maximal",0
+945,"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",3
+946,"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",1
+947,We use a constant SPH artificial viscosity coefficient αSPH ≈ 0.55 such that the corresponding disc viscosity coefficient,2
+948,is αd = 0.01 at the inner radius.,2
+949,These speeds far exceed the few km s−1 planet-frame velocities detected on other planets,1
+950,"The currently accepted distance of NGC 6231 is approximately 1580 pc, and its age is between 2and 8 Myr, with a significant intrinsic spread",0
+951,These included,0
+952,"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 s;",0
+953,"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 81 galaxy with a total hydrogen column density in the range 1.5–5 × 1020 cm-2 and dust temperatures between 13 and 17 K",0
+954,"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 81 and NGC 3077 is of Galactic origin.",1
+955,several exhibit spiral arm morphologies,0
+956,98 clusters are identified by the South Pole Telescope (SPT;,2
+957,but are not included in the Planck PSZ2 catalogue.,6
+958,The most stringent and precise constraints on the self-interaction cross-section have been put on the scales of galaxy clusters (e.g.,0
+959,"where observations require that $\sigma _T/m_chi \lesssim 1\, {\rm cm^2g^{-1}}$.",0
+960,This process may provide an explanation for the observed braking indices of young pulsars with n ≠ 3,1
+961,in contrast to the prediction of a rotating magnetic dipole in vacuum,1
+962,"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.,",3
+963,"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,",2
+964,"However, this does not explain the discrepancy with",1
+965,who also used magnesium.,1
+966,The detailed mechanistic route for the interstellar synthesis of MF is a subject of considerable debate,0
+967,These physical conditions are consistent with what is found for Mrk 231,5
+968,"We then included an absorption component and fixed the photon index to 1.8, as expected for the intrinsic AGN emission (e.g.,",2
+969,"For internal consistency, all EWs in this work have been adjusted to the measurement scale of",2
+970,"If the core does collapse, the explosion proceeds via delayed explosion on short timescales",1
+971,and 2D simulations suggest the explosion occurs before significant convection has had time to develop,1
+972,and hence a symmetric explosion results.,1
+973,"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.′′ 9 ± 0.′′2. At these locations we observe the transition between rigid body rotation and steep rotation curve to a flat one (see also",5
+974,"As mentioned before, we conclude that strong bars drive the trends of bar fraction with (g −r) colour, stellar mass, and SFR observed in other studies",4
+975,A key question that remains unanswered is how BBHs are formed. Viable formation channels include,0
+976,"and dynamical encounters in dense stellar environments, such as globular clusters (e.g.,",0
+977,The existence of relations between SFR and galaxy stellar mass (SFR–Mass) and specific star formation rate and mass (sSFR = SFR/Mass) have been established from z = 0 out to z > 2,0
+978,Therefore the amplitudes estimated in,2
+979,"listed in Table 1, are used in this work as fixed values.",2
+980,"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",0
+981,We followed the implication of this approach described in,2
+982,and refer the reader to that work for more details.,2
+983,"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.,",0
+984,"The radio to X-ray spectrum of the forward shock afterglow emission of GW170817/GRB 170817A is fν ∝ ν−0.6, which yields a p = 2.2 in the slow-cooling synchrotron radiation scenario",2
+985,"while a portion of the Compton component will escape to reach an observer, the remains (refer as ${\tt{\rm simplc}}$,",2
+986,will strike back to the disc to generate the reflected component.,2
+987,"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;",0
+988,Previous observations show that para-H2CO (3–2) is sensitive to gas temperature at density 105 cm−3,2
+989,"The main conclusion in all these studies is that a [C ii] 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.",1
+990,"In principle, an increase in accretion rate would be expected to result in an increase in the scale height of the funnel (e.g.",3
+991,"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 ∼ 1, where H is the scale height of the disc at radius R).",3
+992,Supervised learning has been used to,0
+993,and to determine the redshift of galaxies,0
+994,"In the optically thin limit, the emission is significantly polarized",0
+995,", an effect that has been observed in higher-luminosity AGN sources",0
+996,"To take an even more practical approach, we chose a normalized color parameter based on the Spitzer Infrared Array Camera",2
+997,"as a commonly used photometer for the observation of exoplanets (see, e.g.,",2
+998,This limit is referred to as the quasi-static approximation to MHD,0
+999,although recent numerical studies on its turbulent properties and anisotropy have been done as well,0
+1000,"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",2
+1001,Combined with the red clump sample of,1
+1002,stars in different evolutionary states in Gaia 1 are progressively being sampled.,1
+1003,"This provides a natural route for forming GRBs in low-metallicity environments, as found for most GRB hosts",1
+1004,A detailed theoretical model for gamma-rays from the collision of cosmic ray with the solar atmosphere was presented by,0
+1005,"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.",0
+1006,"Here, τγ, ν is the optical depth of the ejecta to γ-rays and Kγ, ν is the photon inelasticity at a given frequency, where the Klein–Nishina cross section and the cross section for the Bethe–Heitler pair production in the field of a carbon nucleus are taken into account",2
+1007,"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",1
+1008,These methods include:,0
+1009,empirical relations to derive stellar mass in the form of mass-luminosity relations,0
+1010,"It has been found that alkali atoms are present in cool brown dwarf atmospheres, indicating that silicate rainout may occur in these objects",3
+1011,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,0
+1012,"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.,",0
+1013,"Within this scenario, the low water content of Europa is puzzling.",6
+1014,whereas the more accurate ExoMol POKAZATEL line list,0
+1015,is complete up to 4000 K.,0
+1016,"Finally, based on the CASSCF wave functions, the internally contracted multi-reference configuration interaction method with the Davidson correction (icMRCI+Q)",2
+1017,is performed to consider the dynamic correlation and size-consistency error.,2
+1018,"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 – ‘relic discs’",0
+1019,"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",0
+1020,see also,0
+1021,The main group ureilites represent the mantle residues after the extraction of,0
+1022,and a sulfur-rich iron melt,0
+1023,We note that the blowout size can be increased with particle porosity and increasing stellar temperature,2
+1024,"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",3
+1025,"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 Brγ emission but no evidence of He i or Mg ii are B5 or later.",0
+1026,Although SKA might provide number counts at sub-µJy levels,1
+1027,"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",1
+1028,"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",2
+1029,Our result is consistent with that found by,5
+1030,"using XMM-Newton data,",5
+1031,"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.",2
+1032,"In color-magnitude space, YSES 2b is very close to the innermost three planets of the HR 8799 multi-planetary system",1
+1033,"In recent years, integral field spectroscopic (IFS) surveys",0
+1034,have overcome these problems with the use of instruments with larger FoVs and a fully spectral coverage (e.g,0
+1035,"ATLAS3D,",0
+1036,"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",0
+1037,"using optical and near-infrared color selection, and determined a thin disk vertical scaleheight for these sources of 290 ± 40 pc.",0
+1038,"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",0
+1039,"Newer, alternate cosmological probes could help alleviate this issue.",3
+1040,Recent examples of such probes include,0
+1041,H ii starburst galaxy measurements that reach to z ∼ 2.4,0
+1042,Even though there is a lot of scatter in the D − HT diagram caused by variation in f from one comet to the next,2
+1043,This candidate appears to have one of the most compact orbits among the known SMBH binaries and has overcome the ‘final parsec problem’,1
+1044,The simplest of such methods uses a Wiener filtering technique,0
+1045,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.,0
+1046,"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",0
+1047,reflected on their clumpy morphologies,0
+1048,Malanushenko and co-authors,0
+1049,have presented a method for deriving an NLFFF model from sparsely distributed EUV loop observations.,0
+1050,"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.",1
+1051,and we restricted them to the limiting cases derived in Sect. 3.5 of,2
+1052,rather than allowing them to take arbitrary values.,2
+1053,The radial distance between the centres of the Orion and Sagittarius arms near the Sun is λrad ≈ 2 kpc (cf.,0
+1054,"They also can reconnect with the ambient field (e.g.,",0
+1055,"However, recent numerical simulations of thermal tides in optically thick atmospheres by",5
+1056,show behaviour of the flow that is in good agreement with a model that uses radiative cooling.,5
+1057,"Therefore, in this work we assumeNewtonian cooling as a first model of the action of radiation on atmospheric tides.",2
+1058,The Planck survey provides a large amount of data for polarisation studies at cloud scales,0
+1059,carried out a comparison of the metallicity gradients in the ISM (traced by young SPs) obtained by different numerical and analytical models,0
+1060,Different MHD oscillation modes have been identified to be responsible for QPPs in a single flaring loop,0
+1061,"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",2
+1062,"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 (",2
+1063,; cross-matching for both catalogs is as explained in Appendix A.3).,2
+1064,"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 ≳ 1 kpc and a largely CDM-like matter power spectrum at late times",1
+1065,"as was used in our simulations, although these scenarios are not well-motivated.",1
+1066,"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",0
+1067,"Given the nature of the variability, we measure the period via the reduced χ2 of a sinusoidal fit as a function of frequency (ideally suited to sinusoidal variability, e.g.",2
+1068,"MaNGA observed approximately 10 000 galaxies, selected as an unbiased sample in terms of stellar mass (${\it M}_{\star } \gt 10^{9}\, {\rm M}_{\odot }$) and environments",0
+1069,"The (μ, σ) pairs allowed in the window relevant for the operational gravitational wave detectors",2
+1070,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,2
+1071,"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.",1
+1072,"The importance of additional processes such as internal waves (e.g.,",0
+1073,"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",2
+1074,The high Fe charge states (⟨Fe⟩ ≥ 12) and abnormally high O7+/O6+ ratio (≥1) are the result of flare-related heating in the corona,2
+1075,and therefore they are independently reliable ICME indicators,2
+1076,We introduce a method to search for signatures of DM annihilation from a Galactic subhalo population using the non-Poissonian template fitting (NPTF) framework,2
+1077,which has previously been applied to characterize unresolved point sources in the inner Galaxy,3
+1078,"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.,",0
+1079,"For instance, partial ring distributions were frequently observed for solar wind protons at intermediate heliocentric distances, when the spacecraft approached the SWIC",0
+1080,"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",1
+1081,and this is a source of uncertainty in our yield calculations.,1
+1082,Some of these events may correspond to gravitationally lensed events with magnification factors ranging from a few tens to a few hundreds,0
+1083,"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 cent in our richness range",1
+1084,"Allison, Sadler & Meekin (2014) identified four H i absorbers, including one previously unknown source, with the archival data of the H i Parkes All-Sky Survey (H i PASS; see",0
+1085,"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.",3
+1086,its detection has never been confirmed,3
+1087,"However, the masses corresponding to impact flashes recorded on the Moon are several orders of magnitudes larger than mo",6
+1088,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,2
+1089,"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°",1
+1090,"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",1
+1091,"In contrast, higher localization accuracy would be obtained by networking of 3rd generation GW detectors",1
+1092,"Over the last decade, large observational efforts have been devoted to map the molecular gas reservoir of galaxies (e.g.,",0
+1093,"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),",0
+1094,"Along decades, results based on this indirect method have indicated Z near or slightly above the solar value in nuclear regions",5
+1095,in consonance with predictions of chemical evolution models,5
+1096,and with the use of strong-line methods,5
+1097,Benchmarks by Hochlaf and co-workers,5
+1098,"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.",5
+1099,"In panel b of Fig. 12, we also superimpose the distribution of [OIII]/[OII] ratio for the GRB sample of",2
+1100,and GRB 081121 reported here.,2
+1101,"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(Lyα) of 60%) in agreement with potential high fesc(LyC). Nevertheless, the Lyα profile of GRB 021004 is a single peak with no residual flux at the Lyα line center.",1
+1102,"Additionally, CGM observations infer a significant amount of metals (e.g.",0
+1103,"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",0
+1104,Given the reported high spin values for these bright AGNs,2
+1105,we expect the ISCO to sit at ∼1.25Rg.,2
+1106,"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 = (0.7–2.2) × 1050 erg",1
+1107,The data were recorded in psrfits format and processed using PSRCHIVE tools,2
+1108,"determined by ion storage ring experiments,",0
+1109,"The expected B values in star forming regions range from ~100 μG, for low-mass objects",2
+1110,", to ~1 mG, as measured in regions hosting high-mass young stars (e.g.,",2
+1111,Numerous mass spectrometric studies have investigated the production of H+MF via various ion–molecule reactions and its fragmentation by metastable decay and collisions,0
+1112,The salmon-coloured points show recent results from other high-resolution spectrographs:,2
+1113,WASP-121b with ESPRESSO,2
+1114,"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.",5
+1115,"For example, studies of young clusters embedded in moderate-mass MCs (∼104M⊙) (e.g.",0
+1116,"have shown that their age histograms contain a large majority of young (1–2 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",0
+1117,"NGC 419, another young massive cluster with an age of 1.72 Gyr and a mass of ∼104 M⊙, are comparably massive with respect to other star clusters that show clear evidence of MPs",6
+1118,"the possibility that they are tidal dwarf galaxies – 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.,",6
+1119,– is ruled out.,6
+1120,A CO spectroscopic redshift of 3.26 was first suggested by Z-spec,1
+1121,"observations, then subsequently confirmed by observations by",1
+1122,the Zpectrometer instrument,1
+1123,on the Greenbank Telescope,1
+1124,"The Mid-Infrared Spectrograph (MIRS) aboard the Infrared Telescope in Space (IRTS) has also obtained the 4.7–11.7$\, {\rm \mu m}$ spectrum for the diffuse ISM towards l = 44°20′, b = −0°20′",2
+1125,"The primary tracer for H2 in current use is the J = (1−0) 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.,",0
+1126,"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.",1
+1127,"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.",2
+1128,"Previous sub-arcsecond angular resolution N-band (∼8–13 μm) ground-based spectroscopic studies investigated the 11.3 μm PAH feature in the nuclear and circumnuclear regions of AGN (e.g.,",0
+1129,"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.",3
+1130,The pitch angle and the distance at a reference position of the three arms are taken from,2
+1131,for the Local arm,2
+1132,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.,0
+1133,"We found good agreement between the position of the FQS clouds and the modelled position of the Local and the Perseus arms,",5
+1134,"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",2
+1135,"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",5
+1136,"Dynamical models and N-body simulations (see, e.g.,",0
+1137,"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 (≈60 Myr) due to loss of angular momentum from escaping stars",0
+1138,Inspired by earlier studies from Taylor & Manchester (1977) and,0
+1139,"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.",0
+1140,"For instance, we can use these model-independent measurements",0
+1141,to test natural constants such as the speed of light,0
+1142,"Selecting SMGs from observations at longer wavelengths is thought to favor galaxies at higher redshifts (e.g.,",1
+1143,although it is difficult to compare the redshift distributions in an unbiased way,1
+1144,and account for intrinsic variations of galaxy far-IR spectral energy distributions (SEDs).,1
+1145,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,0
+1146,(simply K in other works) is the conversion factor from the MWO HKP-2 H & K flux (numerator of Equation (1)) to physical flux,2
+1147,We assume a power-law energy distribution of radiating electrons with somewhat shallow index of b = −1.5 that can account for the relatively flat spectrum of the source,2
+1148,The present observational probes that allow us to have a peak in this epoch are the absorption spectra of high-redshift quasars,0
+1149,"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 $10^{-4}\, \rm {Z_{\odot }}$",1
+1150,as well as several others with $\rm {[Fe/H]} \lt -5$,1
+1151,Recent relativistic (magneto-) hydrodynamics simulations,3
+1152,"have illustrated the importance of the ambient medium in shaping the jet, thereby highlighting the importance of understanding the remnant structure and ejecta properties",0
+1153,"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.",7
+1154,"While there is almost unanimous agreement that AGNs of low to moderate luminosity (Lbol ≲ 1045 erg s−1) at z ≈ 0–3 lie on or below the main sequence (e.g.,",5
+1155,", no consensus exists for AGNs with Lbol > 1045 erg s−1.",6
+1156,"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",3
+1157,table 2 of,3
+1158,"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.",3
+1159,According to,2
+1160,"the subhalos also retain their identity for quite some time after accreting a larger halo, so satellites in subhalos less massive than ~1012 M⊙ do not immediately see the effect of the hot gas in the larger halo and accrete in cold mode.",2
+1161,"Thus, consistent with the results of Yang et al. (2012) and Béthermin et al. (2013), satellite galaxies continue to accrete gas and convert it to stars over a rather long period,",5
+1162,"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",0
+1163,"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 ;",1
+1164,The open circle and square are the results from the Arecibo Ultra Deep Survey (AUDS),2
+1165,Using a Bayesian approach,2
+1166,we computed 95% upper limits for all the nondetections.,2
+1167,The very fast dissolution of tidally filling models with low King model concentration was already extensively discussed in the literature (e.g.,0
+1168,"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",0
+1169,"However, a large fraction (${\sim } 28{{\ \rm per\ cent}}$) was found to be inconsistent with the theoretical limit of −2/3 (‘line of death’;",6
+1170,"and only specific physical scenarios remain plausible (large emitting radii and Lorentz factors of the flow,",6
+1171,"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 25–50 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 ± 4 per cent,",1
+1172,This method has since been used to successfully uncover highly obscured and even Compton-thick AGNs in several other works thus far,0
+1173,"In the case of collimated relativistic jets, magnetic fields must play an important role",0
+1174,"Optical coordinates, right ascension and declination (epoch 2000.0) for the identified counterpart from Zaritsky et al. (2002), or – when not available there – from",2
+1175,"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",0
+1176,Cepheids analysis from,2
+1177,green,2
+1178,The latter model has been invoked as a possible mechanism in the downstream of the CME shock,2
+1179,"Since then, several authors",0
+1180,"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",0
+1181,"Other emission lines, however, such as the far-infrared [C ii]λl58 µm line, are strikingly enhanced on global scales in dwarf galaxies (e.g.,",1
+1182,"Subsequently, a number of works have",0
+1183,"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 α elements – that we indicate as chemical clocks – and thus maximising the dependence of the relationship with age (see, e.g.,",0
+1184,"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.",1
+1185,Inclusion of mass-loss and/or rotation would produce a similar increase in the Cepheid luminosity level at fixed mass (see,2
+1186,for details).,2
+1187,"Doing so, we find EX ≈ EU ∼ 2 × 1032 erg for AD Leo",2
+1188,Evidence for offset dust continuum emission relative to the rest-UV has been identified in several high-redshift Lyman-break galaxies (LBGs;,1
+1189,"In previous studies, geometrical models based on the assumption of different cone shapes were developed to obtain CME 3D parameters from single spacecraft observations",0
+1190,"Analysis of the particle yields produced in relativistic A+A collisions within statistical (thermal) models, i.e., the Hadron Resonance Gas (HRG) model",0
+1191,shows the importance of the particle hard core repulsion.,0
+1192,"The dimensionless accretion rate is estimated by $\dot{\mathscr {M}}=20.1\, \ell _{44}^{3/2}M_7^{-2}$ from the Shakura–Sunyaev disc model",2
+1193,"where ℓ44 is the 5100 Å luminosity in units of $10^{44}\, {\rm erg\, s^{-1}}$ and $M_7=M_{\bullet }/10^7\, \mathrm{M}_{\odot }$.",2
+1194,The sample of,2
+1195,"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 × 1020 cm-2 the change from slope of 1.0 to 2.0 would alter our estimated fluxes by −14% (ROSAT), −13% (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 2.0–10.0 keV 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.",2
+1196,They can also shed light on the origins of supermassive black holes and early cosmological reionization and chemical enrichment,3
+1197,"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",0
+1198,These findings by,1
+1199,", along with the discrepancy between our calculated ratio of Ebp/kBTc = 5.5 ± 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.",1
+1200,"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.",0
+1201,"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",0
+1202,"Recently, we proposed an improved Amati correlation",0
+1203,"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",0
+1204,"An interesting implication is that, if BHs settle into the disk, they interact dynamically and form BH–BH binaries efficiently, and frequent dynamical interactions and gas effects drive the BHs to merger, producing gravitational waves (GWs) detectable by LIGO, VIRGO, and KAGRA",0
+1205,"Deep Herschel/SPIRE spectroscopy has also revealed a number of FSL detections, either in individual objects",0
+1206,"If 26Al was introduced into the solar system at the earliest stage of the disk evolution (e.g.,",2
+1207,differences in Be–B and Al–Mg systematics between CH–CB 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.,2
+1208,The inner jet,0
+1209,and displays strong and variable radio polarization (e.g.,0
+1210,"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.,",0
+1211,Two-point statistics are central to many of the leading cosmological analyses of the large-scale structure searching for deviations from ΛCDM,0
+1212,and a great deal of effort has gone into accurately modelling the non-linear matter power spectrum in modified gravity and dark energy cosmologies – a theoretical ingredient essential to extract the cosmological information locked in small scales (e.g.,0
+1213,"Indeed, Mg ii is known as a good tracer of high column density H i gas in damped Lyman α absorbers (e.g.",0
+1214,"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.",6
+1215,"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.",1
+1216,Modelling by both Shabala et al. (2020) and,5
+1217,confirms the picture in which the remnant lobes fade quickly below the LOFAR detection limit.,5
+1218,This can be mitigated by using integral field spectroscopy (IFS) which is being increasingly used for extragalactic studies (e.g.,0
+1219,although there could still be projection effects with the IFS data.,0
+1220,"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",0
+1221,It is also well known that the radius R1.4 of canonical NSs is essentially determined by the pressure at densities around ρ0 ∼ 2.5ρ0,2
+1222,while the maximum mass of NSs is determined by the pressure at higher densities reached in the core.,2
+1223,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,1
+1224,A fraction of the stellar wind is captured and channelled along the strong magnetic field,0
+1225,"of the neutron star on to the magnetic poles, producing regular X-ray pulsations caused by the spin period ∼283 s",0
+1226,of the neutron star.,0
+1227,"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%",6
+1228,compared to previous calculations.,6
+1229,We shall adopt here the EoS of the BSk21 model,2
+1230,"as a representative example of contemporary EoS for the complete NS structure,",2
+1231,Our group is addressing this problem by combining a variety of complementary perspectives:,2
+1232,(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,2
+1233,"A dust cloud composed by large grains ( ∼ 1 μm) would suppress the scattered intensity even at 1 keV, while it would significantly attenuate X-rays at ≤0.5 keV (e.g.",2
+1234,"Previously, we retrieved and cross-matched a large quantity of atomic data from several major atomic databases such as the",2
+1235,and providers within the Virtual Atomic and Molecular Data Centre (VAMDC;,2
+1236,in preparation for quality assessment work,2
+1237,A few examples are,0
+1238,and superluminal motion and high brightness temperature,0
+1239,They may also be aligned in the direction of,0
+1240,or the drift velocity of the grains relative to the ambient gas,0
+1241,"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",0
+1242,"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.,",0
+1243,"This Tmai is at the low end of the Tmai output by thermal evolution models for multi-Gyr-old sub-Neptunes (e.g.,",1
+1244,"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",2
+1245,"Alternatively, the scarcity of detected pulsars might be caused by a more complex scattering structure towards the GC",0
+1246,"The upper panel of Figure 4 also shows a strong correlation between [Na/Fe] and the δCN index, which is in good agreement with previous studies",5
+1247,"Thus, in clustered DE scenarios, we should consider the contribution of perturbated DE components to the total mass of the haloes",2
+1248,"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 ≈15% from June 2013 to February 2014 at 41 GHz, with 0.55 Jy corresponding to the strongest variation in the same period,",2
+1249,"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",0
+1250,and clustering,0
+1251,"According to the pseudo-time-dependent gas-phase astrochemical model under dense cloud conditions (104 cm−3, 10 K, 10 mag) by",1
+1252,"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 × 105 yr, and it occurs after the significant fraction of nitrogen is frozen out.",1
+1253,"In particular, it is known to often display a blue wing (e.g.",3
+1254,"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 iii] blue wing",3
+1255,Both Bernard-Salas et al. (2009) and,5
+1256,reported data from the high-resolution Spitzer-IRS spectra.,5
+1257,"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",2
+1258,on the Atacama Pathfinder EXperiment (APEX,2
+1259,telescope,2
+1260,"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",3
+1261,"It has a contribution of at least 15 per cent in the clump at early stages of massive star formation, which is lower than that reported in previous studies",6
+1262,"Interestingly,",0
+1263,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.,0
+1264,As for the experiment on ice by,1
+1265,it is well known that reaction barriers possibly present in gas-phase reactions are not significantly reduced when moving to ice-mediated reactions,1
+1266,We chose to compare to the,2
+1267,spectral models from WM-BASIC for OB-stars,2
+1268,"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 ${}^{44}_{}\mathrm{Ti}$  or excited ${}^{44}_{}\mathrm{Ca}^{*}$",1
+1269,the validity of such an interpretation of the discrepant measurements of ${}^{44}_{}\mathrm{Ti}$  fluxes at 68 and 78 keV and at 1.157 MeV by different instruments and by the same instrument (SPI) may be doubted.,1
+1270,These triggering processes were numerically studied by Karlický & Jungwirth (1989) and,0
+1271,Additional evolutionary channels for SNIa include,0
+1272,the core-degenerate channel,0
+1273,"We ignore the pressure term in equation (4), which leads to a set of equations that conserve energy",2
+1274,"The peak column densities and total masses of both sources deduced from the 1.3 mm continuum emission are ∼1 × 1024 cm−2, and ∼2 × 102 M⊙, respectively, with an assumption",2
+1275,"and a uniform dust temperature of 20 K, which is typically adapted/estimated for galactic high-mass star-forming dust clumps (e.g.,",2
+1276,Dispersions are thought to be driven at least partially by thermal velocities or supernovae,1
+1277,"Early work highlighting the issue of the high-redshift offset in the [O iii]λ5007/Hβ vs. [N ii]λ6584/Hα BPT diagram focused on these parameters (e.g.,",0
+1278,"In fact, the jet–wind interaction alone can already perturb the jet",0
+1279,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,0
+1280,The presence of the substructure has been confirmed by Chandra and XMM-Newton,0
+1281,as well as by more recent SZE measurements,0
+1282,Our flared vertical profiles for the thin and thick disks,5
+1283,and are consistent with the number simulations of the chemodynamical evolution in Galactic disks formed in the cosmological context,5
+1284,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,0
+1285,The laboratory data most widely used for comparison to observations are those provided by,2
+1286,The first reference gives IR spectra and band strengths of methanol ice at 10 K in the 2.5–20 μm range.,2
+1287,"However, over the last few years a number of multifrequency compact source detection techniques have been proposed in the literature",0
+1288,"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;",0
+1289,and that the minimum GCR intensities occur within the MC.,0
+1290,"Indeed, the scientific debate about the emission profile of the jet and the subsequent gamma-ray production mechanism of GRB 170817A is still ongoing",3
+1291,"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",3
+1292,GRB 170817A was followed by the discovery of the optical counterpart Swope Supernova Survey 17a [SSS17a (AT 2017gfo)] ∼11 h later in the galaxy NGC 4993,0
+1293,and later confirmed by others teams,0
+1294,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,0
+1295,"Cluster number counts from Sunyaev-Z’eldovich 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.",0
+1296,This result is consistent with previous research within a 1σ error,5
+1297,"Here, it is worth noting that the 1σ errors of the γ best fit from previous research are both larger than 0.01.",6
+1298,"For the collision term associated with neutrino emission, absorption, and scattering with leptons, nucleons, and nuclei handles, the basic neutrino reactions are adopted",2
+1299,"In the optically thin limit, the emission is significantly polarized",0
+1300,an effect that has been observed in higher-luminosity AGN sources,5
+1301,"It is also much better at driving winds, because the CRs do not suffer strong energy losses via Alfven wave heating",2
+1302,We repeated the plasma pressure calculation presented by,2
+1303,and Fuselier et al. (2012) for the new ENA energy spectrum.,2
+1304,"Such evolutionary behavior is consistent with “strangulation” wherein cold gas that could be used for star formation is depleted as satellites are accreted (e.g.,",5
+1305,"The Pipe Nebula,",0
+1306,has played a workhorse role in a number of previous studies (e.g.,0
+1307,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.,0
+1308,"For instance, the TDCOSMO collaboration",0
+1309,has achieved ∼2% 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,0
+1310,and baryon matter.,0
+1311,As is often observed,5
+1312,", we require multi-temperature components to achieve an adequate description of the observed coronal spectra.",5
+1313,May & Stevenson (2020) claimed that the differences between the retrieved phase offsets is the result of temporal binning which was not used by,1
+1314,"and May & Stevenson (2020) but was used by Mendonça et al. (2018), Morello et al. (2019), and this work.",1
+1315,"Various observational techniques, such as measuring the Gunn–Peterson optical depth from QSO spectra or the prevalence of Ly α 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∼ 6",0
+1316,"More recently,",0
+1317,also investigated the gradients of n-capture element abundance-to-iron ratios with respect to Rgc for a sample of 435 Cepheids.,0
+1318,Except for two objects,0
+1319,in the local Universe no ionizing radiation has been detected directly,0
+1320,although some objects show indirect evidence of photon leakage,0
+1321,"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",5
+1322,"As an example, the analysis of the hyperfine structure of several N-bearing species, such as N-protonated isocyanic acid (H2NCO+,",0
+1323,) which has been detected toward G+0693-0.027,0
+1324,was required for its conclusive line-by-line identification.,0
+1325,"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",2
+1326,"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.",0
+1327,"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.",0
+1328,"Also, NGC 4490 has a giant H i envelope that probably originated from the star formation",0
+1329,"Alternatively, one can compute the bolometric luminosity following",2
+1330,"However, there is overwhelming observational evidence that magnetic fields in the ISM have well-defined directions, indicating that turbulence is sub, trans-Alfvénic and hence turbulent properties are highly anisotropic",0
+1331,"However, the question of whether galactic bars can significantly affect AGN activity is still under debate",0
+1332,"N. E. Raouafi et al. (2015, in preparation) have argued that type II spicules have much more in common with so-called “classical” spicules",5
+1333,"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.",5
+1334,The factor 1.08 is the multiplicative shear calibration bias of the used KSB+ pipeline,2
+1335,to convert from measured to true ellipticity.,2
+1336,"Thus, it is possible that disks were massive enough to form the cores of planets at younger ages. This idea has been suggested by",1
+1337,"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.",1
+1338,The bimodality has now been observed in some simulations,5
+1339,"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",0
+1340,"This process can end up as a SN Ia, a highly magnetized WD (MWD), or an accretion-induced collapse",0
+1341,The synchrotron peak usually moves to higher frequencies with increasing flux during outbursts,0
+1342,but no correlation between the break energy and the flux exists when a broken power law is adopted to fit the X-ray spectra,0
+1343,"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—under the assumption of a strong correlation between radio luminosity and environmental density (e.g.,",1
+1344,but see further in this section for different points of view),1
+1345,"To avoid catastrophic suppression of the dynamo action (α-quenching), the magnetic helicity due to the small-scale magnetic field should be removed from the system",0
+1346,Mechanisms suggested to produce these small-scale magnetic helicity fluxes are:,0
+1347,and through diffusive flux,0
+1348,Top right: the r31 brightness temperature ratio of VLASPECS galaxies (green circles) is similar to that of,5
+1349,and z > 2 dusty star-forming galaxies (DSFGs; blue squares; compilation from Sharon et al. 2016; including data from,5
+1350,"However, at the corresponding frequency of 138 d−1, the TESS high-cadence data (sector 10) show no signs of such a signal, confirming previous negative reports",5
+1351,"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.",0
+1352,"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",0
+1353,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.,0
+1354,The unprecedented quality of the light curves combined with new curve-shifting algorithms,2
+1355,lead to time delays with typically ∼3 per cent accuracy,2
+1356,The stream interface (S′-F′) 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,2
+1357,"For grains surrounded by an ice mantle, the optical properties are derived with the core-mantle Mie theory using the BHCOAT routine given in",2
+1358,The more contentious issue is that of the phase curve’s phase offset and nightside temperature.,6
+1359,"initially reported only a 2σ upper limit on the nightside temperature of 650 K, while all subsequent reanalyses (including ours) favour a significantly detectable nightside temperature of ∼800 K.",6
+1360,"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",0
+1361,then get captured in the disc by hydrodynamic drag as they cross the disc (e.g.,0
+1362,Similar outflows have been reported for,5
+1363,"and for one hot Neptunian planet, GJ 435 b",5
+1364,"Observations of the Antennae galaxies report only one TDG candidate, at the tip of the southern tail",3
+1365,but the exact nature of this structure is still questioned,3
+1366,"Our adopted classification scheme is based on physical properties of a young stellar object, such as envelope and disk masses (e.g.",2
+1367,"rather than on observational signatures, such as submillimeter luminosities or effective temperatures",6
+1368,"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.",2
+1369,"The model has been chosen on the basis of a χ2 test and, in every image, the best fit is provided by a Moffat function",2
+1370,"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.,",0
+1371,"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.",0
+1372,"Nevertheless, a recent study of the dynamics of dwarf spheroidals orbiting around the Milky Way has shown some inconsistencies with previous results",6
+1373,The escape fraction is a key parameter in studies of the contribution of the observed galaxy population to reionization,0
+1374,semi-analytic modelling of reionization (e.g.,0
+1375,Since the errors of the LIGO-estimated rates are dominated by Poisson statistics,2
+1376,"we approximate the PDF for the expected number of detections $\mathcal {N}=\mathcal {R}VT$ (from the surveyed space–time 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’s prior",2
+1377,The estimated spin-down energy is Ė = 1.36 × 1036 erg s-1 and the surface dipolar magnetic field is 7.4 × 1011 G,0
+1378,"The initial perturbation can be compensated or uncompensated, which leads to different void growth scenarios",0
+1379,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,3
+1380,"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.,",0
+1381,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.,0
+1382,"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.",0
+1383,"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.",6
+1384,"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.",2
+1385,While the composition of the target surface was different than in,1
+1386,"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).",1
+1387,"In particular, the “submillimeter-HCN diagram”, first proposed in Izumi et al. (2013) and later expanded upon in",0
+1388,"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(4−3)/HCO+(4−3) and HCN(4−3)/CS(7−6), where all of the molecules involved are considered tracers of dense gas.",0
+1389,"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 Myr of Solar system history",1
+1390,"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 km and above the detection limit.",1
+1391,"The CH and CH/CB (hereafter: CH–CB) chondrites and their components are characterized by enrichments in 15N (up to 1,100‰;",0
+1392,"Once metallicity starts to increase, low- and intermediate-mass stars release carbon and massive stars start to eject more carbon than oxygen",0
+1393,"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.,",1
+1394,These have led to the discovery of metastable maser lines in 22 different regions,0
+1395,"This is confirmed by the blind carbon monoxide (CO J = 1–0) survey of a subsample of the brightest 350 μm peakers (S350 ≥ 115 mJy), which has shown a strikingly similar redshift distribution as 850 μm selected SMGs (zCO = 2.5 ± 0.8;",5
+1396,"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",2
+1397,"For instance, a number of measurements have revealed that the stable isotopic compositions of all meteorites fall into two distinct families",0
+1398,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,1
+1399,"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 λ (e.g.",2
+1400,"; for λ = 1.25 mm, amax = 0.2 mm)",2
+1401,"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",0
+1402,Continuum and methanol line maps from Effelsberg observations have also been obtained as part of the GLOSTAR survey,2
+1403,"The bar, detected in the NIR by Quillen et al. (1997) and",0
+1404,shows a prominent boxy-shape morphology.,0
+1405,The inferred mass of the galaxy (baryons) in the best model (5.4 × 1010 M⊙) is marginally consistent with the estimated stellar mass derived from the velocity dispersion – stellar mass correlation,5
+1406,"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",3
+1407,"Many of these models,",3
+1408,can be constrained by this nonobservation at IceCube.,3
+1409,"These simulations were tailored to the BHB system H1743−332, where there is Chandra high-resolution data in both states giving detailed spectral information on the wind or its absence",2
+1410,The slopes solely inferred from the CARS data are consistent with those reported by Greene et al. (2012) and,5
+1411,and are therefore on the shallower side of previous estimates.,5
+1412,and Kitaura et al. (2012) proposed a Gibbs sampling scheme to jointly infer density and velocity fields and corresponding power-spectra.,0
+1413,"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.",1
+1414,"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",2
+1415,assuming that the positions of the point sources are known.,2
+1416,"Several ALMA blind surveys have been performed and allowed to detect and characterize the faint SMGs across cosmic times (e.g.,",0
+1417,"One can see that the larger the initial amplitude, ρIA, the stronger the decrease of the primary wave’s amplitude, which is consistent with observations",5
+1418,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,5
+1419,"but never clearly observed. These observations, for the first time, show a direct link between the cigar distribution and betatron cooling.",5
+1420,"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",0
+1421,Similar deviations are observed in,5
+1422,outer parts of HSB spiral galaxies,5
+1423,A still slower rotating model,0
+1424,"built large-scale, axisymmetric, cycling magnetic fields of somewhat lower amplitude which did not eliminate the star’s differential rotation, reminiscent of the distributed αΩ-type dynamos prevalent in solar-like contexts.",0
+1425,"kinetic instabilities such as the Buneman and modified two-stream instability (e.g.,",0
+1426,"Lastly, post-AGB stellar evolution models, computed with updated physics in a reduced mass range",6
+1427,show a strong disagreement with the previous grids.,6
+1428,"Starting from our completeness limit at 22 μm, after conservatively dereddening it by AV = 20, we assumed a spectral index γ = −2 (see Table 3 for definition) to compute the MIR luminosity from Eq. (6) of",2
+1429,From here on we present all the basic equations in the irreducible basis (see,2
+1430,for details).,2
+1431,The optical/near-IR photometry was then complemented with the 24 μm catalog,2
+1432,", built as summarized in Section 2.1 from the Multi-Band Imaging Photometer for Spitzer (MIPS) images",2
+1433,"Such a distance would make PSR J2043+2740 a viable target for deep optical observations, never carried out until now, and might be compatible with the debated association",3
+1434,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.,0
+1435,"Among the latter, Joudaki et al. (2018) recently performed a combined analysis of cosmic shear tomography, galaxy–galaxy lensing tomography, and redshift space multipole power spectra using data from KiDS-450 (∼450 deg2 of cosmic shear data from the KiDS survey) and two overlapping spectroscopic surveys, the 2-degree Field Lensing Survey4 (2dFLenS;",0
+1436,"Previous studies have classified light bridges based on their morphological properties. Light bridges separating two umbral regions are called strong light bridges (e.g.,",0
+1437,"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.,",0
+1438,are elongated bright structures that penetrate the umbra. They are composed of rows of bright grains with sizes comparable to umbral dots.,0
+1439,Following the method applied by,2
+1440,"in their Eq. (2), we plot the relation between the LTE kinetic temperature, TLTE, and the para-H2CO (3–2) line ratio in Fig. 5.",2
+1441,"The bulk SW shows a fractionation of elemental abundances correlating with FIP, as previously observed by spacecraft (e.g.,",5
+1442,"However, the better accuracy and element coverage of Genesis data compared to in situ measurements allows further insights into this FIP-related fractionation.",1
+1443,Their numerical simulations were performed using the classical version of the Mercury code,3
+1444,"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–Lidov 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.",3
+1445,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,3
+1446,", 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.",3
+1447,"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",2
+1448,induced by poor random seed choices.,2
+1449,The submm photometry of HATLAS12-00 at 890 μm acquired with the Submillimeter Array (SMA) as part of this programme,5
+1450,is fully consistent with the 870 μm and 850 μm fluxes derived for this source from the LABOCA and SCUBA2 data to be presented here.,5
+1451,"Historically, systematic studies of galactic outflows in nearby and high-z galaxies have focused on the ionized gas",0
+1452,and the atomic phase – based on the Na D or Mg II lines in absorption (e.g.,0
+1453,Relics trace ICM shock waves with relatively low (M   3) Mach numbers,0
+1454,"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.",6
+1455,"In recent years, large-area optical surveys have detected candidate TDEs emitting at temperatures of a few ×104 K",0
+1456,"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.,",6
+1457,", although they undoubtedly explain many of the observed abundance ratios.",5
+1458,"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",0
+1459,"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",2
+1460,More recent numerical and analytic models have continued in this vein (e.g.,0
+1461,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,0
+1462,near the mid-plane.,0
+1463,"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",0
+1464,It was shown by,0
+1465,that this ridge structure is governed by the degree of oscillation modes and resembles the predictions made by Ando & Osaki (1975).,0
+1466,found that the number density of massive quiescent and elliptical galaxies with Re 2.5 kpc decreases by about 30% from z~1 to z~0.2 and that their U−V 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.,0
+1467,"This is not typical for embedded clusters, which have typical half mass radii of ∼0.8 pc",6
+1468,", and therefore would have less frequent interactions between cluster stars and a particular binary.",6
+1469,"Previous works have confirmed that H-atmosphere models accurately describe the spectra of qLMXBs, with radii in the range 10–15 km, as expected for NSs, either from single sources (e.g.",0
+1470,"Alternatively, BBHs can form dynamically in",0
+1471,multiples (e.g.,0
+1472,Since in the experiment by,1
+1473,"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.",1
+1474,"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–disc interactions in more detail. There are well-known examples such as",0
+1475,and Fomalhaut having a narrow and eccentric planetesimal belt,0
+1476,"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.,",0
+1477,NGC 5813 itself has been assumed to be dynamically old,0
+1478,"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",0
+1479,These values are in the range of those observed towards the molecular clouds in the Galactic centre but lower than in Orion KL,1
+1480,"To come to a robust conclusion, independent H0 probes with accuracy better than $2{{\ \rm per\ cent}}$ are crucial",3
+1481,The underlying cause of the split tracks (see,0
+1482,for a clustering analysis into the statistical robustness of this split) for BHXBs is not known,0
+1483,"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",0
+1484,"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 (Ωϕ) and the radial or epicyclic frequency (ΩR).",0
+1485,The approximate rate of RETs (≥10−6 Mpc−3 yr−1,2
+1486,Such cores can be created within the CDM paradigm by a variety of baryonic processes (e.g.,0
+1487,"However, on the other hand, understanding of the formation mechanism of massive stars is still elusive",0
+1488,Price et al. (2010) and,2
+1489,"investigated the sizes of particles smaller than 10 μm 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",2
+1490,while the models with higher He core masses are compatible with the typical kicks of young pulsars,1
+1491,"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.,",6
+1492,"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 ≪ 1, and a more accurate expression of vertical gravity should be adopted for a slim disk",1
+1493,Because they are detected in a wide variety of interstellar sources – in hot cores,3
+1494,it is of prime importance to understand well how these precursor molecules form.,3
+1495,The points mark detections from previous studies in the literature. References:,2
+1496,All relevant numerical routines were extracted from the LLMODELS stellar model atmosphere code,2
+1497,"Nevertheless, the ‘combined’ bar fraction in Fig. 6 is not constant over (g −r) colour and agrees well with",5
+1498,for redder colours [(g −r) colour > 0.5],5
+1499,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,1
+1500,As for the main isotopolog,2
+1501,"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",2
+1502,Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S ii]/H α > 0.4–0.5,0
+1503,the stellar radius and Teff,0
+1504,"In some galaxies, the depletion time in the centres appear shorter",0
+1505,"In 2018, a new technique combining a Terahertz radiometer (41–49) 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",0
+1506,"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.",6
+1507,"Pebble accretion is a mechanism able to speed up significantly the giant planet formation process (i.e.,",0
+1508,"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.",0
+1509,"Historically, models reproducing the evolution of stellar populations and dust emission have been developed separately,",0
+1510,and a thorough comprehension of dust grains physics on the other,0
+1511,"Velocity dispersions in dwarf galaxies can be on the order of the rotational velocity, ∼10–15 km s−1 (e.g.,",1
+1512,Orbiting SMBHBs produce a stochastic GW background (GWB,0
+1513,"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",1
+1514,"In particular, an instrumental line (Cu Kα) is known to affect pn at a rest-frame energy of ~8 keV",2
+1515,"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.",2
+1516,"Since then, these two methods have been widely used to explore the cosmic anisotropy",0
+1517,"by investigating observational data of, for instance, the Union2.1 sample",0
+1518,"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",0
+1519,The blue bump appears mainly due to the presence of late-type WN (WNL) and early-type WC (WCE) stars,0
+1520,The M-type sample consists of the non-Mira stars from the General Catalog of Variable Stars (GCVS;,2
+1521,"with quality flag 3 in the IRAS 12, 25, and 60 μm bands and 60 μm flux ≳3 Jy",2
+1522,"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 ${\tt{\rm simpl}}$,",2
+1523,to generate the Compton component;,2
+1524,while the post-shock temperature in the hot halo near Rv may only be ∼0.5Tv,2
+1525,", P18).",2
+1526,It is worth noting that the original samples from,1
+1527,and Bernard-Salas et al. (2009) have spectra solely covering the central region of the galaxies.,1
+1528,The center-to-limb variations ofintensity I(μij) and polarization P(μij) were found through trilinear interpolation using the look-up tables from Kostogryz & Berdyugina (2015) and,2
+1529,", according to the selected wavelength, surface gravity, and temperature of a star.",2
+1530,The Kamioka Gravitational Wave Detector,0
+1531,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 M⊙,0
+1532,We then attempted to unify the data for each filter to a consistent zero point by using ensemble photometry,2
+1533,"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.",0
+1534,"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.′′ 267 away in 1993 and moving away from the primary",0
+1535,We also plot the SFR in the outer regions of spiral galaxies,2
+1536,square symbols).,2
+1537,"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",2
+1538,"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",5
+1539,"The mass accretion and loss rates for Class 0/I low-mass protostars span the range of 10−6–10−8 M⊙ yr−1, and the derived jet efficiencies (ratio between mass ejection and accretion rates) range between ∼1 per cent and 10 per cent (e.g.",0
+1540,These measurements are within the range predicted by the magnetohydrodynamic jet launching models,5
+1541,"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",0
+1542,"For example, shown in Figure 1 are the values of symmetry energy at 2ρ0, that is, Esym(2ρ0), from",2
+1543,(6),2
+1544,"analyses of NS radii, tidal deformability, and maximum mass within an extended Skyrme Hartree–Fock approach (eSHF)",2
+1545,"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(2ρ0) = 47 MeV within the still relatively large error bars of the individual analyses.",5
+1546,"A second, fast path involves a downward transition in the mass–size plane, at approximately constant redshift",0
+1547,This process requires a substantial “compaction” of the formally extended star-forming galaxies.,0
+1548,"In LTE, a linear dependence of the core/wing ratio is expected (e.g.,",1
+1549,"but such dependence is probably less obvious for the Mg ii h and k line, whose cores form in NLTE conditions.",1
+1550,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,3
+1551,Radio observations were provided by,2
+1552,and the High Energy Telescope,2
+1553,"Plin represents the real-space, linear matter power spectrum for which we use the CLASS Boltzmann solver",2
+1554,"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",1
+1555,"It has a (energy-dependent) angular size of ∼0.1° and its distance has been estimated to be ≈2.2 kpc, corresponding to a physical size of ≈3.8 pc",0
+1556,"At large galactocentric radii (>10 kpc) this includes, among others,",0
+1557,"and streams of stars kicked up from the disk that undergo phase mixing, sometimes referred to as “feathers�� (e.g.,",0
+1558,"with a sample of 322 giants, including 10 planet-hosts, did not find any metallicity offset.",1
+1559,"Bars in spiral galaxies may drive gas inflows, which enhance central star formation (bar-driven evolution;",0
+1560,"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 20−30 pPa, according to Jian et al. (2006).",2
+1561,"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 × 10−10 m s−2",0
+1562,"Different types of software, such as lenstronomy",0
+1563,can handle the inference of lensing quantities from mass maps using fast Fourier transform convolution.,0
+1564,"As mentioned in Sect. 5.7, the 13CO/C18O abundance ratio increases in regions of enhanced UV field",2
+1565,This category is similar to the ‘uncertain’ (UNC) class introduced in,5
+1566,"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.",5
+1567,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 ∼30 K even at several tens of au up to 100 au from the centre,7
+1568,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,3
+1569,It has only recently become widespread to model the formation of galaxies ab initio,3
+1570,and the realism continues to improve,3
+1571,It was the first source identified as a hot corino,0
+1572,"based on the detection of Complex Organic Molecules (COMs) in the source, which was later supported by follow-up studies",0
+1573,"In the case of pre-ELMVs,",0
+1574,and nonradial p- and g-mode pulsations,0
+1575,"revealed that the excitation is probably due to the κ − γ 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.",0
+1576,"Surprisingly, we observe that this data reduction change was only applied to the Balmer β, γ, and δ lines but not applied to the Balmer α 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 α is found in SDSS data releases 9 up to now, i.e. the latest data release 14",1
+1577,"It is more similar to the extremely low values of [14N/15N] found in primitive solar system material, like cometary CN and HCN",5
+1578,"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",0
+1579,"Paper II, hereafter).",0
+1580,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,3
+1581,The most well-known stellar stream in this region is the Monoceros Ring (e.g.,0
+1582,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,0
+1583,These values are consistent with the current observed SFR in the Milky Way,5
+1584,"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.",2
+1585,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,2
+1586,"Usually, we see a decay in magnetic field strength as solar-type stars evolve, as their activity decreases along with their rotation",1
+1587,"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.",1
+1588,Theoretical works,2
+1589,"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 ${\sim}0.5{{\ \rm per\ cent}}$.",2
+1590,"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.",2
+1591,"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",2
+1592,"However, previous results show that fast CME would decelerate during their propagation in interplanetary space (e.g.,",1
+1593,"Moreover, several molecules were detected and resolved toward NGC 1068 with interferometers in the past few years",0
+1594,The Fκ-test is preferred when the magnitude difference between the object and comparison stars is large,1
+1595,derived values of 0.15–0.25,2
+1596,"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.",2
+1597,are at the levels of >4σ for the analysis of,1
+1598,"Multiple feedback mechanisms influence disc evolution. In sufficiently dense environments, star–disc encounters can truncate the disc and induce increased accretion rates",0
+1599,"Accordingly, numerous studies were focused on peak fluxes of SEPs and corresponding acceleration and transport processes (e.g.,",0
+1600,"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",1
+1601,"VLA observations of the NH3 inversion lines (1, 1) and (2, 2) seen in absorption (1\hbox{$\farcs$}.̋1 beamsize) revealed radial infall on scales larger than 5000 AU toward the W51e2 core",0
+1602,"The RXTE observed another outburst in 2002 and re-established its cyclotron resonance feature corresponding to a centroid energy at 30.7 ± 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",1
+1603,QSO flux measurements that reach to z ∼ 7.5,0
+1604,"the absorbed doses used in our fixed energy experiments change from ~ 2 to ~ 15 MGy, whichis quite similar to the absorbed doses in",5
+1605,"In the linear perturbation theory limit of the MHD equations, δB2 includes contributions from shear Alfvén, fast and slow magnetosonic compressive eigenmodes (e.g.",2
+1606,We do detect starburst-like behaviors in galaxies on the main sequence,1
+1607,likely linked to the existence of transitional objects,1
+1608,to limit the references to recent works based on submillimeter observations,1
+1609,"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.,",0
+1610,This limit is referred to as the quasi-static approximation to MHD,0
+1611,although recent numerical studies on its turbulent properties and anisotropy have been done as well,0
+1612,"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.",0
+1613,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.,0
+1614,"In particular, the Magnetospheric Multiscale (MMS) mission has contributed greatly to the kinetic physics of magnetopause reconnection",0
+1615,see fig. 1 of,0
+1616,"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.",0
+1617,"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.",0
+1618,The possible change of macroscopic magnetic moment of pulsars at the moment of a glitch occurring was discussed by Link and Epstein,0
+1619,We use the same normalization,2
+1620,"where time, radius and velocity are normalized to the outer radius a, the resistive diffusion time τR = a2/μ0η, and the Alfvén velocity $V_{\rm A} = B_0/\sqrt{\mu _0 \rho _0}$, respectively.",2
+1621,"As of today, many more mass ejection channels have been discussed:",0
+1622,as MHD-driven winds,0
+1623,"Unfortunately, the previous work does not cover all the phase angles of the images we investigated, but the spectral slope variation between 35–54° (Fig. 3 of",1
+1624,"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° phase angle (image #4), the spectral slopes would vary from 15%/100 nm to 18%/100 nm in the observations we used.",1
+1625,"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",0
+1626,"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.,",0
+1627,A contact binary could result from,1
+1628,(ii) the disruption of a monolithic object due to excessive spin-up resulting from non-gravitational forces or YORP5 effect followed by a reaccretion,1
+1629,"If the pairs are produced via TeV–eV collisions (i.e., via the second path) outside the gap outer boundary, they have outward ultrarelativistic momenta to easily “climb up the hill” of the potential k0",1
+1630,see also Figure 2 of HP16) and propagate to large distances without turning back.,1
+1631,Considering that the relation between the gas temperature and the para-H2CO line ratio may vary at different spatial densities (see Fig. 2 in,2
+1632,"we modeled it at spatial densities 104, 105, and 106 cm−3 in Fig. 5.",2
+1633,"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",1
+1634,"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",2
+1635,The blue squares are data from the GAMA galaxy survey,2
+1636,We probed four orientations for the simulated outflows,2
+1637,the jet direction claimed by,2
+1638,"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.",0
+1639,"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",2
+1640,"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",5
+1641,When the magnetic field lines are parallel it is not easy to have reconnection,2
+1642,"Hereafter, we adopt natural units c = ℏ = 1. have been reported (see, e.g.,",2
+1643,There remains much debate in the literature on the origin of such axisymmetric substructure in protoplanetary disks including,3
+1644,"and toroidal dust traps created by hydrodynamic or magnetohydrodynamic effects (see, e.g.,",3
+1645,The existence of an early ocean is supported by,0
+1646,and from records of the oxygen isotope composition of seawater,0
+1647,"However,",0
+1648,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 (λλ 5000−5350 Å).,0
+1649,"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.",1
+1650,"This cluster has about solar metallicity ([Fe/H] in the range −0.04 to +0.03, e.g.",3
+1651,"Nevertheless, it still faces numerous challenges on galaxy scales. Among these, the most important ones are",0
+1652,or the unexpected diversity of rotation curve shapes at a given mass scale,0
+1653,While the PHIBSS project estimated molecular gas masses by measuring the CO(3–2) line emission,1
+1654,"Scoville et al. (2016, 2017) used the flux on the Rayleigh–Jeans tail of the dust continuum emission to estimate the total gas masses.",1
+1655,"Complementing these observations, the spectroscopic confirmation",0
+1656,"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.",0
+1657,"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",3
+1658,Set II: we now focus on the observational constraints on the model parameters after the inclusion of the local measurement of H0 by,2
+1659,"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.",2
+1660,"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 Δ[Na/Fe] ∼ 0.20 dex, which is comparable to that expected from our chemical evolution model for the bulge stars (Δ[Na/Fe] = 0.2 ∼ 0.3 dex;",5
+1661,"As an example, it has been known for several decades that the Galactic disc contains large-scale non-axisymmetric features, including",0
+1662,a warp,0
+1663,"In low radio states, it has also displayed evidence of a high-ionization X-ray-absorbing wind",0
+1664,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.,2
+1665,"However, the complexity of such simulations obscures the physical mechanisms through which these processes affect the dark matter distribution. These mechanisms normally invoke ‘heating’ of the cold central density cusp through an irreversible process, such as dynamical friction from infalling clumps",0
+1666,"In the jet model, such a p can also reasonably account for the very late flux decline of",2
+1667,"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;",1
+1668,it could be that Oort Clouds are relatively rare.,1
+1669,"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",0
+1670,or white dwarf−white dwarf mergers,0
+1671,"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",5
+1672,Absorption band shifts of CO ice in the UV and IR ranges only occurred at deposition temperatures above 20 K,0
+1673,"suggesting that CO ice grown at lower temperatures is amorphous below 20 K 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.",1
+1674,"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",2
+1675,In the seminal work of BPS,0
+1676,the nuclear masses for the outer crust were provided by an early semi-empirical mass table.,0
+1677,"The corresponding EoS is seen to display a similar pattern with the BCPM, FRDM, and BSk21 results in Fig. 2.",5
+1678,These soft residuals are known to be a common feature in the spectra of ULXs and bright X-ray binaries,5
+1679,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;,5
+1680,"Modelling of DLAs observations suggests that DLAs resemble rotating disc galaxies with circular velocities typically of the order of $100\!-\!200\, {\rm km\, s}^{-1}$",0
+1681,Findings by,6
+1682,", on the other hand, show that the (nh + ns)/nc ratio remains roughly constant with heliocentric distance in the slow wind, suggesting a lack of interchange between the thermal and suprathermal populations.",6
+1683,These three protostars are all embedded in dense cores with masses ≳0.5 M⊙,3
+1684,"Therefore, they are excellent targets by which to study the gas motions on a 100 au scale at an early evolutionary stage.",3
+1685,"In observed spectra, recurrent frequency spacings that may correspond to the large separation or half its value have been found in some stars",0
+1686,"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",5
+1687,"However, our result is consistent with other NLFFF results",5
+1688,"The composite SED was reddened according to the new family of optical and near-infrared extinction laws for O-type stars provided by Maíz Apellániz et al. (2014), which constitute an improvement of the widely used extinction laws by",2
+1689,"For instance, thioformic acid (HC(O)SH) was very recently detected in G+0.693–0.027. Its trans-isomer has an abundance of ~1 × 10–10",0
+1690,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,0
+1691,"Studies suggest that this valley likely marks the transition from the smaller rocky planets: ‘super-Earths’, to planets with significant H/He envelopes typically containing a few per cent of the planet’s total mass: ‘sub-Neptunes’ (e.g.",0
+1692,Spacecraft observations show that wave potential structures of Gaussian form are common in space and astrophysical plasmas,2
+1693,We assume this potential well to have Gaussian form,2
+1694,"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.,",0
+1695,"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",0
+1696,"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",1
+1697,"Such transition might well imply an imminent increase of the SFR, driving the object in the realm of starbursts",1
+1698,"or its cessation, bringing the system back onto or even below the main sequence",1
+1699,with the CO properties potentially able to distinguish between these two scenarios.,7
+1700,The complex dielectric functions of the samples obtained by heating bayerite and boehmite to various temperatures,2
+1701,were derived by modeling the reflectance spectra of pellets obtained by pressing powders of these materials under great pressure,2
+1702,The avoidance of its going into CE evolution is – as we will argue – a consequence of the donor star having a radiative envelope,2
+1703,"In such a case, when the emission beam is confined by dipolar open field lines, we would expect a P− 1 / 2 dependence, which has indeed been observed when correcting for geometrical effects by transforming the pulse width into a beam radius measurement (see",1
+1704,"This effect has been considered in numerical models of GCR modulation to study the long-term modulation mechanism (e.g.,",0
+1705,"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",0
+1706,POWR,0
+1707,"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",1
+1708,"However, even in ellipticals, large differences prevail. Recent observations of elliptical galaxies with Spitzer and Herschel",0
+1709,have revealed that the far-infrared (FIR) luminosity LFIR from these galaxies can vary by ∼100 among galaxies with similar optical luminosity.,0
+1710,"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−1",0
+1711,"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",3
+1712,"Several explanations about their origin have been put forth. Among these theories, interchange reconnection is the most focused upon",0
+1713,"In this scenario, switchbacks are generated in the solar corona, and form at the reconnection sites between open and closed magnetic fluxes.",0
+1714,"However, more recent studies",1
+1715,have revealed small non-mass-dependent variations in Fe isotopes.,1
+1716,"This relation has been further extended to high redshifts, using deep near-infrared (IR) spectroscopy facilitated by large ground-based and space-based telescopes",0
+1717,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,0
+1718,"Toward this goal, conventionally, new summary statistics that can only be measured with imaging have been proposed. These include",0
+1719,bispectrum,0
+1720,"The [C ii]158 μm line is typically the brightest in star-forming galaxies, arising from ionized, and even neutral gas where it is the main coolant",0
+1721,"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.",0
+1722,"Moreover, it was found that the highest dust temperature at which H2 can be formed efficiently is less than 17 K",0
+1723,and through diffusive flux,0
+1724,"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",0
+1725,"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",3
+1726,Whilst this higher total disc mass is still consistent with the dust mass measurements of protoplanetary discs,1
+1727,"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 ‘disc mass problem’, see",1
+1728,The (CH2OH)2/CH2OHCHO abundance ratio of ~0.3–0.5 previously derived in IRAS 16293 by,6
+1729,was revised.,6
+1730,"Some studies find weak statistical links among AGN activity and the presence of bars (e.g.,",0
+1731,"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.",2
+1732,"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",0
+1733,The sample used in this paper is primarily drawn from Sloan Lens ACS Survey (SLACS),2
+1734,The combined sample includes 91 lenses from SLACS,2
+1735,"Using Ks-band (2.15 μm) direct imaging andH-band (1.65 μm) polarimetric imaging with the High-Contrast Instrument with Adaptive Optics (HiCIAO) at the Subaru Telescope,",0
+1736,detected two spiral arms and polarized light down to 0.′′ 1 (15 au) from the star.,0
+1737,"Second, the mass distributions of single and binary sdB stars are indistinguishable (",3
+1738,", Table 3 in particular).",3
+1739,"The choice of SED is very important in the BLR modeling, as different lines respond to the continuum variations on different time scales",3
+1740,"Previous sub-arcsecond angular resolution N-band (∼8–13 μm) ground-based spectroscopic studies investigated the 11.3 μm PAH feature in the nuclear and circumnuclear regions of AGN (e.g.,",0
+1741,"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.",3
+1742,we estimated several dynamical properties of the clusters in the point source sample and compared them with the extent-selected sample presented in,2
+1743,Between the end of inflation at t = te ∼ 10−33 s; (e.g.,0
+1744,"and t = teq = 2.37 × 1012 s, the Universe was radiation-dominated since at the latter instant a radiation-matter equality is reached (Table 1).",0
+1745,"Furthermore, discoveries of atmospheric chemical species allow us to better understand various thermodynamical processes and chemistry, winds in the upper atmosphere",0
+1746,The observations of NGC 1333 IRAS4A and IRAS16293 are presented in Girart et al. (2006) and,0
+1747,respectively.,0
+1748,"Together, these properties lead to the result that an ANN can be trained to provide accurate and practical solutions to Newton’s laws of motion, resulting in major improvements in computational economy",3
+1749,relative to modern technologies.,3
+1750,There are various observations of flux ropes in the,0
+1751,"and solar wind (e.g.,",0
+1752,"At 8.7 GHz we find a PA of 25° ± 5° 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° in the epochs from 1995 to 2013 at angular scales ∼5 mas",1
+1753,"Magnetic field fluctuations have been characterized with great detail at magnetohydrodynamic and kinetic scales, for example, through spectral and high-order moments analysis",0
+1754,"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",0
+1755,"The large scale outflow is observed in CO emission at millimeter wavelengths, with both the red and blue lobes being about 100″ in extent",0
+1756,"In this very region, the analysis of heliospheric imaging (HI;",0
+1757,"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 “flocculation.”",0
+1758,"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",0
+1759,Those cavities have been suggested to exist at ∼pc scales at least for XTE J1550–564 and H1743–322,2
+1760,"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",1
+1761,"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.,",0
+1762,"Alternatively, small dense structures can be temporary density fluctuations frequently created and destroyed by supersonic turbulence (e.g.,",0
+1763,We note that some of our data fits the observational findings of,5
+1764,represented by diamonds over-plotted on the power spectra,2
+1765,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.,1
+1766,"In the absence of QED vacuum polarization effects, this would produce a drastic depolarization of the radiation collected at infinity",0
+1767,see also,0
+1768,"This could stem from the fact that the galaxies studied by Holt et al. (2011),",1
+1769,"are local luminous or ultra-luminous infrared galaxies (U/LIRGs), and those of Villar Martín et al. (2014, 2015) are highly obscured Seyfert 2, thus sampling sources that are more gas and dust rich compared to our sample.",1
+1770,We do detect starburst-like behaviors in galaxies on the main sequence,1
+1771,likely linked to the existence of transitional objects,1
+1772,"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",0
+1773,This chemical scheme was implemented in a chemical model by,0
+1774,to explain the abundance of cyanoallene in TMC-1.,0
+1775,The soft X-ray region of the reflection spectrum is also the most sensitive to modelling assumptions such as vertical disc structure,1
+1776,"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–metallicity relation of z ∼ 2 star-forming galaxies (e.g.",5
+1777,"compact blobs instead show metallicities inconsistent with the mass–metallicity relation (Fig. 7, bottom right panel).",6
+1778,"However, the mean length for QS network jets is smaller (3.53 Mm;",1
+1779,"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;",2
+1780,Figure 5 shows the comparison between our EWs measurements and the line strengths measured by,1
+1781,(in both cases the sum of the two strongest lines) for the five calibration clusters.,1
+1782,"The observed scatter is consistent with the internal errors of the EW measurements,",5
+1783,"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",3
+1784,all lead to local and non-local oscillations in the spectrum.,3
+1785,"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 (∼0.3 dex) between the SFR and stellar mass, M⋆",0
+1786,"In a shearing disc, if the cells adapt in a truly Lagrangian manner, then they are inevitably deformed into a highly sheared/irregular shape",1
+1787,"Several strong processes have been proposed and observed, such as harassment (e.g.",0
+1788,"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",0
+1789,"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.",1
+1790,"If the cirrus ISM component heated by the more general galactic UV radiation field contributes to LIR, then the",1
+1791,relationship overestimates the SFR.,1
+1792,We then remove the cosmic rays using the LACosmic algorithm,2
+1793,"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)",0
+1794,"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.,",0
+1795,Two orange peaks represent the cool lines of O I 1354.60 Å and C I 1354.84 Å,2
+1796,which are far away from the flaring line of Fe XXI 1354.08 Å.,2
+1797,A CO spectroscopic redshift of 3.26 was first suggested by Z-spec,5
+1798,"observations, then subsequently confirmed by observations",5
+1799,and the Zpectrometer instrument,5
+1800,on the Greenbank Telescope,5
+1801,The most stringent and precise constraints on the self-interaction cross-section have been put on the scales of galaxy clusters (e.g.,1
+1802,"where observations require that $\sigma _T/m_chi \lesssim 1\, {\rm cm^2g^{-1}}$.",1
+1803,This form of joint analysis is already being explored within the framework of WMAP,0
+1804,and LiteBIRD,0
+1805,in combination with Planck Low Frequency Instrument data,0
+1806,"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.,",0
+1807,Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S ii]/H α > 0.4–0.5,0
+1808,We adopt a four-level AR classification scheme based on the maximum GOES-level flare an AR ever yields,2
+1809,Al i lines at 6696 and 6698 are used for deriving the Al abundance and these lines have negligible contributions from NLTE effects,2
+1810,As pointed out in,5
+1811,"we found clear evidences of pulsation phase variability with a maximum change of 2 × 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.",5
+1812,The dust radiative transfer and photosionisation code mocassin,2
+1813,"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–bound continuous emission data of Ercolano & Storey (2006).",2
+1814,For BH-LMXBs,0
+1815,and the X-ray spectrum can be well described by a multicolour blackbody spectrum (e.g.,0
+1816,"Equilibrium tides become then effective (e.g.,",2
+1817,and references therein) and the tidal evolution may occur on a longer timescale.,2
+1818,"For instance, for the Lyman α radiation χνr = 0.042 for optimum efficiency χo = 0.1",2
+1819,"In particular, there are currently five main competing models.",0
+1820,(2) Empty Asteroid Belt: embryos and planetesimals in the protoplanetary disk formed concentrated within a narrow belt at ∼0.7–1 au,0
+1821,In what is called the “frozen-screen” hypothesis,0
+1822,"these pockets, or turbulent eddies, are assumed to be fixed in the atmospheric layer that advects over an interferometric array",0
+1823,The dark and light shaded areas in Fig. 10 correspond to the 1σ and 2σ constraints on the redshift of reionization from the cosmic microwave background measurements of the Planck mission,2
+1824,with a reionization midpoint zre = 7.67 ± 0.73.,2
+1825,Previous sub-arcsecond angular resolution N-band (∼8–13 μm) ground-based spectroscopic studies investigated the 11.3 μm PAH feature in the nuclear and circumnuclear regions of AGN,0
+1826,"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.",3
+1827,"In particular, the asymmetric Lyα line profile has enabled redshift confirmations of large samples of sources at both 2  z  6 (e.g.,",0
+1828,The faster solar wind tends to be more imbalanced with greater wave energy flux antisunward than sunward,0
+1829,"In addition, another classification scheme uses a scatter plot of flux and duration fitted with two-dimensional Gaussian functions",1
+1830,"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",2
+1831,"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",0
+1832,"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",0
+1833,"Prior to complete gas removal, moderate values of ram pressure have also been shown to increase the star formation rate in galaxies both observed",0
+1834,and simulated,0
+1835,"However, close encounters with the planets proved not to be enough for creation of the current population of binary systems",0
+1836,Choosing values of these parameters that are consistent with simulations (e.g. those of,2
+1837,"Magnetic reconnection rapidly converts magnetic energy to particle energy, causing emission flare in multiple wave bands and even triggering coronal mass ejections",0
+1838,"So, the mean length for QS network jets from the present work is in good agreement with",5
+1839,We note that a hotter disk during maximum was predicted by a simpler study in the past,5
+1840,"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.",0
+1841,"In Fig. 10, we show the relation between the size and star formation rate of clumps, including samples across different redshifts",2
+1842,Our sample,5
+1843,"despite being at z ∼ 2–6, have sizes comparable to local H ii regions and GCs",5
+1844,but they have SFRs ∼300 times higher.,6
+1845,"However, a study of non-convex shape models for fast two to four hour rotators in",5
+1846,"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.",5
+1847,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.,2
+1848,for a more recent compilation,2
+1849,"Similar signatures were also reported in observations (e.g.,",5
+1850,"For reference, the dark red crosses also show the equivalent satellite/central red galaxy wg + correlations from KiDS×GAMA here (c.f.",2
+1851,"fig. 7, red points/band).",2
+1852,"On large scales at least, our illustristng red sample is consistent with their measurements.",5
+1853,"There are a few interesting features here to note, however.",1
+1854,"Although the general trends match the real data,",5
+1855,"with ss and to a lesser extent cs exhibiting strong scale-dependent IAs in this regime, the magnitude is somewhat higher in our sample.",6
+1856,"This is particularly interesting, given that our sample characteristics are similar (〈L〉/L0 = 0.91 and 0.34 for our red and blue samples, respectively, compared with their ∼0.99 and 0.50).",1
+1857,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,0
+1858,or the continuous large-scale matter distribution (cosmic shear;,0
+1859,The [C ii] deficit persists when including high-z galaxies (e.g.,3
+1860,This problem is also known as the Cosmological Lithium problem,0
+1861,"Over that time they have been assigned different terms, such as",0
+1862,"coronal waves (e.g.,",0
+1863,"For comparison, we show published observations in the same redshift range from the literature in the right panel of Figure 5",2
+1864,We estimated using the,2
+1865,IMF the expected range for the observed M/OB number ratio.,2
+1866,"Minkowski functionals, which are also closely related to the crossing statistics",0
+1867,and have been utilized for cosmological random fields,0
+1868,This phase motion has been seen in magnetospheric data of Alfvén waves,2
+1869,and the simulations of coronal oscillations by,2
+1870,These studies note that the direction of motion is related to the spatial variation of ωc.,2
+1871,"Energetic electrons are unstable to Langmuir waves, thus they are converted into radio emission at the local plasma frequency and its harmonic (see",0
+1872,"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.",1
+1873,"Fourthly, with the NIST data base",2
+1874,which is considered as the most critically analysed data base.,2
+1875,Comparison with observed energies,5
+1876,and with the NIST values shows that the present ab initio values are not fully converged to experimental values.,5
+1877,"The hybrid source XTE J1701–462 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",3
+1878,"As for the planet’s phase offset,",1
+1879,and May & Stevenson (2020) favour a larger phase offset (21 ± 2 °E) than Mendonça et al. (2018) and Morello et al. (2019) (12 ± 3 °E and 11 ± 2 °E).,1
+1880,There are at least three reasons why radiative feedback is an essential ingredient of the galaxy formation process.,0
+1881,"Thirdly, it is difficult to explain the large gas turbulence values observed in star-forming regions without including the momentum input by radiation",0
+1882,"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",3
+1883,"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.,",1
+1884,"noted that heating bayerite at 500°C eliminates the XRD pattern of bayerite, and they note that at 700°C, the infrared reflectance spectrum of the boehmite sample no longer shows OH− stretching bands.",1
+1885,"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",2
+1886,"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 Hα 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",1
+1887,Early attempts of low-resolution three-dimensional numerical simulations on overshooting were made by,0
+1888,(downward overshooting),0
+1889,also showed that the MMF can be generalized for the case where the SED of the sources is not known.,0
+1890,"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).",1
+1891,"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",1
+1892,This result is inline with the number density estimate of the order of ∼10−10 Mpc−3 by,5
+1893,"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",2
+1894,that follow a dispersion relation.,2
+1895,"One warm and compact component at 200 K and a size of 0.35″ (that of the continuum compact emission obtained by ALMA Band 7 observations,",2
+1896,this mass is significantly diminished via stellar winds already during core hydrogen (H) burning,0
+1897,The Low Frequency Array,0
+1898,"has opened up new ways of studying galaxies in the radio, and a number of studies have used LOFAR’s capabilities to investigate this relationship between star formation and radio luminosity in the low-frequency regime – for example",0
+1899,"Read et al. (2018), Smith et al. (2021), and Wang et al. (2019a).",0
+1900,"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",0
+1901,Then a separation of the HC top from that of the prominence was observed during the eruption initiated by the ideal kink instability,6
+1902,"Therefore, this observation offered further important support for the idea that an HC is an MFR",5
+1903,The overall excesses within 805 and 1186 h of HESS exposures,2
+1904,"Most of the radiative models for Sgr A*, which are based on post-processing GRMHD simulations, assume that electrons have a thermal, relativistic (Maxwell–Jüttner) distribution function, and that the proton-to-electron temperature ratio is constant across the simulation domain",0
+1905,There are indeed indications that the buildup of the ice in cold environments results in the formation of pores as shown b,0
+1906,and simulations,0
+1907,"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.",0
+1908,This geometric advantage is shared with the related analysis technique of spherical Fourier-Bessel (SFB) decomposition,5
+1909,"which, in addtion to spherical harmonic decomposition, involves a further Fourier-Bessel transform and data-compression along the line-of-sight.",0
+1910,"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.",6
+1911,While Sn can also be formed from pure H2S ice by photo processing,1
+1912,"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.",1
+1913,"However, for heavily accreting massive YSOs the onset of the H II region could be delayed via stellar bloating",0
+1914,"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 (≪10−3 M⊙ yr−1), or growth beyond ~30−40 M⊙, will result in the YSO contracting to a “main-sequence” configuration, heating significantly, and being able to create an H II region.",0
+1915,"When we change the magnitude of two tides, the final location of the planets can be adjusted",2
+1916,"Concerning the other far-IR PACS band (100 μm) and the mid-IR 24-μm band, we use the association available in the DR1 release and based on the maximum likelihood technique",2
+1917,"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",2
+1918,"At higher Eddington ratios of Lbol/LEdd ≳ 10−2, single-epoch X-ray and UV observations of large samples of AGN have previously revealed a hardening of αOX as Lbol/LEdd drops from ∼1 to ∼10−2 (e.g.,",0
+1919,"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",2
+1920,"We find here that about two free-fall times (as defined for cylindrical systems, see",2
+1921,are sufficient to reach core deuteration fractions of ≳0.1.,2
+1922,"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;",1
+1923,"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",7
+1924,"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.",0
+1925,The growth of dust grains through accretion in the ISM has been proposed as a solution (e.g.,3
+1926,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,3
+1927,"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.",0
+1928,High-ionization UV lines have been detected in the spectra of z ≳ 2 galaxies through,0
+1929,spectral stacking,0
+1930,"The EWs of He II, O III]λ1666, and C III] from these works are larger than those measured in the average spectra of our LAEs, with the exception of",5
+1931,some of the stacks from,5
+1932,The EWs from,6
+1933,are computed from average spectra of a z ≈ 3 LAE population whose median UV luminosity is about two orders of magnitude brighter than ours.,6
+1934,"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",2
+1935,also on the sphere,2
+1936,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,0
+1937,and experimentally studied by Dulieu et al. (2013) and Minissale et al. (2016).,0
+1938,"On the other hand, c-C3H2 is mainly formed in the gas phase",0
+1939,"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.",0
+1940,This gas rich in C atoms is expected in the outer envelope of an externally illuminated dense core,0
+1941,"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.",6
+1942,To date our knowledge of GRGs (see e.g.,0
+1943,"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 – LOFAR – 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.",0
+1944,"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",7
+1945,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.,7
+1946,"Within a 500 arcsec radius centred on NGC 346, we find an atomic gas mass of 2.7×106 M⊙ using the Parkes+ATCA H i map",2
+1947,"Analysis of Chandra observations revealed a hole or bubble within the ICM, cospatial with the eastern lobe of the jet",0
+1948,By using the RADEX2 dense cloud models developed by,2
+1949,"to reproduce the HCN(3–2)/(1–0) 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)",2
+1950,The HB pattern is generally observed in the subcritical regime and the DB pattern is observed in the supercritical regime,0
+1951,Previous 12CO observations either reported no detection of outflow emission toward this source,1
+1952,or only weak compact blueshifted emission towards east of the continuum source,1
+1953,The [OII]λ3737 emission traces on-going star formation,0
+1954,but it also depends on the metallicity and can be a poor tracer for dusty galaxies (e.g.,0
+1955,"Moreover, other studies have compared AGN selected from various wavebands and find that their host galaxies tend to have different properties",3
+1956,and star-formation rates (SFR;,3
+1957,"The model atmosphere used in this work was interpolated from the line-blanketed, local thermodynamic equilibrium (LTE) ATLAS9-ODFNEW grid",2
+1958,"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",0
+1959,"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.",0
+1960,"Aside from the observational implications, the planet’s 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)",0
+1961,"As a further comparison, data from the SOHO/EPHIN spacecraft (red square marker) between 40 MeV and 53 MeV are also presented",2
+1962,"The agreement appears to be good in all the three examined periods, considering both statistical and systematic uncertainties.",5
+1963,"Covering these spatial scales in ≤108 yr requires a diffusion coefficient of D ≥ 9 × 1028 cm2 s−1, which is slightly higher than observed in spiral galaxies",6
+1964,"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",2
+1965,"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",0
+1966,Current cosmological hydrodynamic simulations of galaxy formation employ a variety of subgrid models (e.g.,0
+1967,"that artificially launch galactic winds,",0
+1968,"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–K stars or the oldest Cepheids and open clusters, do not currently follow the exact location of those arms (e.g.",1
+1969,fig. 8 therein,1
+1970,The above equation should reduce to the jet Lorentz factor profile used in,5
+1971,when ζ = 1.,5
+1972,"The core stable within 200 μas constrained by the VERA can be explained by Lorentz factors within a factor of two variation for the slower ejecta, i.e., 8 ≤ Γs ≤ 17, by assuming",0
+1973,Γf/Γs ≤ 1.01,0
+1974,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,5
+1975,"When planets become massive enough, they can carve gap",0
+1976,and disturb the dynamics of the gas,0
+1977,Galaxies formed in these halos because of the cooling of,0
+1978,or molecular hydrogen,0
+1979,"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",0
+1980,The bright end of the UpSco population has been examined in X-rays,0
+1981,A full description of the GLOSTAR continuum data calibration and imaging is given in,2
+1982,"More precisely, it takes 3–4 orbits for MRI to develop and ∼10 orbits to saturate",2
+1983,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⊙ 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.,0
+1984,"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.,",0
+1985,"Our analysis was rather easy, starting from a prediction based on",2
+1986,parameters.,2
+1987,Other examples of AGN with at least two variable phases of the X-ray winds are,0
+1988,and PG 1114+445,0
+1989,"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.",1
+1990,The results were obtained implementing a Bayesian scheme that uses the spectroscopic constraints and frequency ratios as the parameters in the fit,2
+1991,", the latter being almost insensitive to the surface effects in solar-like oscillators",2
+1992,"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.",0
+1993,"This shows that for reconnection to be triggered, the enhanced electrical resistivity as well as the plasma flows are important.",3
+1994,"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.,",3
+1995,Figure 1 shows the view obtained from polarimetric observations: the left panel shows the QΦ image in the J band obtained by,2
+1996,"using SPHERE on a linear scale, and the two rings are clearly visible.",2
+1997,We also used some observational data obtained within several other programmes,2
+1998,The nuclear reaction rates are those from the NACRE project,2
+1999,", supplemented by the updated reaction rate from",2
+2000,Ccf is a factor that removes the color term from S and is a function of Johnson,2
+2001,"Intrinsic Lν(1400)/Lν(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 τ = 0.1Gyr, exponentially rising with τ = −0.1Gyr), metallicties (Z⊙ and 0.02 × Z⊙), and stellar-population ages;",2
+2002,As described in,2
+2003,BC03 provides the spectral energy distribution of stars obtained from a comprehensive library of theoretical model atmospheres (KBFA in the table).,2
+2004,"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.",0
+2005,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,1
+2006,There are at least three possible types of outflows around young stellar objects: (1) a disc wind launched from the accretion disc (e.g.,0
+2007,"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",2
+2008,"Experimental measurements by e.g. instantaneous laser tomography have given values ranging from D = 2.1−2.4 in a variety of flow geometries, with a preferred value of D = 2.35",2
+2009,If a single SMBH model with a BLR d of 95 light days is true (see,1
+2010,a differential signal would be 0.9°.,1
+2011,"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",2
+2012,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,0
+2013,"However, recent experiments indicate that this product channel occurs in only 19 percent of collisions, with 81 percent of collisions forming CH + S",1
+2014,"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",0
+2015,"The value R ≈ 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",2
+2016,"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.,",3
+2017,"However, there is indication of non-negligible poloidal fields as well as toroidal fields—resulting in helical magnetic fields—in the jet environment of other distant AGNs, which results in transverse RM gradients with no sign changes (e.g.,",0
+2018,Open clusters have been used to test the scaling relations for giants,0
+2019,RASCAS deploys a general two-step methodology (e.g.,2
+2020,"On the other hand, high values of temperature, surface density, and velocity dispersion in a turbulent ISM of starbursts and merging systems will shift αCO towards lower values",1
+2021,"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",2
+2022,Recent proper motion data confirm that most of the classical MW satellites do indeed have a common orbital plane,0
+2023,aligned with the plane normal defined by the satellite positions alone,0
+2024,"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–Paczyński test",3
+2025,There are further analytical approaches described in the literature,0
+2026,", 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.",6
+2027,"However, since the identification of the Ly α forest in hydrodynamic simulations",0
+2028,"it was realized that in the context of cosmological models for structure formation, the Ly α forest is due to a fluctuating, continuous IGM (e.g.",0
+2029,"Alternatively, the origination of giant pulses is proposed from the coherent instability of plasma near the magnetic equator of light cylinder",0
+2030,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,2
+2031,"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",3
+2032,and obtain corresponding physical parameters associated with oscillating coronal loops,3
+2033,"lists the orbital parameters (orientation and separation) of WDS 02499+0856 and gave θ = 194°, ρ = 5.66 arcsec and magnitude difference ΔV = 0.07 mag (the magnitude difference can be as large as ΔV = 0.36 mag, due to photometric variability of the eclipsing binary)",0
+2034,"Complementary to the study of the overall metallicity distribution, the abundance ratios of several other elements, such as α-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.",0
+2035,"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.,",0
+2036,"Furthermore, given the demonstrated sensitivity of computed low-energy galactic electron intensities to various turbulence quantities (see",2
+2037,", 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",2
+2038,"As motivation, we note that a variety of observations in the solar wind",3
+2039,"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 Alfvén waves (KAWs).",3
+2040,"Events that took place in the far past are expected to have induced a thickening of the early Galactic disc,",0
+2041,"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",0
+2042,There have not been many simultaneous multi-wavelength studies of flaring stars,3
+2043,"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.",3
+2044,"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",0
+2045,have been considered as valid 'recent time' quenching candidates.,0
+2046,"There are a number of such ground-based experiments, including",0
+2047,the Shaped Antenna measurement of the background RAdio Spectrum (SARAS;,0
+2048,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,5
+2049,"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.",0
+2050,"While the K2 optical data set detected a 3.3 day periodic 1% photometric modulation, it is not present in the Spitzer observations",6
+2051,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.,1
+2052,Conversions to magnitude are based on the standard zero-points in the Vega system as described in the ACS Data Handbook,2
+2053,"At high accretion rate, the inner region of a standard α-disc",2
+2054,Recent works suggest that the deformation of the magnetic field lines is determined by the parameter δ (the ratio of the gravity to the magnetic pressure),0
+2055,Bayesian reconstruction methods have become increasingly popular in cosmology and have been applied in a range of different applications such as,0
+2056,weak lensing,0
+2057,"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",0
+2058,"In what are sometimes called ‘semi-empirical’ 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",0
+2059,"In the case of midplane spiral structures, their origin may be linked to the presence of a companion—stellar, fly-by, or planetary",0
+2060,"However, it differs from Eq. (2) in",6
+2061,The accretion of gas and the dynamical evolution of BSBHs are likely to be coupled,0
+2062,such that the occurrence rate of BSBHs depends on the initial conditions and gaseous environments at earlier phases,0
+2063,"For comparison, we also show the integral number count",2
+2064,and from the high-resolution ALMA follow-up of LESS,2
+2065,"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.,",0
+2066,since it depends on the particular source of turbulence.,0
+2067,"These pads provide the digital readout of the detector up to 22 particles m−2, allowing the count of the air shower charged particles without any significant saturation up to primary cosmic-ray energies of about 200 TeV",0
+2068,"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",0
+2069,"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",2
+2070,using GALEX data from,2
+2071,"we find log FFUV/FJ = −2.49, log FNUV/FJ = −2.11",2
+2072,Analytical fits of these neutron-star EoSs have been constructed in order to facilitate their inclusion in astrophysical simulations,0
+2073,whereas in,5
+2074,and Mennella et al. (1998) and in the present study this correction was not applied,5
+2075,The majority of observed SPDBs are connected to solar flares,0
+2076,"On the other hand, the annual variation in the IMF polarity in the band of 256–512 days, which is referred to the Rosenberg–Coleman effect",2
+2077,"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–Coleman effect had been confirmed by the IMF Bx component during 1964–2002.",1
+2078,Such a model is used to study,0
+2079,flows of accreting matter in neutron stars,0
+2080,This can be done either in the EoS parameterizing methods,5
+2081,or the nonparametric approach,5
+2082,and the results are well consistent with each other.,5
+2083,"Moreover, in DR processes, the H ejection is in general favoured more than H2 ejection",1
+2084,"Currently, there are two possible scenarios on the origin of S0 galaxies.",0
+2085,The other is that S0 galaxies are intrinsically different from spiral galaxies since their formation,0
+2086,"In this respect, GRGs have a crucial role in the acceleration of cosmic rays over large cosmic scales (e.g.",3
+2087,"Gap-type emission models offer a promising alternative and different realizations have been proposed in the literature (e.g.,",3
+2088,The correlated angular momenta result into correlated inclination angles of neighbouring galaxies and thus ultimately into correlated ellipticities,2
+2089,We address this issue by calculating local number density of galaxies using kth nearest neighbour method,2
+2090,"It is supported by correlated optical/γ-ray flares in FSRQs (e.g.,",5
+2091,"Thus, for planets in the Solar System, it was shown both in the observations",1
+2092,that the presence of a weak magnetic field can intensify atmospheric escape.,1
+2093,"Numerous investigations of tidal activity on extrasolar planets have been conducted, with a range of topics",0
+2094,issues of spin dynamics,0
+2095,The inner few arcseconds is a complex mix of,0
+2096,"polarized, broad optical emission lines due to scattering by dust",0
+2097,It has been suggested,0
+2098,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.,0
+2099,Some of these fragments have been recovered,0
+2100,and 2016–2017,0
+2101,"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.,",2
+2102,"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.",5
+2103,We also plot the results of previous blank-field surveys,2
+2104,This model has been previously used for the modelling of planetesimal formation in PPDs,0
+2105,The size distribution is probably shallower,1
+2106,"All our low-mass galaxies are characterized by moderate Ly α luminosities in a narrow range between 1042.19 and 1042.74 erg s−1 (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 ∼1 order of magnitude higher than those for GPs (black asterisks;",1
+2107,While the fluorescent signal powered by the diffuse metagalactic UV background,0
+2108,"with an expected surface brightness (SB) of $\rm SB_{Ly\alpha }\sim 10^{-20} \,erg \,s^{-1} \,cm^{-2} \,arcsec^{-2}$",0
+2109,is still out of reach for current optical instrumentation (but see,0
+2110,"Ly α fluorescence is predicted to be boosted up into the detectable regime in the vicinity of bright ionizing sources, as luminous quasars",0
+2111,"In literature studies, CO line ratios do appear enhanced in low-metallicity regions or galaxies (e.g.,",0
+2112,The NFW profile has been shown to provide an overall good agreement with observations and simulations over a broad range of scales in GR,5
+2113,"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 ~ 5.5–10,",0
+2114,the bulk of the galaxy population residing in the early Universe does not contain such phenomena,0
+2115,Common definitions include,2
+2116,"or the $\rm [O\, III]$ flux weighted radius",2
+2117,"As evolved stars ascend the RGB, C and N abundances may be changed by first dredge-up",0
+2118,and extra mixing,0
+2119,The discovery of this correlation has led to an increased interest on the abundances of other elements in planet hosts(e.g.,3
+2120,"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",3
+2121,as well as several others with $\rm {[Fe/H]} \lt -5$,3
+2122,"while BL Lacs are powered by an advection-dominated, low radiative efficiency accretion flow",0
+2123,"Given the rh = 20 au distance of our measurements (and the expected large size of 2014 UN271), we adopted a beaming factor η = 1.175 ± 0.42, based on measurements of 85 Centaurs and TNOs",2
+2124,"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",0
+2125,"At this point, the fragmentation is halted, setting a scale below which no fragments form.",0
+2126,"On scales up to a few Mpc from the nearest galaxy cluster, possibly along filaments, only a few diffuse synchrotron sources have been reported",0
+2127,"The inertial range, which is dominated by magnetohydrodynamic (MHD) turbulence, follows the cascade models with spectral indices αi from around 3/2 to 5/3",0
+2128,"The expanding box uses these comoving coordinates, approximating the spherical coordinates by the Cartesian ones",2
+2129,"To assess the star formation contribution to the Hα 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",2
+2130,"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",0
+2131,"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",0
+2132,"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–Friedrich–Levy 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.",0
+2133,"The beam fluxes used had values of 3 × 109, 1 × 1010, and 3 × 1010 erg cm−2 s−1, while the low-energy cutoff EC covered the parameter space where flare values are usually found (20–120 keV;",2
+2134,"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",1
+2135,"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.",1
+2136,"However, such a dynamical system is linearly unstable to parametric instabilities and large-amplitude Alfvén waves are known to decay into compressible and secondary Alfvénic 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",0
+2137,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,0
+2138,This equation and the condition $F_i-q^\prime _if\ne 0$ furnish the generalized NBH equations,2
+2139,"In the avoidance scheme, smooth-spectrum foregrounds should, in the ideal case, occupy a wedge–shaped region of the two–dimensional power spectrum space (where the wavenumber k can be decomposed into k⊥ and $k_\Vert$ that are the transverse and line-of-sight wave numbers, respectively) whereas the remaining area – the so-called EoR window – is dominated by the 21 cm emission",0
+2140,"Maybe we do not need to intentionally take to heart such the classical dichotomy, because waves and reconnections may interact with each other",3
+2141,"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",0
+2142,"On kpc scales and in the discs of nearby star-forming galaxies, τdep is approximately constant around 1–2 Gyr",0
+2143,Several other works,0
+2144,"applied a Gaussian process, principal component analysis (PCA), and deep learning neural networks to radiative transfer models of SNe.",0
+2145,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,0
+2146,"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)",2
+2147,Our investigation is based on a magnetospheric model that synthesizes the corotating magnetosphere model and the vacuum model,2
+2148,", 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.",2
+2149,"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",0
+2150,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,0
+2151,"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",1
+2152,"Secondly, although a fraction of LBV stars are isolated (e.g.",1
+2153,"For internal consistency, all EWs in this work have been adjusted to the measurement scale of",2
+2154,by using this relation.,2
+2155,The shock is then revived by adding an energy injection following the parameterized method of,2
+2156,"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",5
+2157,A similar feature has also been observed,5
+2158,CB 3 and CB 246,5
+2159,"As the SN explosions start occurring within the cavity formed by the stellar wind bubbles, super-bubbles are created (e.g.",0
+2160,"), which may eventually reach kiloparsec sizes.",0
+2161,"In particular, it was noted that “the Simpson et al. (2017) stars do not define a red giant branch in the theoretical plane, suggesting that their parameters are not correct” (Fig. 1 of",1
+2162,"In the non-rotating case, the GW emission from the post-bounce phase has been studied using self-consistent 3D simulations by many groups",0
+2163,High temperatures in the accretion disc can induce exothermic nucleosynthesis too,0
+2164,All these processes taken together in an advective disc will produce very hot jet base.,0
+2165,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,0
+2166,The original function proposed by,6
+2167,"(Eq. (6) with q = 0.62, see left column) does provide a good approximation of the observed distributions, when assuming the original Θmed − S relation described by Eq. (7), only at flux densities S150 MHz≳10 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≲1 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).",6
+2168,"Similarly, the peak bolometric luminosity of SN 2012au (∼ [6.56 ± 0.70] × 1042 erg s−1) is higher than the mean peak luminosities of SNe Ib and Ic, but still lower than those of SNe Ic-BL",1
+2169,"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.",0
+2170,active or enhanced regions,0
+2171,"CH3C3N itself may form the protonated species, C4H3NH+, through reactions with the HCNH+ and C2H5+ ions producing HCN and C2H4, respectively",1
+2172,Proton plasma properties provide an alternative to determine the solar wind type,0
+2173,A clear advantage of this approach is that the required observables are available from more spacecraft.,0
+2174,"However, if the kink-unstable filament is heated during magnetic reconnection, it is often observed in the AIA 1600 Å channels (e.g.,",2
+2175,"By comparison, the total background at 850 μm inferred from COBE-FIRAS is 3.1–4.4 × 104 mJy deg−2",1
+2176,"Summing these separate surface brightness densities together, we find that the LBGs with L1700 > 1029 erg s−1 Hz−1 in our z ∼ 3, 4, and 5 samples comprise around 6–8 per cent of the submm background at 850 μm (where the range of values simply reflects the uncertainty in the COBE-FIRAS result).",1
+2177,"In this study, we use the Stratospheric",2
+2178,chemistry schemes.,2
+2179,Compared with simulations by,5
+2180,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,5
+2181,"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 ∼250 kpc",1
+2182,"the Galactic bulge, and gas heated by the shocks associated with the bubble",1
+2183,none of which is included in our model (and could evolve as the bubble ages).,1
+2184,"The penultimate point has been widely discussed (e.g.,",0
+2185,involving the role of the flare material and the interacting CMEs on seed particles.,0
+2186,"In such a case, to accelerate particles up to an energy Ec via a diffusive mechanism, the mean-free path λc ∼ rg(γc, B)2/s in the shock downstream region, where B is a small-scale field, has to be smaller than Larmor radius in Bjd",2
+2187,These astrophysical observations are furthermore theoretically explained by deep crustal heating due to pycnonuclear reactions,1
+2188,"In particular, theoretical studies have shown that the MBH–halo occupation fraction can be low in dwarf galaxies",0
+2189,"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",0
+2190,"These nebulae, whose first examples were detected in Hα",0
+2191,more recently have been discovered and observed in X-rays and sometimes in radio,0
+2192,"However, numerical results (e.g.",1
+2193,"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.",1
+2194,"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.",7
+2195,"In addition,",1
+2196,claim that previous estimates of the evolution in the RS GLF,1
+2197,were also due to SB effects.,1
+2198,"Moreover, the disk formation process has been revealed to be much more complicated for binary and multiple cases,",0
+2199,"and in numerical simulations (e.g.,",0
+2200,We test the results in Stanimirović et al. (2014) and,6
+2201,which differ by several factors.,6
+2202,"Meanwhile, a similar power-law index of energy distribution for non-repeating FRBs is also found",5
+2203,"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, 1–10% of the ejecta may fall back into a CB disk according to Kashi & Soker (2011), and Passy et al. (2012) suggest that ∼80% of the ejected material may remain gravitationally bound to the binary (also see",1
+2204,"In recent years, a deficit of star-forming galaxies in the infalling region of clusters has been reported (e.g.",0
+2205,"In the local universe, relationships between strong emission line ratios and metallicity can be calibrated to “direct” electron temperature-determined metallicities from",0
+2206,or photoionization models of star-forming regions,0
+2207,"We utilized a sample of ALMA-identified SMGs in the UKIDSS-UDS field, which has been studied in detail with proper SED fittings",2
+2208,"Similarly to our observations, the sample of",5
+2209,was drawn from a flux-limited sample produced by the SCUBA-2 Cosmology Legacy Survey,5
+2210,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,0
+2211,"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",1
+2212,or an application of some iterative procedure,1
+2213,These latte typically involve several matrix-vector multiplications at each iteration step.,1
+2214,"Moreover, precisely determined DIB profiles",2
+2215,"showing a specific substructure pattern each, should facilitate their carrier's identification.",2
+2216,"For the radio-loud magnetars, given their large variability, we have chosen the brightest radio pulses reported in the literature (data collected from",2
+2217,detected PAHs on subarcsec scales in about half of their sample of 29 nearby Seyfert galaxies.,0
+2218,"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.",1
+2219,"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 – while PAHs were detected in most AGNs, the equivalent width was lower in the centre.",5
+2220,Knots in SS433’s jet can be resolved at radio frequencies using very long baseline interferometry (VLBI) and indicate the presence of highly relativistic electrons,0
+2221,", 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",0
+2222,"Further monitoring, predominantly at frequencies between 0.6 and 15 GHz, has since taken place (e.g.",0
+2223,"Multilevel FIR transition lines have now been widely surveyed in local galaxies, originally by ISO (e.g.",0
+2224,"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 ∼6–7 keV (see e.g.",2
+2225,The Galactic sample of post-AGB stars have been found to be a very diverse group of objects,0
+2226,"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.",2
+2227,"At the wavelength around 4.6 μm 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 μm. Many near-infrared observations have revealed the same feature on the blue wing part of the CO absorption feature",1
+2228,which was suggested as an absorption feature of XCN ice.,1
+2229,"Despite the observational evidence, and to keep alive the inherited model,",1
+2230,"proposed to decrease the theoretical 60Fe abundance in molecular clouds by assuming that stars more massive than 30 M⊙ 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⊙ contribute to less than 50% of the 60Fe production2, this proposition cannot resolve the two orders of magnitude discrepancy between the model and observations.",1
+2231,The orbital phase is calculated using the TEMPO2 package,2
+2232,Although a cavity of 55 astronomical units (au) in radius has been inferred from dust millimeter emission,1
+2233,infrared polarized intensity observations have found no clear evidence for a cavity in scattered light,1
+2234,"For the other lines in the 10 − 36 μm interval,",1
+2235,"did not report a detection, and we used the data presented in Bernard-Salas et al. (2009) for a total of 15 objects.",1
+2236,These compact remnants,0
+2237,"can inject strong energy inputs in the primeval universe (e.g.,",0
+2238,Five clusters from the sample of,2
+2239,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.,2
+2240,These processes have been studied both by investigating normal modes of the inhomogeneous structure,0
+2241,"One striking problem is the ${\rm ^{14}N}/{\rm ^{15}N}$ isotopic ratio of nitrogen in comets. Its average value, 144 ± 3",3
+2242,", is three times lower than the bulk ratio of 441 ± 6 in the protosun as inferred from solar wind measurements",3
+2243,"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.",3
+2244,"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",1
+2245,: there is more kinetic energy in the solar wind than the bulk velocity vector would let us think.,1
+2246,"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",1
+2247,The quasar-level AGN activity,3
+2248,at the center is blocked by the thick dusty torus acting as the “coronograph”,3
+2249,"this makes HzRGs true obscured type-2 quasars, allowing us to probe their host galaxies and CGM without strong AGN contamination (e.g.",3
+2250,"for radio-quite type-2 sources, see",3
+2251,This is in contrast with previous studies,6
+2252,"where the backward modeling approach is employed to constrain the probability of mass for a given richness,",6
+2253,"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",0
+2254,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.,0
+2255,"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",0
+2256,The Hβ BEL is considered to be rotating gas in a flat “pancake-like” region in which the normal to the BEL disk is parallel to the jet axis,2
+2257,"Thus, the FWHM that appears in Equation (4) depends on the LOS.",2
+2258,"This method has since identified a large number across the extragalactic sky, i.e., more than 100 lensed candidates at z > 1",0
+2259,Observations from local galaxies,0
+2260,have shown H2O emission to be ubiquitous with intensities as bright as CO lines.,0
+2261,Such high-precision RV surveys include those being undertaken currently with,0
+2262,and CHIRON,0
+2263,We estimated the precession period using the theory from Terquem et al. (1999) and the binary parameters taken from,2
+2264,"– Mh = 0.8M⊙ (the mass of the hot WD companion), Mp∕Mh = 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).",2
+2265,"Driven by dynamical friction and global torques from this disc, the pair of MBHs decays very efficiently down to separations of the order of ∼1–0.1 pc, where it forms a gravitationally bound binary",0
+2266,and the kilonova AT 2017gfo in the ultraviolet–optical–infrared band,0
+2267,as well as the combination of the H2O-K2 index with pEWs to derive [Fe/H],0
+2268,These have revealed a surprising diversity in the orbital alignments (for example,0
+2269,"which is in contrast to the Laplacian ideals of planets forming inside a flat disk, coplanar with the stellar equator and staying there",1
+2270,Following our previous work,2
+2271,we have adopted here a G+L profile fit.,2
+2272,The tilt angle compared to a completely edge-on orientation was suggested to be 3° in the model of Hogerheijde et al. (1995) and,2
+2273,A tilt angle of 3° is equivalent to an enhancement factor of 20 for the measured column densities.,2
+2274,"The Largest Linear Sizes (LLS) and radio powers of relics are correlated, as well as the integrated spectral index and the radio power",0
+2275,An alternative and attractive pathway for seed BH formation is via the so-called direct collapse,1
+2276,"where a supermassive star (SMS) with ${\sim } 10^{5}\, \mathrm{M}_{\odot }$ collapses into a BH with a similar mass by general relativistic instability",1
+2277,"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.,",1
+2278,"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",0
+2279,decay of chromospheric activity,0
+2280,"Adopting an expansion velocity equal to half the velocity interval where the structure is observed, Vexp = 7.0 ± 1.3 km s− 1 , the molecular mass given in Table 1 and the atomic and ionized masses estimated by",2
+2281,"1450 and 3000 M⊙, respectively, we obtain Ekin = (2.5 ± 1.0) × 1049 erg, assuming a 40 per cent error for the masses.",2
+2282,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.,0
+2283,"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",7
+2284,"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",1
+2285,"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;",0
+2286,"By default, these techniques are applicable only to single-frequency sky images: even for multiwavelength observatories such as the Herschel Space Observatory",0
+2287,or Planck,0
+2288,"the standard detection pipelines have produced individual source catalogs for each frequency band (see e.g.,",0
+2289,"The next logical step is to boost the signal of faint sources by combining the different bands into a single detection, that is, “multifrequency detection”.",3
+2290,"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⊙, measured by The H i Nearby Galaxy Survey (THINGS",1
+2291,"Open clusters are a valuable alternative, being on average younger",0
+2292,and therefore a better tracer of the gradients in the disc out of which the most recent stars formed.,0
+2293,While tides on the progenitor of the second-born black hole can spin up the progenitor star,1
+2294,"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",1
+2295,It is particularly important to understand if cluster mergers,3
+2296,"or, alternatively, if they have no direct effect (e.g.",3
+2297,"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 20Â times brighter than the solar zodiacal cloud assuming a smooth brightness distribution (e.g.,",0
+2298,This model was successfully applied to,0
+2299,as well as atoll sources,0
+2300,so it could be a universal model for NS-LMXBs.,0
+2301,The overall incidence rate of magnetic upper main sequence stars in close binaries is less than 2 per cent,1
+2302,although this fraction is significantly higher if one includes wide long-period systems,1
+2303,The patchy beam scenario is one of the common beam models that has been used to explain the emission properties of pulsars (see,0
+2304,Previous studies showed that WL masses obtained from the tangential shear fitting were biased low up to 10 per cent with a scatter of ∼25 per cent,0
+2305,"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.",0
+2306,"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",1
+2307,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,3
+2308,"Being associated with old stellar populations, they represent the basis of an alternative Population II distance scale",0
+2309,"more suitable to calibrate secondary distance indicators that are not specifically associated with spiral galaxies (e.g. the globular cluster luminosity function, see",0
+2310,and references therein).,0
+2311,The difference between the Saro et al. (2013) and,1
+2312,galaxy scaling relations depends on the details of the semi-analytic and hydrodynamical implementations used in Saro et al. (2013) and,1
+2313,respectively.,1
+2314,"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 ‘groups’ of galaxies (e.g.",0
+2315,Possibly the material is accelerated by radiation pressure,0
+2316,or cosmic rays (CRs; e.g.,0
+2317,but alternatively the high-speed cool gas may be due rapid radiative cooling in some situations.,0
+2318,"In addition, it also shows evidence of relativistic jets",0
+2319,"Although a supermassive BH can be modeled by adding a Keplerian potential, it is much simpler to model the BH as this small Gaussian",2
+2320,"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.,",1
+2321,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,0
+2322,of molecular oxygen,0
+2323,all indicate that comet 67P formed at low temperature and did not experience any substantial global-scale heating after its formation.,0
+2324,"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",1
+2325,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,1
+2326,which are a good probe of star formation activity,1
+2327,"However, the proposed astrophysical pathways to mergers remain highly debated. Possible compact-object merger pathways include isolated binary evolution",0
+2328,individual periodic signals or continuous waves (CWs,0
+2329,Combining different samples from various instruments at different redshifts therefore inevitably introduces ENLR size–luminosity relations with different slopes α depending on the details of target selection and analysis approaches. Slopes ranging from,1
+2330,α = 0.25 ± 0.02,1
+2331,are reported in the literature.,1
+2332,Growing indirect observational evidence suggests that magnetars could act as the central engines of both LGRBs and short-duration GRBs,7
+2333,Different approaches of subgrid models were explored,0
+2334,to mechanical feedback where the momentum boost during the unresolved adiabatic phase is calibrated through small-scale ISM simulations and injected into the ISM,0
+2335,"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.",3
+2336,"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.,",1
+2337,"However, recent observations of the pickup helium focusing cone using the Plasma and Suprathermal Ion Composition (PLASTIC",2
+2338,on board the Solar and Terrestrial Relations Observatory Ahead (STEREO A) spacecraft measured the peak density and determined the inflow longitude to be,2
+2339,After first being reported in the Earth’s magnetosheath,0
+2340,"Therefore, GRB afterglows are good probes of burst environment and the interstellar dust and gas in distant, star-forming galaxies",3
+2341,"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",2
+2342,"are of the inverse-polarity type, and those that disobey Martin's Rule are of the normal-polarity type.",2
+2343,"Complementing these observations, the spectroscopic confirmation",0
+2344,"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.",0
+2345,"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.",2
+2346,found a positive correlation between flux and spectral slope for a sample of bright RXTE AGN in the 2–10 keV 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.,2
+2347,"In response, shock acceleration transport models were developed in recent years based on the numerical solutions of the focused transport equation",0
+2348,to take advantage of the fact that focused transport is not restricted to small pitch-angle anisotropies.,0
+2349,The fit also provided a low value of electron temperature (kT) consistent with the high value of β obtained,5
+2350,"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.,",7
+2351,which could improve the constraining power beyond the averaging method introduced here.,7
+2352,"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",0
+2353,"Investigations show the layered accretion in the inner disk, where the midplane region is “dead” due to low ionization while the surface layer is “active” due to sufficient ionization",0
+2354,The traditional habitable zone concept assumes a planet with a functioning silicate-weathering feedback and a positive CO2 greenhouse effect,0
+2355,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.,0
+2356,"For σ0 ≳ 2.45, the spread of η for the observed galaxies (e.g.",1
+2357,"broadens and spans both positive and negative η values. In fact, majority of the galaxies tend to have positive ηs. This change in behaviour is well known.",1
+2358,"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",5
+2359,"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.,",0
+2360,"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",0
+2361,"Radial migration of stars via cold torquing, also known as “churning,” by a bar and spiral waves",2
+2362,then allows for the populations to spatially overlap in the solar neighborhood.,2
+2363,In Fig. 11 (upper panels) we show the evolution of the spectral break measured through the DB definition,2
+2364,as well as the relative strength (the ratio) between the two (lower left panel).,2
+2365,We use the Mishima et al. (1983) formulation (see Appendix of,2
+2366,Examples of relics in this category are those in,0
+2367,and Abell 85,0
+2368,A few CTTSs binaries are thought to potentially be accreting through accretion streams. These include DQ Tau,0
+2369,None of these stars shows the type of Hα 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.,6
+2370,"The colored rectangles represent the errors of the DEM curve, which are calculated from 100 Monte Carlo (MC) realizations of the observational data",2
+2371,"Finally, a number density ratio (rd = n0/ne) of ∼0.02 between outside and inside of the flaring loop is determined, which is very close to the density contrast from recent observations",5
+2372,"Quasars’ lifetimes are not long ( 0.1 Gyr,",0
+2373,"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.,",0
+2374,There is another possibility of the FB formation due to the tidal disruption of stars,0
+2375,and the acceleration of individual particles by the arising shock waves.,0
+2376,"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, ∼1000 kg s−1 (e.g.,",0
+2377,"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.,",0
+2378,"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",5
+2379,"Since Eggen et al. (1962) showed a model of the MW’s 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,",0
+2380,LAMOST,0
+2381,and more.,0
+2382,"Above the turnover, the GMC mass function has a power-law form with β ∼ 1.9, close to the observed range of β ∈ [1.6, 1.8] for clouds in the Milky Way",1
+2383,"The rotational period of RX J1856 is P = 7 s and the X-ray pulsed fraction is the lowest among the XDINSs, ∼1.3 per cent",0
+2384,This anticorrelation between stellar mass and λeff is qualitatively consistent,5
+2385,as well as other observational evidence (e.g.,5
+2386,"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",5
+2387,We test in Section 2 two available one-dimensional (1D) codes:,2
+2388,"and a modified version of the Eulerian, 1D hydrodynamic flash4.0 code with thermonuclear burning",2
+2389,"against the ρ0,7 = 1 case.",2
+2390,"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).",1
+2391,This progress has led to a general consensus about the main physical ingredients required to describe the evolution of the galaxy population (e.g.,0
+2392,"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.,",0
+2393,"Indeed, variability between the yields of different mergers is required to explain observed abundances in metal-poor stars",2
+2394,"Measurements from Muller et al. (1980), Danjo et al. (1984), Mueller et al. (1985), and",1
+2395,demonstrated onsets below the ionization threshold.,1
+2396,"The rate at which water vapour will be released is da/dt ∼ 1.5 × 10−3 μm yr−1 (scaled to the distance of the ring, from the result of",2
+2397,"), where a is the vertical thickness of the layer.",2
+2398,Due to the complicated physical processes involved in spectral line formation in a 3D atmosphere (e.g.,2
+2399,"it is difficult to quantify higher order effects beyond the linear relation between $\mathfrak {v}$ and Wλ; that is, the systematic uncertainty of the linear fitting.",1
+2400,"Dense cores, where stars form, are located along or at the intersections of some of these fine substructures (e.g.",0
+2401,"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",0
+2402,"Currently, a limited number of observations",0
+2403,are available to explore the environment dependence of the metallicity,0
+2404,"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.,",0
+2405,The predictions are based on experimental data from,2
+2406,for ethylene glycol,2
+2407,It has also been generally believed accordingly that most activity (namely active galactic nuclei—AGNs) of supermassive black holes (BHs) at the centers of galaxies at low redshifts,0
+2408,"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,",0
+2409,"Additionally, glycolaldehyde (C2 H4O2), the simplest form of sugar and one of the first intermediates in the formose reaction",0
+2410,", has also been detected in this object for the first time in space in 2012",0
+2411,"On the other hand, the super-Chandrasekhar WDs were often explained by incorporating different physics, such as a",0
+2412,presence of charge in the WDs,0
+2413,and the 3D numerical simulations,0
+2414,"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.",0
+2415,"They were discovered as dark silhouettes against the galactic background at 8 and 15 μm with the Midcourse Space Experiment (MSX,",2
+2416,The comparison sample is compiled from the literature up to z ∼ 3,2
+2417,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.,0
+2418,while similar works were performed on INTEGRAL data (e.g.,0
+2419,"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 Φ would not be chosen arbitrarily and would be self-consistently determined by the MHD equations, given the Ψ and Ω specified (e.g.,",0
+2420,"Based on its SED, MWC 758 has been classified as a pre-transition disk",0
+2421,"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",1
+2422,"In this sample, we observe the opposite trend.",6
+2423,and have coupled the code to SN ejecta models,2
+2424,"The large mass and solid angle covered by highly concentrated galaxy clusters make them ideal gravitational lenses, which can be used as ‘cosmic telescopes’ to observe very distant galaxies (e.g.",2
+2425,"For example, the well-known density–morphology relation reveals that the ellipticals are preferably found inside the dense groups and clusters, whereas the spirals are intermittently distributed in the fields",0
+2426,"More recently, indications of radial anisotropy in the outer regions of DM haloes have been obtained from numerical simulations (e.g.",0
+2427,"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.",4
+2428,"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 “J1407 b”) with a mass of 60–100 MJup",0
+2429,"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.,",5
+2430,Nuclear optical line emission has been reported from spectroscopy,0
+2431,There is some tentative evidences for alignment with respect to the magnetic field,3
+2432,"in, e.g., the IRAS 4A system at cm wavelengths",3
+2433,"For the case of ρIA = 1.3 (magenta), a decrease of the amplitude of the primary can hardly be observed, as expected for low-amplitude wave",5
+2434,"Similar rapid changes in the optical-UV flux are typically seen in other BLS1s, especially those at low Lbol/LEdd (e.g.",5
+2435,The mechanism by which a nascent millisecond magnetar might power a GRB jet has been studied in detail over the past decade,0
+2436,Other authors observed different systems and likewise saw chro-mospheric excess emissions,0
+2437,"In fact, the X-ray continuum in AGNs is well modelled by a power law with a high energy roll-over (e.g.",0
+2438,The fraction of clumpy galaxies was studied from z = 0 up to the most distant galaxies identified today at z ~ 10,0
+2439,Another major coolant of the ISM is [O i]63 μm,0
+2440,"For V593 Cen, we updated the orbital parameters using more complete light curves. The orbital inclination of 83°.18 is similar to the result (82°.6) obtained by",5
+2441,Using the critical intensity advocated by recent studies,1
+2442,this ranges from a few Gpc−3 (e.g.,1
+2443,to 10−6 to 10−4 Mpc−3,1
+2444,"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",0
+2445,"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.",0
+2446,Unprecedented flux and spectral variability during these episodes have been observed,0
+2447,These IGM transmissions are estimated from Monte Carlo simulations (,2
+2448,) which generate 10 000 sightlines for redshifts consistent with the H i cloud distribution defined analytically by Inoue et al. (2014).,2
+2449,The problem of accretion on to an SMBH has been studied via hydrodynamical simulations (e.g.,0
+2450,"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 β photons are at the limits of either completely optically thick or optically thin at SNR shocks, i.e. they are completely converted to H α photons or not at all (e.g.",1
+2451,Similar energy dependent pulse arrival time behavior can also be found in,0
+2452,and XTE J1807–294,0
+2453,with different break point energies.,0
+2454,Prominences are generally believed to be supported by the magnetic tension force of the dips in sheared arcades,0
+2455,"For grains consisting of two or three materials, we first derive effective optical constants following the Maxwell Garnett mixing rule",2
+2456,"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",0
+2457,"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.,",0
+2458,The HCN(1–0)/HCO+ ratios for M31 GMCs,2
+2459,are indicated by the turquoise shaded region in panels c and d.,2
+2460,Using Bayesian analysis to fit,0
+2461,and a similar distribution function analysis using 5D phase-space data from Gaia,0
+2462,This was done using the complex dielectric function for the sample obtained by heating boehmite at 1173 K from,2
+2463,"assuming a spheroid with depolarization parameters of (0.35, 0.035).",2
+2464,"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",1
+2465,many modern simulations have used a purely Newtonian approximation for gravity,1
+2466,This has been shown using,0
+2467,as well as cosmological simulations,0
+2468,Large numbers of works have extensively studied the binary-disk system in the Newtonian regime with,0
+2469,and hydrodynamical simulations,0
+2470,"If we considered the AIA 304 Å observations alone, the on-disk condensation, and hence coronal rain events we report here would resemble those occurring in magnetically closed field lines",1
+2471,which are generally interpreted as a manifestation of the heating-condensation cycles due to thermal nonequilibrium,1
+2472,"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.",1
+2473,"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.",2
+2474,"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.,",2
+2475,"Moreover, the disk formation process has been revealed to be much more complicated for binary and multiple cases, both in observations",0
+2476,"In spite of its huge infrared luminosity, the host galaxy is classified from the optical morphology as an ordinary Sa-type galaxy ([R’]SAB[s]a;",1
+2477,Typical values are close to D2 = 1.4–1.5,5
+2478,which are consistent with the fractal dimension as derived for the young stellar structures.,5
+2479,"In particular,",5
+2480,and Li etal. (2016) both found that the rotation measure predicted from the ADAF is roughly consistent with the observational values.,5
+2481,"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",0
+2482,"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",1
+2483,In previous work,1
+2484,"we used a custom filter centred on the deep 1.45 µm feature present in YPMOs to distinguish between them and background sources. In the 2–5 µm 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 ‘water’ 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.",1
+2485,"Clarke et al. (2019) and Buck (2020) suggest that bimodality should be common in disc galaxies, whereas",1
+2486,suggest that it is rare.,1
+2487,RCW 86:,2
+2488,GeV,2
+2489,"For our disk model, we are using the power-law profile for the scattering surface height H and the separation r found by",2
+2490,for the disk around HD 97048. This profile describes the flaring discovered in this source reasonably well up to a separation of ~270 au.,2
+2491,These PESs have also been able to account for even subtle effects such as the GP,0
+2492,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.,7
+2493,These considerations are beyond the scope of this paper.,7
+2494,"However, there is no theoretical argument (or pathology) against GWs propagating faster than light (see",2
+2495,and references therein),2
+2496,"In past years, several alternatives have been proposed to constrain the redshift of BL Lac objects, including",0
+2497,or from the neutral hydrogen in the intergalactic medium (e.g.,0
+2498,While this approach initially appeared to work remarkably well in the case of starburst galaxies,1
+2499,there is now ample evidence that there is no tight universal relation between the UV slope and the,1
+2500,"Such an approach, also known as floating chunk offset method (FCO;",2
+2501,"has proven extremely reliable even in the presence of complex activity signals, as shown by Malavolta et al. (2018).",1
+2502,"The initial condition is the Orszag–Tang vortex (OTV) (e.g.,",2
+2503,"In the case of GRBs, approximately 1/6 of examples are consistent with a galaxy nucleus",1
+2504,"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.",0
+2505,"High-resolution CO observations are critical for evaluating where high-redshift galaxies fall on the true surface density version of the Schmidt–Kennicutt relation, where ΣSFR and Σgas can be compared on a pixel-by-pixel basis within individual galaxies (as done for local galaxies; e.g.,",3
+2506,Studies have shown that heating mainly escapes through the outflow cavity in deeply embedded sources,0
+2507,"Secondly, in practice, determining the location of the cutoff is vulnerable to systematic effects, such as contamination from the narrow metal lines",0
+2508,The process of morphological quenching,1
+2509,"where the formation of a stellar bulge stabilizes the disk against further star-formation, is also improbable.",1
+2510,"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",2
+2511,We observe a very similar behavior and dependency of abundances on the Ye distribution for all exploding models of the 15 M⊙ progenitor.,5
+2512,"Atiras or Interior Earth Objects (IEOs) have aphelion distances 0.983 au and can only be observed at low solar elongations (often 70○); Vatiras have aphelia 0.718 au, are observed at very low solar elongations (typically 40○–45○), and just one such object is currently known",0
+2513,"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 γ Cas",2
+2514,"NLs have high accretion rates (∼10−8 M⊙ yr−1), so are in a persistent high state, and they gather above the period gap in the period distribution of CVs",0
+2515,"In particular, the SPS approach has been applied to observations of various Galactic and extragalactic environments (e.g.,",0
+2516,"showing power spectral slopes β roughly ranging from −2.7 to −3.7 depending on the tracers used (e.g., H i, carbon monoxide (CO), and dust).",1
+2517,"Since the halo concentration cannot be reliably measured for haloes with fewer than about ∼400 particles, we use the method presented by Ramakrishnan, Paranjape & Sheth (2021) to assign concentrations cvir (assuming",2
+2518,NFW profiles) conditioned on the mass and local tidal environment of individual haloes.,2
+2519,"Finally, the MFD internal shock (IS) model for GRBs also suffers some criticisms, such as",6
+2520,and inconsistency with some empirical (Amati/Yonetoku) relations,6
+2521,"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° (namely, the disk is seen approximately edge-on;",0
+2522,data release as well as calibration vectors for the MaNGA survey,2
+2523,DR14 data release,2
+2524,in Fig. 6.,2
+2525,"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 Å. 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 β, γ, and δ lines",1
+2526,"One can also observe the change in the median residual spectra of DR9 and DR12 in Fig. 1. However, the Hα feature remains uncorrected from DR9 to DR14.",1
+2527,Given our very limited knowledge of the ternary C/O/Ne phase diagram,6
+2528,this effect cannot be quantitatively implemented in our evolution models.,6
+2529,"However, we note that our current understanding of 22Ne phase separation is remarkably consistent with the missing cooling delay.",5
+2530,"Interestingly, we found that, four HSPs did not show any IDV",1
+2531,The newest model developed by,0
+2532,"is based on similar ideas, but makes use of the optical Hα surface brightness and a wide set of various calibrators.",0
+2533,"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.",0
+2534,"Indeed, the first molecular searches of PNe turned up negative (e.g.,",0
+2535,Treatment of errors for combining distance moduli across methods or across measurements is suggested by,2
+2536,"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.",2
+2537,"Further, the higher contrast of the acoustic features in EE power spectrum compared to astrophysical foregrounds",7
+2538,"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.",7
+2539,The role of twisted magnetic field in the MHD waves has been studied in many theoretical works (e.g.,0
+2540,"However, a hot region with radius 3–4 times smaller than R can still produce a pulsed fraction below current limits of 20–40 per cent in the spin period range 0.1–0.4 s of known CCOs (see Section 1; for pulsed fraction dependence on spot size, see, e.g.",2
+2541,"Indeed, the ultraviolet and X-ray variability detected for many of these LINERs",5
+2542,"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 III] morphologies found for LINERs are spheroids, if we assume that the [O III] traces the NLR.",5
+2543,showed that the main differences between the migration recipes from Jiménez & Masset (2017) and Paardekooper et al. (2011) lie in the computation on the corotation torque.,1
+2544,"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",0
+2545,"with fuelling from major mergers strongly disfavoured by recent observations (e.g.,",0
+2546,he protoplanetary embryos masses scale as M ≈ r3(2 − x)/2Δ3/2,2
+2547,where Δ is the mutual Hill radii separations between embryos orbits.,2
+2548,The flux ratio ϕ(α)/ϕ(0) can be derived by using the dust phase function,2
+2549,Several SNe surveys have set strong constraints on cosmological models from the distance–redshift relation (e.g.,0
+2550,"However the measured apparent magnitudes, have a residual scatter arising from its intrinsic scatter and effects due to line-of-sight (LOS) structures.",0
+2551,"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",1
+2552,"An LBV star provides an adequate explanation for the transient time-scale, the isolation (e.g.",1
+2553,"the lack of a host H ii region (Fig. 2 and 3; see below, however), and the transient/main source offset (d ≈ 0.3 kpc, for D ≃ 8 Mpc; Table 1; see below, however).",1
+2554,As a result of the analysis of 3 min oscillations detected in observations from the Atmospheric Imaging Assembly instrument,0
+2555,on-board the Solar Dynamic Observatory (SDO;,0
+2556,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,0
+2557,Only a few hot corinos have been identified so far either with single dish or interferometric observations:,0
+2558,HH212,0
+2559,Sparse and/or irregular sampling is a very common issue in SF analysis,3
+2560,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,0
+2561,Observations of such ‘low-luminosity’ ULXs,0
+2562,"have revealed changes in the disc emission that may imply the creation of a radiation pressure supported, larger scaleheight flow in the inner regions",0
+2563,or magnetic pressure support,0
+2564,Whether the core collapses or the deflagration disrupts the core depends sensitively on the ignition density,2
+2565,This is consistent with other results (e.g.,5
+2566,"which have shown that galaxies having higher current SFR relative to their past averaged SFR are likely to deviate above the IRX–β relation, i.e. have larger AFUV(IRX) for a given AFUV(β).",5
+2567,"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.",6
+2568,We excluded stars with saturated photometry,2
+2569,"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.",2
+2570,"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.,",2
+2571,"For example, using Gaia Data Release 2 (DR2)",0
+2572,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,0
+2573,discussing three bursts of star formation in the Orion Nebula cluster).,0
+2574,"Many systems have not been taken into account due to several issues. For instance, the system PG1115+080",1
+2575,from the CASTLES survey has been discarded because the lens mass model is steeper than isothermal.,1
+2576,Theoretical predictions are now available,0
+2577,"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.,",0
+2578,"More generally, a body of work in various domains,",0
+2579,to geophysical fluid dynamics (e.g.,0
+2580,"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.",0
+2581,"Here, we report on Large Binocular Telescope (LBT) observations of an isolated pulsar, PSR J2043+2740",0
+2582,detected by,0
+2583,and Fermi,0
+2584,The grain-surface network has been further updated to include all studied routes to water formation under interstellar and circumstellar conditions,2
+2585,"We estimated the projected spatial wavelength λproj of the “wiggling” wave according to λ = λproj∕sin i, where i is the angle between the jet symmetry axis and the line of sight, and T = λ∕υ, where υ is the jet velocity, from",2
+2586,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,0
+2587,", at least for massive haloes, M ∼ 1013 M⊙.",0
+2588,"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",1
+2589,which instead seems likely to be due to the very different sample selection of the S4G and SDSS galaxy samples.,1
+2590,"We recalculated the lifetimes of molecules assuming AV = 3 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",2
+2591,for more details on the assumed dust properties).,2
+2592,"The 10.0–70.0 keV flux of the source is found to be (2.26 ± 0.01) × 10−9 erg cm-2s-1, much lower than the value (5.6 ± 0.3) × 10−9 erg cm-2s-1, previously reported from SUZAKU data",6
+2593,"To speed them up, we used the Modified Random Walk method implemented in RADMC-3D",2
+2594,"For example, there is good evidence",0
+2595,"that the local overdensity correlates with the group-centric distance (e.g.,",0
+2596,One should note that during studies of the isolated Abell groups,1
+2597,only a rudimentary alignment was found and related only to the brightest cluster members.,1
+2598,"We also manually perform the absolute wavelength calibration using a relatively strong neutral line, O I 1355.60 Å (see",2
+2599,The extended star formation history and the broad range of metallicity (−1.5 ≲ [Fe/H] ≲ 0.2) discovered in the stream fields can be explained by a disk galaxy progenitor,2
+2600,"In the case of NGC 7213, the photometric data included in the analysis are:",2
+2601,and the FIR photometry by,2
+2602,"However, such a degeneracy can be broken when the inner edge of the disk is very close to the compact object",1
+2603,"Asteroid 469219 librates around $\omega _{\rm r}=-90{^\circ }$ for Venus, the Earth, and Jupiter. This behaviour corresponds to domain III in",2
+2604,"horseshoe-retrograde satellite orbit transitions and librations (around $\omega _{\rm r}=-90{^\circ }$ or 90°). For a given cycle, the lower part corresponds to the horseshoe phase and the upper part to the quasi-satellite or retrograde satellite phase.",2
+2605,"Indeed, constraints from explosion parameters have shown the majority of CCSNe to be consistent with lower mass progenitors, as opposed to more massive Wolf–Rayet stars",0
+2606,GRBs likely represent a population with rather larger initial masses,0
+2607,"It is thought that the early pre-solar nebula was hot (>1500 K), such that both volatiles and refractories (Tsub ≳ 1400 K) are in the gas phase out to larger distances",0
+2608,Such lens model has found widespread astrophysical applications in the literature,0
+2609,"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​​ ∼ ​​0.1 pc and a dispersion of less than a factor of ∼2",0
+2610,"The different cosmologies used in the Millenium simulation (in particular, σ8 = 0.9; Springel et al. 2005) by Saro et al. (2013) and the simulations by",1
+2611,σ8 = 0.8) may also play a role.,1
+2612,"To perform the fitting to the data, we adopted the Python package emcee",2
+2613,", a pure-Python implementation of Goodman & Weare’s Affine Invariant Markov chain Monte Carlo (MCMC) Ensemble sampler.",2
+2614,"SN 2006jd was observed at 1638 days, an epoch very similar to that of SN 2014C, with Spitzer/IRAC and WISE",2
+2615,"In all three cases, the photometry and spectra from 1 to 10 μm are well fitted by purely carbonaceous dust models, which we overplot in Figure 6 using dust parameters from the literature.",5
+2616,"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.,",0
+2617,The presence of the substructure has been confirmed by,0
+2618,as well as by more recent SZE measurements,0
+2619,"By using these techniques, some studies show a correlation between both 12 + log (O/H) and log (N/O)",0
+2620,Studies of clusters and groups at $z$ ∼ 0 have evidently shown that outskirts of groups and clusters,3
+2621,and filaments of galaxies,3
+2622,are favourable sites for galaxy transformations.,3
+2623,"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",1
+2624,become inefficient at describing the AO PSF.,1
+2625,One of the methods based on the synergy between UV and WL observations is the Doppler dimming technique,2
+2626,"This result is in broad agreement with models of jet launching from ADAFs (e.g.,",5
+2627,which predict the formation of a thin and mildly-relativistic outer layer.,5
+2628,Both clusters host two kinematically distinct populations,0
+2629,More details can be found in our previous papers,0
+2630,A bright X-ray background source such as,0
+2631,or a GRB (e.g.,0
+2632,can be used to detect the WHIM by producing absorption features in its energy spectra,0
+2633,References for the observational data are as follows: RX J0852.0−4622:,2
+2634,GeV,2
+2635,"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",2
+2636,"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),",0
+2637,and Loiacono et al. (2019) find low gas fractions in powerful AGN at cosmic noon hosting high-velocity molecular and ionized outflows,0
+2638,"During the transition from the subcritical to the supercritical regime, sources show two different branches in their hardness–intensity diagram (HID) which are known as horizontal branch (HB) and diagonal branch (DB)",0
+2639,"This correlation, hereafter referred to as the R–σv relation, is usually interpreted as the result of turbulent motions in the interstellar medium on all scales",0
+2640,Observation of magnetic fluctuations in the SW indicates that omnidirectional power spectra approach a k−1 wavenumber dependence and that low-frequency turbulence exhibits some sunspot cycle variability,0
+2641,"For a circular polarized wave, the dispersion relation in the laboratory frame is given by (e.g.,",2
+2642,"We measured 164 ± 13 background-subtracted counts between 0.2 and 2.0 keV, as determined using calc_data_sum in Sherpa",2
+2643,"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",0
+2644,Equation (7) of,2
+2645,"then yields Lbol ~ 1.7–2.8 L⊙, depending on whether the NIR flux is neglected (which may be the case) or extrapolated from γ = −2.",2
+2646,"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",1
+2647,"In addition, recent observational and theoretical studies on RSGs and SNe II indicate that RSG wind mass-loss rates may be independent from metallicity",0
+2648,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,0
+2649,"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.,",0
+2650,"he SFR reported in Table C.1 refers to a stellar mass range from Mlow = 0.1M⊙ to Mup = 100M⊙, is averaged over the past Δt = 100 Myr, and was calculated using the standard SFR(LIR) relationship from",2
+2651,"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×LIR[L⊙] M⊙yr-1.",2
+2652,Recent advances in understanding the properties of magnetohydrodynamic (MHD) turbulence,3
+2653,stimulate a renewed investigation on density statistics,3
+2654,which provide important insight into key physical processes such as star formation in the turbulent and magnetized ISM,3
+2655,"The surface temperatures of such hydrostatic, strongly inflated models computed with plane parallel grey atmospheres are then compared with the fictitious effective temperatures at τ = 20 of the atmosphere calculations performed by",2
+2656,"Moreover, Draine’s formulation is accounted to determine the lunar surface’s photoelectric efficiency (",2
+2657,) – its spectral dependence can be represented as ${\chi _{\nu r}} = {\chi _o}[1 - ({\phi _r}/{E_\nu })]$.,2
+2658,Since the source emission has been stable for more than 15 years,2
+2659,"we performed the joint fit with the longest, burst-free NuSTAR observations (ObsID = 30001025012) and XMM-Newton observations that were performed ∼11 years earlier.",2
+2660,"However, LC II/LFIR is not constant, but declines with increasing LFIR, known as the ‘[C ii] deficit’",0
+2661,Despite the considerable scatter in both colors and color gradients,1
+2662,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.,1
+2663,"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",0
+2664,"As happens within Earth’s 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",2
+2665,"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",2
+2666,for how the listed temperature we extract from the Gaia catalogue is inferred from the Gaia data).,2
+2667,"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.,",2
+2668,"These often-called starburst galaxies, with an IR luminosity LIR ∼ (0.1–5) × 1012 L⊙ (e.g.,",0
+2669,become increasingly more common at high z.,0
+2670,"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",1
+2671,"However, from spectro-polarimetric observations of a γ-ray emitting NLSy1 galaxy, PKS 2004 − 447",1
+2672,and accretion disc modelling of a sample of 23 radio-detected NLSy1 galaxies,1
+2673,indicate that they have masses similar to the blazar class of AGNs.,1
+2674,"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 − 9",3
+2675,"Indriolo & McCall (2012) find a mean ζH of 1.8 × 10−16 s−1 in their sample of diffuse molecular sight lines, and values as large as ∼1 × 10−15 s−1 have been reported in the literature",1
+2676,It should be noted that only a handful of studies so far have looked at the correlation between α and global galaxy properties:,0
+2677,while,0
+2678,identified H II regions via Paα,0
+2679,"However, the stellar number densities required for tidal truncation are high, and in practice few observed regions satisfy this condition",1
+2680,"Since long cosmologists have felt motivated to look for alternative explanations for the DE beyond a rigid cosmological constant Λ. The scalar field paradigm was then profusely used also to make the cosmic vacuum dynamical: Λ = Λ(ϕ). In the old days, the main aim was to adjust the large value of Λ typically predicted in QFT to be zero. There were many early proposals (see e.g.",0
+2681,"Second, while the predicted shadow feature is nearly independent of the spin or orientation of the black hole to within 10%",0
+2682,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.,0
+2683,"We adopt a different perspective in proceeding from the basic guiding center kinetic equation (e.g.,",2
+2684,instead of the transformed Vlasov equation (Skilling 1975) used by Zank et al. (2014).,1
+2685,It has already been tested with real data collected by the LIGO and Virgo detectors,0
+2686,"though the constraints obtained so far with this ‘statistical’ 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.",6
+2687,"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",0
+2688,"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",0
+2689,We note that a similar result was found in observations of the Seyfert 1.2 ICÂ 4329a and the narrow-line Seyfert 1 SWIFT J2127.4+5654 with NuSTAR,5
+2690,In the recent paper by,5
+2691,the Helios proton data radial gradients of the GCR flux were found to be 6.6 ± 4% above 50 MeV and 2 ± 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).,5
+2692,The collision velocity dependence of the coefficient of restitution between particles was observed in experiments,0
+2693,Assuming a set of stellar population models,2
+2694,"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.,",2
+2695,"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",0
+2696,as illustrated in Fig 3.,0
+2697,"Most recently, Rodriguez-Almeida reported the first unambiguous detection of ethanethiol in the ISM, toward the G+0.603-0.027 molecular cloud",0
+2698,On galactic scales massive molecular winds are common in local Seyfert galaxies (e.g.,0
+2699,"Unfortunately, measurements of UV radiation are strongly hampered by the interstellar medium absorption (up to 70%–90%), which is significant even for relatively close stars, so that estimates of stellar UV radiation strongly rely on modeling (see",0
+2700,", for a recent review).",0
+2701,"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 α effect, where α is a measure of the net kinetic helicity in the flow (see, e.g.,",0
+2702,"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.,",5
+2703,In the literature there are several theoretical works on the evolution of [Ba/Fe] and [Y/Fe] in the Galactic thin disc (e.g.,0
+2704,The main and novel aspect of our work is the analysis of the diffuse radio emission resulting from radio haloes in galaxy clusters,4
+2705,"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 ≈ 105.5 K where the O+5 ionization fraction peaks",2
+2706,"Red novae are recognized as manifestations of on-going mergers of non-compact stars such as main-sequence dwarfs, sub-giants, or red giants",0
+2707,This method and its variants,0
+2708,have been used to estimate the angular power spectrum of the diffused galactic foreground,0
+2709,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.,0
+2710,"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",0
+2711,The spatial density measured with para-H2CO (303–202) and C18O (2–1) in N113 and N159W is n(H2) ~ 105 cm−3 on a size of ~30″,2
+2712,We perform this emissivity calculation separately for the main sample of spectroscopically confirmed LBGs and LAEs from M13 (using the UV luminosity functions from,2
+2713,"for LAEs),",2
+2714,"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",0
+2715,"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.",1
+2716,"Among the main proposed formation channels for merging binary COs, we find:",0
+2717,via stable mass transfer (e.g.,0
+2718,The gas-phase chemical network from Röllig et al. (2007) (mainly based on the UMIST99 ratefile;,2
+2719,"allows us to reproduce the C+, CO, and HCO+ abundances in PDRs",2
+2720,so we use this network together with the ionization of the atomic species and corresponding recombinations in the H ii regions.,2
+2721,Another element of the realistic phenomenological hadronic EoS corresponds to the short-range repulsive interaction of the hard core nature between particles,0
+2722,Although the production of HCOOH has also been investigated experimentally,0
+2723,its formation process and chemical link to nitrogen-bearing species are puzzling.,3
+2724,"So far, the biggest efforts were focused into two, somewhat complementary approaches. The first is represented by simulations like",0
+2725,Millennium II (ms-II;,0
+2726,"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.",0
+2727,"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",0
+2728,"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",0
+2729,Such carbonaceous mantles are efficiently processed by UV photons,0
+2730,but can stay H-rich as long as the radiation field is attenuated,0
+2731,We used shielding functions from,2
+2732,which include effects in lines.,2
+2733,"Indeed, the assignment in",6
+2734,was based on only one line of the gGg′ conformer of ethylene glycol about 200 cm-1,6
+2735,above the lowest-energy aGg′ conformer – and thus tentative.,6
+2736,"In this work, we will provide the ζ(T, f) function calculated under the assumption of ionization equilibrium using the CHIANTI spectral code",2
+2737,"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.",2
+2738,Observations have shown that the IRX-β relation varies with,0
+2739,age,0
+2740,"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 (∼104M⊙) (e.g.",0
+2741,"have shown that their age histograms contain a large majority of young (1–2 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",0
+2742,"It is likely that some of these products are also formed in our experiments, but except for CO2, HNCO, and NCO−, 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",1
+2743,we expect that the prevalent dissociation channels will lead to small molecules that will not interfere much with the absorptions of urea.,1
+2744,IRIS observations show that Fe XXI 1354.08 Å is a hot (∼11 MK) and broad emission line and is always blended with many narrow chromospheric lines at the flaring ribbons,2
+2745,Haloes were identified using rockstar,2
+2746,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 χ2 minimization,0
+2747,"\label{number5} \end{eqnarray}kα=κα/hα, kβ=κβ/hβ.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⊥≈−(∇ωc)t,which is a generalisation to three dimensions of the results of Mann et al. (1995),",2
+2748,and,2
+2749,"for lower dimensional systems, which developed phase mixing in only one perpendicular coordinate.",2
+2750,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.,1
+2751,"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",3
+2752,"The 16th and 84th percentile of the resulting peak flux density distributions, together with the systematic flux scale density uncertainty of 5%",2
+2753,"for the FIRST and LoTSS survey, respectively, are used to determine the error on the spectral index.",2
+2754,"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",0
+2755,Bound galaxies (subhaloes) were identified within the simulations using the subfind algorithm,2
+2756,in the same manner as in the EAGLE simulations,5
+2757,"As a result, recent studies have shifted to using dark-matter halo masses as large as 1011 M⊙",0
+2758,based on halo abundance matching arguments.,0
+2759,"However, the results of",6
+2760,show strong offsets in the kinematics of the gas from the host galaxy (≈100 km s−1;,6
+2761,whereas the COS-AGN sightlines do not (bottom panel of Fig. 6),6
+2762,"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",3
+2763,"In analyses of the resolved star formation properties of nearby disks, a near-unity index for the Schmidt–Kennicutt relation is also found in regimes where the molecular gas dominates the total gas mass surface density (Σgas >9 M⊙ pc−2; e.g.,",5
+2764,As pointed out by,1
+2765,"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, ⟨σα⟩∼σ68 ∼ σstd.",1
+2766,"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–host galaxies",0
+2767,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,0
+2768,"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.",3
+2769,Lupus 3 MMS is a Class 0 protostar with a bolometric luminosity (Lbol) of 0.41 L⊙ and a bolometric temperature (Tbol) of 39 K in the Lupus 3 cloud at a distance of 200 pc,0
+2770,The parameter m play crucial role in the launching of Blandford–Payne type wind from the accretion disc,0
+2771,While He lines are often removed due to substantial differences between magnetometry results obtained from He versus metallic lines (e.g.,1
+2772,"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.",1
+2773,"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,",0
+2774,and Gaia-ESO survey have led to the discovery of a large group of N-rich field stars,0
+2775,The residence time can be calculated as the time it takes to deflect the accelerated electron by an angle ~1/Γsh,2
+2776,"In addition, there is evidence demonstrating that bars can enhance star formation in the central regions of galaxies (e.g.",0
+2777,This connection between radio emission and star formation is strongly supported by the close infrared (IR)-radio correlation observed in galaxies (e.g.,0
+2778,We use the quadratic limb-darkening coefficients reported by,2
+2779,"to establish the stellar center-to-limb intensity profile,",2
+2780,"However, to date only the FIRE collaboration has implemented the two moment method (capable of dealing with CR streaming) in such simulations, and – in contrast to, for instance, van de Voort et al. (2021) – the plasma β in their winds is too high for the acoustic instability to develop",1
+2781,"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",0
+2782,The spectral properties of LAEs are usually interpreted as coming from young (≲50 Myr) and low-mass (M*​   ​1010 M⊙) galaxies,0
+2783,"which are actively star forming (SFR​ ∼ ​1 − 100 M⊙ yr−1) and dust poor (dust attenuation AV​   ​0.2, see e.g.",0
+2784,Using deep LOFAR 150 MHz observations in the 7 deg2 Boötes field,0
+2785,studied the FIRC at 150 MHz from z ∼ 0.05 out to z ∼ 2.5. They found fairly mild redshift evolution in the logarithmic IR to radio luminosity ratio in the form of qIR ∼ (1 + z)−0.22 ± 0.05.,0
+2786,"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.",1
+2787,The interplanetary manifestations of CMEs,0
+2788,can be measured by a spacecraft at about 1 AU and exhibit the following characteristics:,0
+2789,counterstreaming suprathermal electron (CSE) strahls and declining speed,0
+2790,"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",0
+2791,"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–colour diagrams",2
+2792,"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",1
+2793,A possible explanation for these low braking indices may be through the emission of a relativistic particle wind,0
+2794,"For example, Sirko et al. (2004), Kafle et al. (2012),",0
+2795,Kafle et al. (2014) and King et al. (2015) fit an ellipsoidal distribution of velocities,0
+2796,"Taking into account all these effects, the HPR of the overall RASS PSF is 84″",0
+2797,"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",0
+2798,"As of today, many more mass ejection channels have been discussed:",0
+2799,and by viscous effects,0
+2800,The course of the outburst was monitored in,0
+2801,sub-millimeter,0
+2802,It has been demonstrated that the statistical predictions of the ‘bubble model’ and the 21cmFAST agree fairly well with radiative–hydrodynamic simulations,5
+2803,"at least when recombination, feedback, etc. are ignored.",1
+2804,Because of their scale height,2
+2805,"these two sequences are associated with the thick disc (high-alpha) and thin disc (low-alpha), respectively.",2
+2806,This is in agreement with the finding that the thick disc has a shorter scale length than the thin disc,5
+2807,"In the case of collimated relativistic jets, magnetic fields must play an important role",3
+2808,"A periodogram of these RVs showed a clear signal at 35.57 days, but the TESS photometry and the RHK index",6
+2809,"indicate a stellar rotation period of around 35 days, calling for caution.",6
+2810,"The accretion rate then reaches the standard value predicted for MYSOs of $10^{-3}\, \rm M_{\odot }\, \rm yr^{-1}$",1
+2811,"up to the onset of the disc formation happening at ${\approx } 12\, \rm kyr$.",1
+2812,"Since the planet is synchronized within a timescale of a few thousand years, the stellar tide drives the secular orbital evolution",0
+2813,This method required,2
+2814,"to assume an effective medium theory, such that a pellet is a mixture of one of their samples with a matrix of air.",2
+2815,The slow rising afterglow light curves also rejected a uniform top-hat jet,1
+2816,"We have not included in our models the effects of ‘kicks’ 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.",6
+2817,"This effect, however, seems to affect less than 10 per cent of binaries",1
+2818,"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 γ Cephei",2
+2819,"do harbor planets. Therefore, some formation mechanism does in fact exist.",2
+2820,Owing to its proximity,0
+2821,"and nearly edge-on orientation, the Bar provides an ideal laboratory for testing PDR models",0
+2822,"and a primary target for observational studies of physical and chemical structures of PDRs (e.g.,",0
+2823,"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",0
+2824,"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",0
+2825,"Regarding its distance, there are currently two different methodologies based on parallaxes from Hipparcos",0
+2826,"and isochrone fitting, respectively.",0
+2827,"Traditionally, bulges were thought to invariably form early-on via",0
+2828,or mergers,0
+2829,with the disk gradually building up around them.,0
+2830,"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.",1
+2831,"No fits of these sizedistributions are available, but the figures in",2
+2832,and Price et al. (2010) indicate that the differential sizes may follow a log-normal distribution.,2
+2833,"These stellar absorption lines are intrinsically weak in star-forming galaxies, with EW0 typically well bellow 1 Å (e.g.",0
+2834,The general morphologies and the locations of the high-twist fields are also in agreement with many previous studies,5
+2835,"Second,",1
+2836,discovered that the distributions of X-ray photon spectral indices between RLAGNs and their radio-quiet counterpart are very similar,1
+2837,"The location of the star (Teff ≃ 45 000 K, log g ≃ 4.5;",5
+2838,is consistent with a current mass of M∼0.55 M⊙ which implies an initial mass in the main sequence of ∼1 M⊙.,5
+2839,By taking into account the results of the initial qualitative classification by Le Fèvre et al. (2020) and of the more recent quantitative analysis of a subsample of the ALPINE targets by,4
+2840,we proceed with a more in-depth characterization of the [CII]-detected galaxies aimed at obtaining a robust merger fraction at z ∼ 5.,4
+2841,Because they are detected in a wide variety of interstellar sources,0
+2842,and even in comets,3
+2843,it is of prime importance to understand well how these precursor molecules form.,3
+2844,"However, it is worth noting that since GRB relativistic blast waves generate synchrotron radiation as they expand into the circumstellar (wind generated) medium",2
+2845,we expect the forward-shock of the afterglow to peak more brightly at 15.7 GHz and at earlier times than the peaks recorded by Chandra & Frail (2012).,1
+2846,We therefore require a higher monitoring cadence at early times (within 5 d post-burst) to detect similar radio peaks.,2
+2847,The high-twist region in our result is also in agreement with,5
+2848,the location of the flare ribbons,5
+2849,The flexibility in ESPRESSO’s operations has been tackled by adopting a new DFS deployment plan described in,0
+2850,that is exceptional under various aspects because it has to cope with various telescope and instrument configurations while remaining operationally simple.,0
+2851,Many studies (e.g.,2
+2852,"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.",2
+2853,"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",0
+2854,The initial mass function of first stars is thought to be more or less top-heavy,0
+2855,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 Alfvén wave turbulence component,0
+2856,a view that is consistent with analysis of solar wind observations,5
+2857,and with the finding that quasi-2D turbulence alone is not sufficient to explain observed solar wind turbulence,5
+2858,"Due to different emission zone locations, standard pulsar radiation models include the",0
+2859,"the slot-gap (SG) (e.g.,",0
+2860,models.,0
+2861,"By averaging over 222 976 supergranular cells and applying time-distant helioseismic inversions,",1
+2862,"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 0.3–0.6 km s−1. 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.",1
+2863,"Scudder & Olbert (1979) also predict that the halo Ebp/kBTc ratio remains constant with heliocentric distance, whereas",6
+2864,find that the halo Ebp/kBTc ratio decreases with heliocentric distance.,6
+2865,"This is crucial since, although space weather forecasting often focuses on estimating the onset and intensity of geomagnetic storms",0
+2866,Previous works in the literature have shown an increase of [C/O] ratios as [O/H] increases (e.g.,1
+2867,but our ratios present a quite large dispersion that together with the shorter range in [O/H] prevents us from seeing a clear behaviour.,1
+2868,"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",0
+2869,and Bussmann et al. (2013).,0
+2870,"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",0
+2871,"In Figure 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",2
+2872,Other proposed solutions include those,0
+2873,or through dynamical feedback driven by starbursts or active galactic nuclei (AGNs;,0
+2874,The linear separation of the V and 37 GHz emission region can be estimated using the relation,2
+2875,"Secondly, the chemical abundance of SF galaxies at z ∼ 2 is lower by 0.1–0.3 dex for a given stellar mass compared to those at low-z",0
+2876,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,0
+2877,This also stresses the need for systemic tracers beyond  Lyα to distinguish IGM signatures and pinpoint the origins of various spectral features.,3
+2878,"More recently, unified EoSs for NS have been derived by the Brussels-Montreal group",0
+2879,"has also mentioned the well known problem of the “anomalous ions”, that is, the observed high intensities of the Li- and Na-like (as Si iv) ions",0
+2880,Additional searches in the infrared (IR) regime have yielded a few more candidates (e.g.,0
+2881,"Several studies show that one can distinguish at least classes of channels, such as isolated binaries and dynamically induced mergers,",0
+2882,as well as the orbital eccentricity at some reference GW frequency,0
+2883,"In the sub-Keplerian flow, shocks are formed when the Rankine–Hugoniot conditions are satisfied",0
+2884,"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",3
+2885,"Unlike common chemical peculiarities seen in Am and Ap stars, λ Boötis stars are not constrained to slow rotation",1
+2886,"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.,",1
+2887,"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.",1
+2888,"In addition, some models",0
+2889,exhibit low-frequency GW emission due to the standing accretion shock instability (SASI,0
+2890,"This condition corresponds for CG X-1 to the requirement MBH ≳ 1.5 vw, 10004δ2 M⊙, where MBH is the BH mass, vw, 1000 is the wind velocity in units of 1000 km s−1, and δ ≈ 1 is a dimensionless parameter",2
+2891,see also,2
+2892,"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-β",0
+2893,"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",1
+2894,"The recent discovery of peculiar highly overluminous SNeIa,",0
+2895,"indicates a huge Ni-mass and confirms the highly super-Chandrasekhar white dwarfs, having mass 2.1–2.8 M⊙, as a suitable progenitors",0
+2896,Predicting the amplitude of a solar cycle can be done using solar polar magnetic fields from the previous cycle as “precursors” of the next cycle,0
+2897,"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",5
+2898,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,5
+2899,using filament density as a proxy for the thickness of filaments,0
+2900,"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",0
+2901,"However, if this fraction is very low, as required if GW170817 leaves behind a black hole",1
+2902,the fast magnetar model may fail to explain the small fraction of LGRB/SLSN-like hosts in FRB samples.,1
+2903,The general morphologies and the locations of the high-twist fields are also in agreement with many previous studies,5
+2904,"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",0
+2905,"In particular, we have also used the ML1 (α = 1,a = 1 / 8,b = 1 / 2,c = 24,",2
+2906,We used the,2
+2907,"tracks, as recommended by Bruzual & Charlot (2003)",2
+2908,"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",0
+2909,"thus leading to the possible enhancement of HCN and the depletion of HCO+ via newly available formation and destruction paths, respectively.",0
+2910,"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",3
+2911,"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 μm infrared photons due to the presence of hot dust around AGN. These photons vibrationally excite HCN to the ν2 = 1 state. Upon de-exciting from this state back to the vibrational ground state, ν = 0, the HCN line intensities are thus pumped to higher fluxes",3
+2912,"However, we note that it is also not unlikely that the 12 μm infrared photons can similarly vibrationally excite HCO+, thus nullifying the extent of this effect",3
+2913,"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%–0.5% of that of their host star (e.g.,",0
+2914,"Alternatively, mass transfer rate-related events such as X-ray state changes and disc instability can also cause long-term modulations",1
+2915,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,3
+2916,The WD companions to Be stars proved unexpectedly elusive,0
+2917,"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–positron pairs or protons, respectively.",3
+2918,"The density can be expressed in number density of hydrogen atoms (mH = 1.6727 × 10-27 kg), 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−|z|100 pc,where z is the galactic height",2
+2919,and nH is given in atoms per cm3.,2
+2920,"However, as all results show that EII product ion fractions decrease as the complexity of the molecules increases",3
+2921,"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",1
+2922,The disk-wind model suggests that the BLR gas comes from winds produced by the accretion disk,0
+2923,Pioneering work with integral field unit (IFU) observations of four GPs,0
+2924,"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.",0
+2925,"This region exhibits a steeper density gradient in its outer envelope, with qout ≃ −2.5, also illustrated by the cloud structure studied with probability density function",5
+2926,"Interesting enough, these two portions of the stream are separated by a very narrow region across which Alfvénicity changes abruptly, from high to low",0
+2927,"During the occurrence of X-class flares, the complex AR had shown δ-sunspots, which are identified with a complex distribution of sunspot groups in which the umbrae of positive and negative polarities share a common penumbra",0
+2928,"This scenario is strengthened by the recent observations of warm Neptunes at the border of the desert, on the verge of",5
+2929,considerable mass-loss.,5
+2930,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,1
+2931,The general dynamics of this process have been studied extensively in purely hydrodynamical simulations,0
+2932,"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",1
+2933,"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",1
+2934,"In some cases, double relics have been detected on opposite sides of the cluster centre (e.g.,",0
+2935,"In these clusters it is possible to constrain the merger history, providing important information about the formation processes of relics.",0
+2936,"The mass accretion and loss rates for Class 0/I low-mass protostars span the range of 10−6–10−8 M⊙ yr−1, and the derived jet efficiencies (ratio between mass ejection and accretion rates) range between ∼1 per cent and 10 per cent (e.g.",0
+2937,"On the other hand, FRB 20180916B has a nominal RM and has shown a gradual variation in RM value over the two year timescale",6
+2938,"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",1
+2939,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−2 in all three plasma regions in the nose of the heliotail,1
+2940,"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.",1
+2941,"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",3
+2942,"It is unquestionable that such a unique sample of Cepheids – likely all members of the cluster and at the same distance, chemical composition and age – 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",3
+2943,"in both the optical and near-infrared bands, and have tested different methods to calibrate the PL relations in different filters.",3
+2944,"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",0
+2945,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,0
+2946,Similar results are obtained in studies of individual galaxies at z ∼ 6–8,5
+2947,"However, given the low angular resolution of these data, they can not rule out the possibility that one or more merging [C II]-bright satellites are mimicking the smooth gradient observed in the velocity maps",1
+2948,Massive YSO outflows mapped in high-velocity CO lines have collimation factors R = length/width ∼2.05 ± 0.96 as compared to R ∼ 2.81 ± 2.16 for low-mass stars,1
+2949,indicating a weak tendency that outflows associated with massive stars are less collimated than those from low-mass stars as previously thought,1
+2950,The combined detector and telescope PSFs are described in detail in,0
+2951,"In addition,",1
+2952,and the snow line is located at a greater distance from the central star,1
+2953,"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.",1
+2954,"Specifically, we create mock data cubes that mimic ALFALFA observations",2
+2955,Recent work also finds that transient spiral structure,0
+2956,"may lead to the formation of moving groups,",0
+2957,"Thus, in order to discover all planets in a system, one either needs to image old stars – which seems currently impossible given the already low detection rate around young stars probed by large DI surveys (e.g.,",0
+2958,– or try to minimize the impact of the stellar activity of young stars.,0
+2959,"Furthermore, even spherical grains can produce polarized emission by self-scattering of large grains in an anisotropic radiation field",1
+2960,FSRQs have high luminosity and a thin and radiatively efficient black hole accretion disk,0
+2961,"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;",0
+2962,"The user defined heating is therefore highly stratified, spatially smooth and steady (e.g.",1
+2963,KOI-94,3
+2964,is interesting because of the presence of a Saturn mass planet in a similar orbit to 55 Cancri.,3
+2965,"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⊕ 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.",1
+2966,"We expect to detect the GWB first, followed by detection of individual SMBHBs",0
+2967,that stand out above the GWB.,0
+2968,"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",1
+2969,and Higa et al. (1996).,1
+2970,Strong non-potential field arcades have been observed in hot X-ray sigmoids on scales of hundreds of arseconds,0
+2971,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.,0
+2972,Absorption coefficients for pure water ice (kH2O) at sub-mm-to-cm wavelengths are discussed extensively by,0
+2973,who also provides several analytic formulations to estimate them as a function of frequency and temperature along with illustrative plots.,0
+2974,This trend is in agreement with the metallicity dependent yields from,5
+2975,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).,5
+2976,Recent numerical studies,0
+2977,"show that the retention of BHs in dense stellar clusters of wide mass range, beginning from low-/medium-mass young and open clusters",0
+2978,through globular clusters,0
+2979,"comprise environments where BHs can pair up through close dynamical interactions, which, furthermore, lead to general-relativistic (hereafter GR) coalescences of these BBHs.",0
+2980,"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",2
+2981,"We followed the second approach since there are natural thermal instabilities in the plasma, such as instability caused by X-ray irradiation",2
+2982,"The abundances of these rare but massive subhaloes has important implications for, among others, the statistics of massive satellite galaxies (e.g.",3
+2983,"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 ΛCDM with Ωm = 0.27, so-called Rh = ct universe",2
+2984,A cross-correlation method was applied to derive continuous 2D speed maps of a CME from coronagraphic images by,2
+2985,"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 h−1)3) to expect such an object (e.g.",2
+2986,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,0
+2987,"There are two primary causes for darkness in GRBs: attenuation by dust, or rest frame ultraviolet H i absorption at high redshift",0
+2988,The number density of the ambient medium is assumed to be,2
+2989,"In absorption, bands at 3.4, 6.85, and 7.25 μm 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.",5
+2990,there is a second OB star mentioned by,0
+2991,but its location is actually outside the structure,0
+2992,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,0
+2993,The Sun is situated at the inner edge of the Orion arm,0
+2994,"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",1
+2995,though this finding is still debated,1
+2996,The discrepancy can be calculated using a statistic like χ2,1
+2997,but here we will work with the Freeman–Tukey discrepancy since it is weight independent,1
+2998,"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.",2
+2999,These values were computed by an analysis of the differences between the Portsmouth stellar masses of our galaxies,2
+3000,Previous studies have considered the implications of structure models on the true energetics and rates of GRBs,0
+3001,while the Σnl parameter encodes the smoothing of the BAO peak due to non-linear effects,2
+3002,"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—all of these small-scale magnetic activities contribute greatly to coronal heating",0
+3003,"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.,",2
+3004,Our estimate of the stellar mass fraction agrees,5
+3005,and with the estimates from strong lensing studies (see for example,5
+3006,which produced stellar mass fractions in the range 30%–70% integrated inside the Einstein radius of the lenses.,5
+3007,"In particular, solar wind samples containing more Alfvénic fluctuations are typically associated with less developed turbulence, as inferred from both shallower spectra and reduced intermittency (see",0
+3008,and references therein).,0
+3009,"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",1
+3010,"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.",3
+3011,"Therefore, during our fitting procedure we use the frequencies determined in",2
+3012,as starting values plus their derived errors as Gaussian priors,2
+3013,"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",1
+3014,"while ‘achromatic’ flux variability (no colour evolution,",0
+3015,have also been reported.,0
+3016,"Even though arguments (e.g. variability,",6
+3017,"exist that favour a compact corona, we used extended coronae.",6
+3018,"To obtain the structural parameters of the LSBG candidates, the detected sources are usually fitted with a Sérsic model",1
+3019,Specific procedures such as GALFIT,1
+3020,or IMFIT,1
+3021,"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 Sérsic fitting to save computational time. This is not trivial because structural parameters from automated segmentation catalogs are much less accurate than Sérsic fit modeling, making correct screening of the sample challenging. As a last step, a “supervision” 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.",1
+3022,Other single-dish samples of SMGs have also been obtained at 1.1–1.3 mm using,0
+3023,and at 2 mm with GISMO,0
+3024,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,0
+3025,"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",2
+3026,It has been shown elsewhere that these models produce similar results to those of numerical cosmological simulations and other SAMs,5
+3027,and that they are also in agreement with higher redshift observations of galaxy populations,5
+3028,the reionization history,5
+3029,We also show the Spitzer Infrared Nearby Galaxy Sample,2
+3030,analyzed in da Cunha et al. (2008) as purple stars for comparison.,2
+3031,"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",1
+3032,The angular speed was estimated based on the global velocity gradient along the major axis of the dense core observed with single-dish telescopes,2
+3033,Following the results shown in Fig. 2 of,2
+3034,"we roughly estimated that XO-2N could have ingested an amount of iron slightly higher than 5 M⊕ to increase its photospheric iron content by ~0.05 dex, given its Teff ~ 5300 K.",2
+3035,"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",2
+3036,"Marks et 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",0
+3037,This initial binary population is then altered by dynamical evolution. Close binaries with orbital periods below about 10Â days undergo eigenevolution,0
+3038,"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.",0
+3039,Strong non-potential field arcades have been observed in,1
+3040,micro-sigmoids in soft X-ray imaging on scales of ∼50″,1
+3041,and now at EUV temperatures in QS-like mixed network fields with lengths down to ∼10″. 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.,1
+3042,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,0
+3043,Surveys of radio bursts in decimetric wavelengths is presented in papers by Isliker & Benz (1994) and,0
+3044,"within 1–3 GHz and 0.8–2.0 GHz frequency ranges, respectively.",0
+3045,FDs caused by high-speed streams (HSS) from coronal holes (CHs) have a recurrent character,0
+3046,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,7
+3047,"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.",5
+3048,"Also, we consider $Q^{+}_{{\rm diss}}-Q^{-}_{{\rm rad}}=fQ^{+}_{{\rm diss}}$ in ADAFs (where f, the advection parameter, is defined by",2
+3049,The linear relationship that we observe between breakpoint energy and core temperature is in line with previous measurements (e.g.,5
+3050,for both the halo and strahl.,5
+3051,"For more details, we refer the readers to",0
+3052,While we know that very massive stars (VMS) above 100  M⊙ exist,0
+3053,this mass is significantly diminished via stellar winds already during core hydrogen (H) burning,0
+3054,Previous works,1
+3055,have found very high reddening and densities associated with ionised outflows in local objects,1
+3056,"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",0
+3057,through detailed 3D simulations.,0
+3058,"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,",0
+3059,The,0
+3060,"photometric follow-up started in August, 2010, and ended in October, 2012, coinciding with these LBT data.",0
+3061,The discrepancy is even larger in the case of the low-mass models of,6
+3062,"After combining with the existing NB2071 data (186 min integration), we reconstructed all the data using the reduction pipeline mcsred2",2
+3063,which is written as iraf3 scripts,2
+3064,Using the diagonal elements of the 14N quadrupole coupling tensor in NEFA,2
+3065,we have computed the expected hyperfine splitting of all lines in the W band.,2
+3066,"From studies on the optical–IR colour–magnitude diagram, it is known that FSRQs in general show an RWB trend, which is attributed to them having a luminous accretion disc",0
+3067,"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",2
+3068,"These galaxies hereafter referred to as LyC leakers, possess many properties similar to those of high-redshift galaxies both at z ∼ 2–3 and z$\gtrsim$ 6 such as compact morphology with similar galaxy radii (e.g.",1
+3069,"Later on, Gomes et al. (2005), Gallardo et al. (2012), and",0
+3070,showed that the Lidov–Kozai 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.,0
+3071,Since these characteristics are somewhat consistent with model predictions for drift mode of MTSI,5
+3072,", 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.",5
+3073,We used data for two clusters observed by Kaluzny and his collaborators with the highest number of CBs (except for ω Centauri).,2
+3074,"In M4,",0
+3075,detected nine CBs with one BS among them,0
+3076,Polarimetricimages with,2
+3077,SPHERE,2
+3078,"show a gap at around 36 au, with an outer ring at a separation >40 au from the star.",2
+3079,"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",0
+3080,"However, there is an important caveat; PAHs are destroyed by ionizing radiation from newly formed stars",1
+3081,"leading to a deficit in the 8 μm luminosity in galaxies with low metallicity, whereas PAHs are less well shielded by metals",1
+3082,"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 ≲ 0.4, following previous works such as Wellstein et al. (2001), Hurley et al. (2002) and",0
+3083,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.,1
+3084,The concentration parameter is defined as the ratio of the surface brightness within 0.1 R500 to the surface brightness within R500,0
+3085,"Intuitively, the expectation is that the smaller the core radius, the more compact the cluster.",0
+3086,"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.",1
+3087,assuming a mean beam efficiency ηMB = 0.49,2
+3088,"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",0
+3089,"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.",0
+3090,Observations have struggled to confirm these theories.,6
+3091,"Moreover, the degree of central concentration of a halo depends on its formation epoch and hence on its total mass (e.g.,",1
+3092,"This is consistent with the magnetic field measured by Hubrig et al. (2009), 89 ± 26 G, although non detections have also been reported",5
+3093,In our long-term project aimed at reconstructing the past magnetic activity on the Sun,3
+3094,"we also use indirect measurements of magnetic fields obtained, in particular, from chromospheric spectroheliograms.",3
+3095,In the work by,2
+3096,", 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.",2
+3097,"Historically, systematic studies of galactic outflows in nearby and high-z galaxies have focused on",0
+3098,"and the atomic phase – based on the Na D or Mg II lines in absorption (e.g.,",0
+3099,"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.,",1
+3100,"To allow fast calculations, we make the major assumption that the grains are spherical and compute their optical properties using the Mie theory",2
+3101,with the Fortran 90 version of the BHMIE routine given in,2
+3102,"The oxygen line ratio [O III]λ 5007 Å/[O II] λλ3726, 3728 Å (O32) proposed by Jaskot & Oey (2013) and",2
+3103,was successfully used to select LyC-leaking candidates,2
+3104,"From the theoretical point of view, it is believed that low-mass main-sequence stars synthesize 3He through the p–p chains with peak abundances of few 10−3 by number",0
+3105,"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",2
+3106,first presented the dynamical estimate of mass of the source to be around 7.4 ± 1.1 M⊙.,2
+3107,"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",0
+3108,"First, ultra-hot Jupiters are accessible objects to observe. Their short orbital periods (1–2 d) and hot, extended atmospheres make them perfect targets for transmission spectroscopy",3
+3109,"Based on a radial velocity of $-13\pm 17\, {\rm km^{\rm -1}}$ and a distance of 2.07 ± 0.18 kpc",2
+3110,", 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 $W=3.1\pm 5\, {\rm km^{\rm -1}}$.",2
+3111,"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",0
+3112,"Each of the new detrended light curves, jointly with the nominal PDC-SAP flux, is then processed through the transit least squares (TLS) package",2
+3113,in the search for transits.,2
+3114,In contrast to the classical box least-squares (BLS) algorithm,1
+3115,the TLS algorithm uses an analytical transit model that takes the stellar parameters into account.,1
+3116,"For the case of β Pictoris and HD 169142, also having giant planets at long distances, CA models seem to be favored",0
+3117,"The exact value of the interferometer’s modulation efficiency (ME), which acts essentially as an additional throughput loss, is the major source of uncertainty on the absolute flux calibration",0
+3118,We also show as a gray band the best fit for the stellar fraction in the form of stars determined by,2
+3119,"in a study of a large sample of lens galaxies using strong lensing and photometry,",2
+3120,"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.",0
+3121,"the number of known SMGs is now of the order of a few thousand (e.g.,",0
+3122,and intensive observational efforts have been devoted to understanding their physical properties.,0
+3123,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,0
+3124,We recall that in these models (see also,2
+3125,"the dense clouds can be either self-gravitating virialised clouds, which implies that their internal velocity dispersion (Δvsg) is locked to their mass (Mvir) and size (R) through Δvsg = (GMvir/G)1/2, or unbound clouds, for which Δv ≫ Δvsg.",2
+3126,"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",7
+3127,XRD performed by,1
+3128,"of the sample of bayerite prepared at 1273 K suggests only θ-alumina was present, and their infrared and NMR spectroscopy confirms this.",1
+3129,From the convective flux as presented in,5
+3130,one also would expect a similar temperature gradient in the overshooting zone.,5
+3131,"Of course, the recent report of an absorption signal in the sky-averaged spectrum at z ∼ 17 from EDGES (Bowman et al. 2018)",3
+3132,or a brighter background,3
+3133,than models in ΛCDM cosmologies generally predict.,3
+3134,"Subsequent observations have led to the detection of new metastable ammonia masers, including",0
+3135,"NH3 (2,2)",0
+3136,"However, over the last few years a number of multifrequency compact source detection techniques have been proposed in the literature",3
+3137,Despite a direct conflict,1
+3138,with the theoretical expectation that the IMF should vary as the star-forming environment alters,1
+3139,the observed IMFs of star clusters in the local Universe are consistent with no variation,1
+3140,"In this case, the mass of the white dwarf is also calculated from the IMFR of",2
+3141,Many previous works,2
+3142,used a constant smoothing length.,2
+3143,"Using 3D simulations,",0
+3144,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 “observed” intensity fluctuations due to radiative transfer could be significant enough to reverse the sense of mode asymmetry.,0
+3145,"For the lowest 41 energy levels, we see that our calculated energies and previous fac energies",5
+3146,belonging to the n = 3 complex in Ni xiv agree well with each other and both set of calculation are of the same accuracy.,5
+3147,"However, our calculated ground state configuration levels show better agreement with measured energies in comparison to those of fac calculations (7.2 per cent).",6
+3148,"As predicted by asymptotic theory, the pulsation periods for γ Dor and SPB stars were observed to form period spacing patterns (e.g.",0
+3149,"On the other hand, the stellar rotation leads to shifts in the observed pulsation mode frequencies",3
+3150,"Indeed, the ultraviolet and X-ray variability detected for many of these LINERs",1
+3151,is in favour of a direct view of the AGNs (i.e. perpendicular to the disc under the UM).,1
+3152,"This is consistent with the fact that most of the [O III] morphologies found for LINERs are spheroids, if we assume that the [O III] traces the NLR.",5
+3153,"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.,",0
+3154,"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",0
+3155,"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",0
+3156,SEP events with gigaelectronvolt components are accompanied by type II radio bursts from meter (m) wavelengths to kilometer (km) wavelengths,0
+3157,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,0
+3158,he RWI can be triggered at steep radial density gradients,0
+3159,such a gradient may be generated at the viscosity transition between regions in which the magnetorotational instability can operate (e.g.,0
+3160,This group was complemented by,2
+3161,the four candidate HVSs from the LAMOST survey,2
+3162,Numerous studies have been performed using chemical models,0
+3163,"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",1
+3164,"from a more recent origin following its injection into the inner Solar System (e.g.,",1
+3165,"Low gas temperatures are associated with Serpens South ranging from 8.9 to 16.8 K with an average of 12.3 ± 1.7 K, which is consistent with the mean value of 11 ± 1 K found by",5
+3166,"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",5
+3167,"and also numerical simulations (see, e.g.",5
+3168,"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.",1
+3169,"Improvements in cosmological measurement in recent years have been said to hail an era of “precision cosmology,” with observations of",0
+3170,luminosity distance–redshift relation of Type Ia supernovae (SNIa;,0
+3171,"providing constraints on cosmological model parameters at percent, or subpercent, level precision.",0
+3172,Possible compact-object merger pathways include isolated binary evolution,0
+3173,accompanied by mass transfer,0
+3174,These parameters are entirely consistent with those found in preliminary studies,5
+3175,"Here, we present a new approach to derive the VDF based on the lens redshift distribution",2
+3176,"and to constrain its evolution out to z ∼ 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).",2
+3177,"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",0
+3178,"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",5
+3179,"However,",6
+3180,reported that there is no correlation between the turbulent and outflow energies.,6
+3181,"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",0
+3182,"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.",0
+3183,of the orbital phase (while the MSP remains largely uneclipsed at inferior conjunction of the pulsar).,0
+3184,"M15 show, via use of covariance spectra (see",0
+3185,"for a review of the technique), that the ULX continuum emission originates from at least two components that cross at ∼1 keV.",0
+3186,"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° in longitude",0
+3187,and that near-relativistic electron events can spread up to almost all around the Sun.,0
+3188,"For these reasons, detections in emission at high-redshifts are currently limited to deep fields",3
+3189,while detections at z1 are now becoming available,3
+3190,Many studies of the outburst evolution of these sources have been reported in the literature (e.g.,0
+3191,"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.",0
+3192,The angular expansion rate of 0.64 arcsec yr−1 obtained from comparing X-ray images from 2007 and 2009,2
+3193,"gives an upper limit for the age of about 160 yr, less if (as is almost certainly the case) deceleration has occurred;",2
+3194,"This boils down to quantifying the relation between molecular gas and star formation rate (SFR), which appears nearly linear in nearby discs",0
+3195,"In precision cosmology, Bayesian inference is the main tool for setting constraints on cosmological parameters",0
+3196,"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 J1745–290 and the diffuse emission",0
+3197,"The three transitions of singly ionized Sulfur (Sii; upper ionization potential 23.3 eV) at λλ1250.58, 1253.81, 1259.52Å represent important tracers for neutral and weakly ionized gas in the local interstellar and intergalactic medium and in distant galaxies (e.g.",2
+3198,"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",5
+3199,"with the sole exception of cluster ESO121-3 and very recently also KMHK1592, as reported by",6
+3200,"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",0
+3201,The nonlinear PT for MG was developed initially in,2
+3202,and has been further studied in several other works,4
+3203,"Observations on smaller, sub galactic scales, have proven more problematic for ΛCDM, with suggestions that the low abundance (e.g.",1
+3204,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.,1
+3205,The LS-Ska,0
+3206,"EoSs were constructed using the Skyrme effective nuclear forces Ska and SLy4, respectively.",0
+3207,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,0
+3208,"First, thermodynamic calculations of conditions in photodissociation regions (PDRs) have been coupled with self-consistent equations for the thermally driven disc wind",2
+3209,"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",3
+3210,"As a result, magnetars have been suggested as the central engines for some GRBs, including both long and short events",0
+3211,This problem might be alleviated in future simulations by introducing more realistic top boundary conditions like that used in,7
+3212,"These vortices tend to have a long lifetime and are widely observed in space, laboratory, and numerical simulation of plasma",0
+3213,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,0
+3214,"Following the approach of Nguyen et al. (2010), we have inferred a GCE relationship between δ29Si 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",2
+3215,Such non-evolving VDF has been extensively applied in the previous studies on lensing statistics,0
+3216,"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",0
+3217,"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",2
+3218,The dust-based estimates of G18 and,0
+3219,"(and, by extension, the z ∼ 3 semi-constraints) assume a gas-to-dust ratio (G/D).",0
+3220,"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.,",5
+3221,"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",2
+3222,The RVs were measured using the two-dimensional cross-correlation algorithm TODCOR,2
+3223,The captured material can form a quasi-spherical shell,0
+3224,"The standard internal shock model of blazars considers that the discrete ejecta with higher speeds (with Lorentz factor Γf) catch up with the preceding slower ejecta (with Lorentz factor Γs), and the collision leads to the nonthermal emission (e.g.,",0
+3225,"Indeed, some misaligned circumbinary discs have already been reported",3
+3226,and HD 98800B,3
+3227,"The two panels show model spectra at times t = 0, 1, 3, 5, and 7 Myr after a coeval burst of star formation, using evolutionary tracks with rotation, at solar metallicity (Z = 0.014 from",2
+3228,After the discovery of the first FRB,0
+3229,"a number of dedicated facilities have been conducted to search FRBs, such as",0
+3230,and the Five-hundred-meter Aperture Spherical radio Telescope (FAST;,0
+3231,"All these efforts result in an increasing rate of new FRB detections. Among them, more than 20 repeating FRBs have been reported.",0
+3232,"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",2
+3233,the predicted number of cluster M stars doubles considering the mass interval 0.25–0.5 M⊙ rather than 0.35–0.5 M⊙.,2
+3234,The second scenario involves mass transfer episodes and the evolution of the binary is obtained following the prescriptions of the bse package,2
+3235,following the parameter assumptions detailed in Camacho et al. (2014).,2
+3236,"The covariance of the 3PCF, on the other hand, is not diagonal, even for Gaussian fluctuations, which makes the modelling more difficult",0
+3237,"In the last 20 years, disc-oscillation and resonance models and wave models have been proposed (e.g.",0
+3238,"Temporal variability studies during the 2012 September–October multi-band flaring period found a near-simultaneous γ-ray and optical flaring behavior, inferring a co-spatial origin",1
+3239,As reported in previous works,2
+3240,"this interval is characterized by two different spectral scalings: a typical inertial range ∼ τ5/3 is found at large scales (i.e., τ > τb), while a steeper scaling ∼ τ7/3 is found at small scales (i.e., τ τb), with τb ∼ 2.4 s",2
+3241,"For a galaxy of halo mass Mh, the relation between the halo mass and the velocity dispersion is simply Mh = 2σ2R/G; while the velocity dispersion can be directly related to the black hole mass using the MBH–σ relation",2
+3242,"The most basic result, already mentioned in Sect. 4.4.1, is that initial conditions which have a finite nonzero flux integral (called ‘the mass’ in the mathematical literature for the PME) converge toward the ZKBP solution with the same flux integral (‘mass’) asymptotically in time",1
+3243,"Theorem 18.2); here, allowance is made for either a positive or negative flux integral by globally changing the sign of the ZKBP solution",1
+3244,"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",0
+3245,"with an X-ray luminosity much smaller than expected, i.e., much smaller than the disk luminosity.",0
+3246,"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",0
+3247,Signatures of past mergers take the form of faint extended tidal features such as tails (e.g.,0
+3248,– which are typically produced by major mergers,0
+3249,"Several studies of lower-luminosity AGN host morphologies with inactive control samples have been conducted in HST extragalactic survey fields (e.g.,",0
+3250,"[C ii] 158-μm luminosity, L[C II], has been discussed as an indicator of SFR (e.g.",3
+3251,"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 ν−2 or even ν−3 (see e.g.",3
+3252,", in contrast with a typical ν−0.8 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).",3
+3253,"the farthest blazar detected so far is at z = 5.47,",0
+3254,"From 2008–2009 INTEGRAL data, Beckmann & Do Cao (2010) report a cut-off of ∼80 keV with a hard photon index, but these results are not confirmed by NuSTAR",1
+3255,Studies of orbit composition of B/PS bulges and X-structures in different numerical and analytical models,0
+3256,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.,0
+3257,This is indeed the case for the realistic bar potential,0
+3258,"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",6
+3259,"With the goal of identifying new exotic pulsar systems or highly stable MSPs suitable for PTA studies, the SPAN512 pulsar survey",3
+3260,was conducted between 2012 and 2018 at the NRT.,3
+3261,"CS approaches based on constrained optimization problems, solved via convex optimization techniques, have been applied broadly in RI imaging",0
+3262,"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.",1
+3263,"This approximation works well, even for evolved density fields, while deviations from Gaussianity can also be taken into account",1
+3264,and possible alternative explanations of the changing-look behaviour are,1
+3265,"transient events, e.g. tidal disruption of a star by the central black hole (e.g.",1
+3266,Stripping and star formation consume the available gas and galaxies first appear as truncated disks,0
+3267,Optical ionised gas has been observed by,0
+3268,"next to the black hole in a field of view1 of 5′′ × 3.5′′, but this emission is weak.",0
+3269,Initially the core size of a galaxy was determined by fitting the so-called ‘Nuker-profile’,0
+3270,"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.",0
+3271,"In these radiative envelopes, the transport of chemical elements on a macroscopic scale is ascribed to",0
+3272,"or internal gravity waves (IGWs, e.g.,",0
+3273,The problem of accretion on to an SMBH has been studied via hydrodynamical simulations (e.g.,0
+3274,"More recently, the emission-line OMEGA-OSIRIS survey provided similar results",0
+3275,Many simulations consider either an intermediate-mass BH (e.g.,0
+3276,"Accordingly, it is informative to investigate the shape of the probability distribution of the matter density field and its evolution",3
+3277,"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",0
+3278,"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.",0
+3279,"In this scenario, depending on the misalignment angle, the outer disk image will show narrow shadow lanes (e.g.,",1
+3280,The reason that high-velocity features are interesting to investigate in connection with blueshifted Na i D features is that there are suggestions that the high-velocity Ca ii features may be at least partially due to ejecta–CSM interaction (e.g.,3
+3281,"Therefore, if a link between these quantities was identified, it would provide evidence that blueshifted Na i D features are due to CSM also rather than contamination.",3
+3282,"CMEs have been observed to occur often having spatial and temporal relation with solar flares, eruptive prominences",0
+3283,"In order to produce a steep gravitational potential at low |z|, there could be a breathing mode in the stellar disk",2
+3284,which is currently in its most compressed state.,2
+3285,"Indeed, other studies confirm that abiotic buildup of ozone is possible (e.g.,",5
+3286,The input of dust from the inner disc triggers a streaming instability in the outer disc,2
+3287,lasting ≈0.1 Myr and concentrating pebbles and fractals sticking to pebbles into filaments where the comet nucleus collapses by gravity at speeds 1 m s−1 into a randomly packed,2
+3288,"aggregate of cm-sized pebbles, with the fractals stored in the voids among the pebbles",2
+3289,"In addition to morphological disturbances, galaxy mergers can trigger vigorous galactic outflows associated with feedback from the enhanced star formation (e.g.",0
+3290,Similar conclusions can be reached for the,5
+3291,sample where they adopt the same analysis as in Nestor et al. (2013).,5
+3292,"For example, star count observations in the solar neighbourhood",0
+3293,followed by its characterization as the old α-enhanced population in the double sequence exhibited by the solar neighbourhood stars in the [α/Fe] versus [Fe/H] plane,0
+3294,"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",2
+3295,"Each deformable mirror uses 672 actuators that routinely correct 400 modes and provide Strehl ratios exceeding 80%, 95%, and 99% at 1.6 μm, 3.8 μm, and 10 μm, respectively",0
+3296,In our second work,0
+3297,"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.",0
+3298,"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",2
+3299,This matter replenishment may be channeled from within the cloud itself through molecular filaments,0
+3300,or toward hubs,0
+3301,"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",0
+3302,Theoretical models have found that CO should be the dominant carbon-bearing molecule for hydrogen-dominated atmospheres above 1000 K,1
+3303,and CO has been detected at high resolution in hot Jupiter atmospheres (e.g.,1
+3304,"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",0
+3305,The discovery of snail shells in the phase-space distribution of MW disk stars,0
+3306,has inspired debates about their origin:,0
+3307,"Another model for their formation is by increasing their spin rates due to incident and remitted solar photons, known as the Yarkovsky–O'Keefe–Radzievskii–Paddack (YORP) effect. The YORP effect on contact binary asteroids has been studied",0
+3308,A sample that contains 120 angular size measurements in intermediate-luminosity quasars from the very long baseline interferometry (VLBI) observations,0
+3309,"has become an effective standard ruler, which have been extensively applied to test cosmological models",0
+3310,"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.,",0
+3311,have shown that the turbulent cascade in magnetized plasma tends to develop mainly in directions perpendicular to B0.,0
+3312,The linear stability analysis of these idealized configurations,5
+3313,as well as the corresponding non-linear solutions (e.g.,5
+3314,confirms this view.,5
+3315,These properties can also be explained by the locations of resonances,1
+3316,Varying star densities can affect the results (e.g.,2
+3317,In this section we therefore explore the sensitivity of the shear measurement bias to various assumptions and simplifications made in the simulations.,2
+3318,Most DSFGs are discovered in wide-area observations using single-dish far-IR (FIR)/millimeter instruments such as,0
+3319,the Herschel Space Observatory,0
+3320,"In addition, we also included fgas estimates derived from the (median) stacked FIR spectral energy distributions of ETGs at",2
+3321,"z ∼ 1.2, z ∼ 0.8, and z ∼ 0.5 (1394, 1536, and 563 galaxies, respectively;",2
+3322,hereafter M20,2
+3323,"Increasing numbers of LAEs are being observed by surveys including narrow-band imaging (e.g.,",0
+3324,Recent work also finds that transient spiral structure,0
+3325,"may lead to the formation of moving groups, as well as perturbations due to spiral arms in the MW",0
+3326,"As a consequence, only large or massive planets are detected around the classical evolved stars",1
+3327,and references therein,1
+3328,"The atmosphere above the Canary Islands, and especially the western islands Tenerife and La Palma, has been extensively characterized over the past 50 yr",0
+3329,(54 509) was the first asteroid for which the effect of YORP has been observed,0
+3330,"There is indeed evidence for a potentially large population of heavily obscured, possibly Compton-thick AGN, among the WISE population (e.g.",0
+3331,"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",2
+3332,"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–2 and SMC X–1;",5
+3333,These characteristics resemble closest the behavior often observed in (luminous) red novae,0
+3334,a modern category of eruptive stars known from our and other galaxies (e.g.,0
+3335,"J04221332+1934392 (a~7 AU,",2
+3336,"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.",1
+3337,"Some recent investigations showed that the mass-transfer process in the lobe-filling BH binaries is more stable than previously expected (e.g.,",2
+3338,; the maximal mass ratio of the donor star to the BH for stable mass transfer can reach as high as ∼6. Hence only a few BH–He XRBs with orbital periods of ≲1 day are produced in our calculations.,2
+3339,"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",2
+3340,In this context we promoted the ESO-VLT Multi-Instrument Kinematic Survey (hereafter the MIKiS survey;,3
+3341,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.,3
+3342,"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.",0
+3343,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.,1
+3344,The concentration parameter is defined as the ratio of the surface brightness within 0.1 R500 to the surface brightness within R500,2
+3345,Note that there is some degeneracy between broken power-law break frequency,1
+3346,"and extinction, which could lead to inference of grey dust for some instances",1
+3347,"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",1
+3348,"and included in the Tholen taxonomy, due to its flat spectrum and low albedo;",1
+3349,"Although it appears that small-scale flux ropes tend to contract or merge predominantly incompressibly in discussions of particle simulations (e.g.,",1
+3350,"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.,",0
+3351,"However, the measured solar disk emission flux was about a factor of seven higher than that predicted about this disk component by a “nominal” model",6
+3352,"In the past, the limited observations showed that precursor activities of solar eruptions can come in various forms,",0
+3353,as well as nonthermal processes in microwave or hard X-ray wavelength,0
+3354,are most common ones.,0
+3355,"Moreover, these disc-sources are confirmed to be binaries and show orbital periods between 100 and 2000 d",1
+3356,"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.,",0
+3357,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,0
+3358,"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.,",1
+3359,The global fits included,2
+3360,29 lines from,2
+3361,"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.,",1
+3362,"Based on this behaviour, it becomes possible to form hot Jupiters on retrograde orbits by combining the eccentric ZLK effect and tidal friction",0
+3363,"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 Å, the Fe ii lines at 1353.02 Å, 1354.01 Å, and 1354.75 Å, the Si ii lines at 1352.64 Å and 1353.72 Å, and the unidentified lines at 1353.32 Å and 1353.39 Å (e.g.,",0
+3364,"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",3
+3365,"Furthermore, in galactic nuclei with a high X-ray flux we would expect to see an increase in the dust temperature and infrared luminosity",2
+3366,"Therefore in galactic nuclei, and in particular in AGNs, we expect a reduction in [C ii] emission relative to FIR/IR emission depending on the relative contribution of different ISM components to the [C ii] luminosity.",2
+3367,"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",1
+3368,"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",5
+3369,These explanations can be very roughly divided into two main categories:,0
+3370,"and mergers due to dynamical interactions (e.g.,",0
+3371,"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",1
+3372,"The Rayleigh–Jeans 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",0
+3373,"In the regime of stability, the normal modes are undamped oscillation modes in absence of lateral streaming",2
+3374,"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",2
+3375,if Ngds+is = 0 in that mass bin.,2
+3376,This method and its variants,0
+3377,have been used to estimate,0
+3378,as well as the power spectrum of H i distribution in nearby galaxies,0
+3379,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.,0
+3380,"Observational calibrations of the virial factor also tend to support this conclusion (e.g.,",5
+3381,"according to diffusive shock acceleration (DSA; e.g.,",2
+3382,"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",5
+3383,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,0
+3384,"To estimate the positions of the snow lines in observed disks, the temperature profile is often assumed to be a simple power law",2
+3385,which is broken if the disk has shadows on the disk surface,2
+3386,"The last column in Table 1 reports the number of OB stars minus the “diffuse” 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",2
+3387,is assumed for the star-formation region.,2
+3388,"The spectrum of He seems harder than that of H as indicated by many spectral studies, implying, e.g. time-dependent particle acceleration",1
+3389,or more efficient He injection in the shock acceleration process,1
+3390,The turning point of increased relative production of carbon from massive stars takes place at A(O) ~ 8.7 dex (see Fig. 2 of,2
+3391,which equals to [O/H] ~ 0.0 dex.,2
+3392,"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).",6
+3393,"In the simulations, hydrodynamics and neutrino transfer in general relativity are solved simultaneously",2
+3394,"Alone, the energy released by jetted outflows appears to be on the same order as the energy needed to offset cooling (e.g.",2
+3395,therefore suggesting that AGN feedback is a good candidate for solving the cooling flow problem.,2
+3396,Other proposed solutions include,0
+3397,or through dynamical feedback driven by starbursts or active galactic nuclei,0
+3398,"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",1
+3399,The starting point is the “hybrid Vlasov–Maxwell” (HVM) code,2
+3400,"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∥, e and p⊥, e (where ∥ and ⊥ refer to the local magnetic-field direction, b = B/|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∥, e and q⊥, e).",0
+3401,"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 × 10−4 M⊙ yr−1",0
+3402,their Fig. 5).,0
+3403,while short GRBs are consistent with null or negligible intrinsic spectral lag and are therefore an ideal tool to measure the LIV effect,3
+3404,also denoted $X^N_{2m}$ in,0
+3405,"Similarly, stronger-than-expected 21-cm signals can arise if the cosmic radio background has contributions other than the CMB",3
+3406,"The existence of MPs in Pal 13 supports the statement that this phenomenon is not unique in Galactic GCs formed in situ (e.g.,",5
+3407,"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.",0
+3408,After convolving our models with a 10″ FWHM Gaussian kernel to simulate the data analysis presented in Lefèvre et al. (2014) and following the,2
+3409,"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 μm intensity for the 21 starless cores of Lefèvre 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.",2
+3410,Inspired by the new observations of this GW event at 3.3 yr after the initial merger,3
+3411,"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.",3
+3412,We primarily used the OGLE catalogues for RR Lyrae stars,2
+3413,but we also used RR Lyrae stars by CTRS,2
+3414,These cross-matches returned a list of 88 578 known RR Lyrae stars in our sample of 140 784 stars.,2
+3415,"This up-gradient transport into the jet can result from Rossby waves, coupled Rossby–Kelvin waves, mixed Rossby–gravity waves, wave–jet resonance, barotropic instability, or baroclinic instability",0
+3416,This property enables the creation of steep phase ramps that efficiently diffract light into a single order without scattering,2
+3417,"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",0
+3418,or protostellar outflows,0
+3419,Despite this only six radio pulsars have been discovered within half a degree of Sgr A*,0
+3420,"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",5
+3421,Many near-infrared observations have revealed the same feature on the blue wing part of the CO absorption feature,5
+3422,which was suggested as an absorption feature of XCN ice.,0
+3423,According to,2
+3424,", the Poisson noise is 200 e− for a typical detector with a gain of a few e− ADU−1 and the flat illumination level is of 20 000 ADU pixel−1 = 40 000 e− pixel−1. Thus, a typical photometric aperture with a radius of 3 pixels contributes ∼1 mmag photon noise.",2
+3425,This complex environment is multiphase and has been observed in numerous surveys,0
+3426,at low redshift.,0
+3427,"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",2
+3428,"For a collision at a velocity ∼108 cm s−1, which is a typical velocity scale for young SNR shocks, the cross-section is ∼10−13 cm2, giving a reaction rate ∼10−5 cm3 s−1 (e.g.",2
+3429,"Thus, if the density is ∼106 cm−3, the collisional depopulation becomes important.",2
+3430,"In OMC-1, the low- and high-velocity outflows from BN/KL plunge into the ambient molecular cloud",2
+3431,producing hot (from Tk ≃ 200–2000 K) and dense (up to n(H2) ≃ 106–107 cm−3) post-shocked gas in H2 Peaks 1 and 2,2
+3432,"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",0
+3433,"As already noted, the companions are generally significantly fainter than the exploding star, although this is frequently not the case for stripped SN progenitors – 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",0
+3434,"In order to estimate a temperature for the dust, we have fitted a modified blackbody to the available photometry at wavelengths longer than 10 µm (AKARI, WISE, IRAS, Herschel)3 and the new ALMA photometry using the emcee Affine Invariant Markov chain Monte Carlo Ensemble sampler implementation",2
+3435,Graham (2001) analysed a sample of 86 face-on disc-dominated galaxies previously selected by,2
+3436,"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.",2
+3437,"The disk of an AGN provides a natural environment for stars and compact objects to accrete materials and to migrate within it (e.g.,",0
+3438,"Recently,",5
+3439,claimed that the mass of XTE J1859+226 is perhaps in between 6.58 and 8.84 M⊙ which is similar to the prediction of Shaposhnikov & Titarchuk (2009),5
+3440,although the lower mass limit is estimated as 5.4 M⊙ by Corral-Santana et al. (2011).,6
+3441,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,2
+3442,"(18)\begin{equation} f_{\rm esc}^{\rm HO06} = 1/{\rm cosh}(\!\sqrt{2 N_{\cl}\epsilon}), \label{eq:fescHO06} \end{equation}fescHO06=1/cosh(2Nclϵ),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) ϵ, we adopted a value of c1(1−e− τd,cl) with c1 = 1.6 [c1 = 0.06] to match the NHI,cl = 1022 cm-2 data points for τd,cl = 10-4 [τd,cl = 1].",2
+3443,Early studies concentrated on measurements of higher order correlation hierarchy in the angular space due to small survey size,0
+3444,"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.",0
+3445,Since then they have been extensively employed to study the morphology of the large-scale structure of the universe and the cosmic web,0
+3446,"Next, we adopt the position of 3FGL J1640.4-4634c provisionally provided by the 3FGL catalog",2
+3447,"This is illustrated in Fig. 5, where thick blue and red data points show mild high-energy excesses of the electron spectra derived by",2
+3448,"Kerszberg et al. (2017), Kerszberg (2017) over broken power-law models derived from the fits to lower energy data.",2
+3449,"Other global 21-cm experiments, including the Large-Aperture Experiment to Detect the Dark Ages",0
+3450,"provide upper limits on the signal from Cosmic Dawn and the Epoch of Reionization (EoR), ruling out some extreme astrophysical scenarios.",0
+3451,"It was soon realized that these frequencies are probably related to oscillations of the neutron star, and several groups tried to identify them as",0
+3452,Alfvén oscillations,0
+3453,The data were manually calibrated by the EA ARC node using the Common Astronomy Software Applications (CASA) of the version 5.1.1,2
+3454,Recent measurements of the LMC abundances based on the X-ray spectral analysis of SNRs,6
+3455,"suggest ∼50% lower LMC abundance values for O, Ne, Mg, and Fe than the previously estimated values",6
+3456,"Our derived shock parameters are consistent (within statistical uncertainties), assuming either set of these LMC abundances in tbnew.",6
+3457,"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",0
+3458,"stellar mass, and star formation rate",0
+3459,In this scenario SMBHs have to begin growing even earlier than the very first stars are assumed to have appeared (see discussion in,2
+3460,"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.",0
+3461,disrupting morphologies (e.g.,0
+3462,"A whole host of ions, atoms, and molecules have been detected through a variety of, often complementary, techniques,",0
+3463,and high resolution spectroscopic techniques (e.g.,0
+3464,"To date, several candidate jet–ISM interaction sites have been identified;",0
+3465,XTE J1550–564,0
+3466,"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).",0
+3467,"However, the depth of the feature is ΔT21 ∼ 0.5 K ($99{{\ \rm per\ cent}}$ confidence level), which is two to three times stronger and considerably wider (Δν ∼ 19 MHz) than that predicted by the most optimistic astrophysical models (e.g.",6
+3468,"Vázquez-Semadeni, González-Samaniego & Colín (2017) have recently shown that the simulations of Colín et al. (2013) in fact produce stellar age histograms highly resemblant of the observed ones",5
+3469,"Moreover, in massive galaxies, the role of AGNs in influencing galaxy evolution and quenching SF is supported by several observations",0
+3470,"On the other side, we have the tidal (gravitational) mechanisms occurring",0
+3471,or among neighbour galaxies,0
+3472,"In fact, homologous jets, continuing for hours at a time, have been commonly observed (e.g.,",0
+3473,More evolved disks do not show a degree of linear polarization larger than 0.5%,0
+3474,and a similar phenomenon has also been observed in the case of,5
+3475,CB 3,5
+3476,Since cool core clusters have short radiative cooling time-scales on the order of 108 yr in their centres (e.g.,2
+3477,starbursts are expected to be common at the centre of such clusters.,2
+3478,"Comparison of 1D marginal posterior distributions over the parameters S8 ≡ σ8(Ωm/0.3)0.5, σ8 and Ωm, from DES Y3 data as well as other experiments, and consistency tests for this work (in blue).",1
+3479,"Constraints from other weak lensing surveys, namely HSC Y1",1
+3480,are shown in grey,1
+3481,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 Σ(Hα) of approximately a few 10−18 erg s−1 cm−2 arcsec−2,0
+3482,while only a handful of galaxies have extended cold or hot gaseous tails,0
+3483,Since relxillDCp considers the thermal Comptonization model nthComp,2
+3484,"as the irradiating (primary) continuum, we replaced the zpowerlw continuum with nthComp.",2
+3485,"For this paper, κ is taken to be equal to 1, in agreement with numerical simulations of decaying turbulence",2
+3486,"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. Γjet ≲ 2. More strictly, the bulk Lorentz factor is restricted to be as Γjet ≲ 1.67",0
+3487,and Γjet ≲ 1.2,0
+3488,A similar effect is also found in measurements of the propagation velocity of travelling waves,0
+3489,"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",0
+3490,For solar-type stars k2 ∼ 0.035,2
+3491,This kind of weak anti-correlation between the activity cycle and the meridional flow has been found in solar observations,5
+3492,"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",3
+3493,"and energy propagation to the upper atmospheric layers (see, e.g.",3
+3494,that cannot be addressed otherwise from an observational point of view.,3
+3495,"In particular, the analysis of CMB data, most notably from the Wilkinson Microwave Anisotropy Probe",0
+3496,and Planck,0
+3497,"experiments, has not yet provided conclusive evidence for the hypothesis of Cosmological Isotropy",0
+3498,"Several works have pointed out that AGN activity coincides with a recent starburst, with the AGN having significant accretion events at least ∼200 Myr after the starburst has occurred",0
+3499,giving the neutral material time to propagate out to the impact parameters probed by COS-AGN,0
+3500,"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",5
+3501,"Higher angular resolution observations of the (3, 3) NH3 absorption line (0\hbox{$\farcs$}.̋3 beamsize) showed signatures of rotation within 2000 AU based on a position-velocity (pv) diagram",0
+3502,"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",0
+3503,Here we adopted an intermediate value between the solar and supersolar G/Ds used in,2
+3504,and we increased the error bars of these points to include both the solar and supersolar confidence estimates.,2
+3505,Although hotspots located at the foot of accretion streams can affect RV measurements mimicking the signal of an orbiting body,2
+3506,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.,2
+3507,"As for the density profile, simulations of the FHSC stage show a flat inner region, corresponding to the FHSC structure and extending up to ∼10 au",1
+3508,Some of the recent observations and studies,0
+3509,indicate that the CGM can account for a good fraction of the baryons in these galaxies.,0
+3510,"From power spectrum analysis, significant periodicities ranging from about 1.4 to 10 yr were found in PSR B1540−06, PSR B1642−03, PSR B1818−04, PSR B1826−17, PSR B1828−11, and PSR B2148+63",2
+3511,"In all cases, we consider a solar metallicity for the main SF episode and, according to the results of",2
+3512,a subsolar metallicity (Z = 0.004) for the later one.,2
+3513,"If the carbene is formed in its first excited singlet state (a1A1), the insertion is barrierless",2
+3514,"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.,",0
+3515,As shown by comparisons to dark moon observations only particle events are recorded in the stow position,0
+3516,The cool molecular envelope exhibits ice and dust absorption bands,0
+3517,Sagittarius A* (Sgr A*) is inferred to be accreting at a rate of 10−3 to $10^{-2}\ \dot{M}_{\rm B}$ (e.g.,2
+3518,"In more detail, the existence of a “blue” and possibly also a “purple” 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 “red” kilonova1",0
+3519,"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",1
+3520,which is one of the commonly used methods of mass determination in galaxy clusters (see e.g.,0
+3521,"This new estimate is consistent with the ratio expected between the aGg′ and gGg′ conformers under thermal equilibrium conditions at 300 K, the excitation temperature of glycolaldehyde derived in IRAS 16293",5
+3522,see equations 3 in,0
+3523,these are based on the vector eccentricity and the vector inclination.,0
+3524,"The initial condition is the Orszag–Tang vortex (OTV) (e.g.,",2
+3525,"also, ‘convergence’ 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 → ∞ faster than a negative power of the time with an exponent which is a function of n, m, and p (e.g. −1/3 for n = 2 and m = 3 in the L2 norm; see details in the book by",0
+3526,"The CO photodesorption yield reaches its highest value when this ice is deposited at low temperatures (down to 7 K, the lowest temperature studied experimentally) and decreases gradually at higher deposition temperatures",0
+3527,The explanation for this phenomenon motivated further research.,3
+3528,"On the other hand, if the torus is made of a collection of clouds, each cloud is heated to ∼300 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",6
+3529,The first three LoTSS Deep Fields are the European Large-Area ISO Survey-North 1 (ELAIS-N1,0
+3530,"Lockman Hole, and Boötes",0
+3531,"these were chosen to have extensive multi-wavelength coverage from past and ongoing deep, wide-area surveys sampling the X-ray",0
+3532,and to infrared (IR; e.g.,0
+3533,wavelengths,0
+3534,"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.",0
+3535,This proved to be a useful distinction and an excellent predictor of several trends,1
+3536,"but recent results, including our present and previous analysis",1
+3537,show that the demarcation between starburst and main-sequence galaxies is more blurred that we previously considered.,1
+3538,"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.",0
+3539,"For example, it was observed that a single emission line at around 14 keV can fit two features around 10 and 20 keV for",2
+3540,Her X-1,2
+3541,"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.",1
+3542,"In this context ‘scale-free’ 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.",0
+3543,Extreme geomagnetic storms can cause widespread interference and damage to technological systems,0
+3544,"and then lead to significant economic loss (e.g.,",0
+3545,"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 ∼ 0.02–0.04, apart from the Crab PWN which has an Fopt/Fx ∼ 2",6
+3546,This is also the case for the PSR J1124−5916 PWN,1
+3547,Also the dependence of the IMF on the SFR is nowadays observationally well established,0
+3548,but see also a noticeable exception in,6
+3549,"An interesting implication is that, if BHs settle into the disk, they interact dynamically and form BH–BH binaries efficiently, and frequent dynamical interactions and gas effects drive the BHs to merger, producing gravitational waves (GWs) detectable by LIGO, VIRGO, and KAGRA",0
+3550,"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.,",1
+3551,or could also mean that simulations still cannot fully capture the true rotational influence on turbulent convection in the Sun.,1
+3552,"But there is no well-resolved system that matches the theoretical expectations (see, e.g.,",3
+3553,"Nevertheless, it still faces numerous challenges on galaxy scales. Among these, the most important ones are",3
+3554,"for dwarf galaxies, the tightness of the baryonic Tully–Fisher relation",3
+3555,The comparison sample is compiled from the literature up to z ∼ 3,2
+3556,"There have been searches for a periodic signal in the prompt emission of GRBs with a number of instruments with no success, for example:",0
+3557,and Burst Alert Telescope (BAT) GRBs,0
+3558,"At certain geocentric velocities the cometary [O i] 6300 Å 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)",1
+3559,"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.",3
+3560,"Here, Ai,j are the entropic functions of the particles",2
+3561,"A cold-phase of the CGM at ≈104 K has also been observed, but its origins are less clear",3
+3562,It was the first source identified as a hot corino,0
+3563,"based on the detection of Complex Organic Molecules (COMs) in the source, which was later supported by follow-up studies",0
+3564,Turbulence on scales less than the scale height of the warm–cold ISM likely originates primarily due to the feedback from young stars,0
+3565,"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",2
+3566,As reported in,0
+3567,", 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.",0
+3568,"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 “view” of Rosetta at 67P, with the larger lobe blocking out the neck and head.",3
+3569,"According to the time-lag analysis,",0
+3570,"found that the disc thermal emission (∼0.3–0.7 keV, soft band) leads the power-law variations (∼0.7–1.5 keV, hard band) on long timescales (> 1s).",0
+3571,The propeller regime has been investigated both analytically,0
+3572,"In this paper, we adopt Mpi = 20 M⊕ and Mpf = 10 M⊕ nominally (close to the standard model adopted in",5
+3573,Negative radial metallicity gradients have been widely observed in the low-redshift galaxy population (e.g.,0
+3574,Gravitational interactions in the perturbed disc drive turbulence causing the disc to self-regulate in a marginally stable state with Q ≲ 1,0
+3575,that can last for more than a Gyr so long as the accretion is not interrupted.,0
+3576,"Apart from cosmological simulations, dedicated zoom-in simulations",0
+3577,have revealed that dry mergers that dominate the passive evolution of ETGs below z ≈ 2 could make the total density profile shallower than isothermal,0
+3578,We calculate the GW amplitudes A(f) of NS–WD binaries using the phenomenological (PhenomA) waveform model in the Fourier domain,2
+3579,"According to the review of the leptonic model (see, e.g.,",2
+3580,"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.",2
+3581,and a comparison with the other EoSs of the BSk family,7
+3582,and the RMF family,7
+3583,shall be left for future study.,7
+3584,Intermittency is related to the scale-dependent shape of the probability distribution function of the increments Δϕ,0
+3585,"This, additionally, implies the existence of nonvanishing odd moments.",0
+3586,"whereas radio relics are apparently associated with localized, post-merger shock-fronts",0
+3587,and the Coma cluster,0
+3588,an apparent link is seen between radio galaxies and radio relics.,0
+3589,Although,6
+3590,"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.",6
+3591,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,1
+3592,Although period-folding improves performance,1
+3593,"Becker et al. (2020)’s time-space RNN does not require the period to be calculated, and is thus less computationally expensive in terms of preprocessing.",1
+3594,"This representative value for our AGN is in line but not as low as previous work targeting extremely powerful sources (e.g., Mgas, mol/M*  0.05 in",1
+3595,"As a result, when the power spectrum is observed as a function of (k∥, k⊥), the foreground emission remains concentrated near the low k∥, inside the ‘wedge’",2
+3596,Another problem is the use of time-dependent mixing-length formalisms,0
+3597,"to account for modal surface effects (e.g.,",0
+3598,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,0
+3599,"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.,",0
+3600,"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",1
+3601,"In addition, we argue that the Galaxy is the azimuthally asymmetric spiral system (cf.",6
+3602,"The charge transfer inefficiency (CTE) correction for the ACS data was performed by the pipeline, whereas CTE losses in WFC3/UVIS",2
+3603,were treated manually using the tools supplied by STScI.,2
+3604,"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.,",1
+3605,so we should not expect complete agreement.,1
+3606,"Here, we use the new formalism presented in",2
+3607,"who showed that the Newtonian potential is exactly reproduced by using an intermediate scalar function ℋ, namely \hbox{$\Phi = \partial_{xy}^2 {\cal H}$}Φ=∂xy2ℋ. 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}ℋ(x,y,z)=−G$Ω′ρ(x′,y′,z′)κxy(X,Y,Z)dx′dy′dz′,with X = x−x′, Y = y−y′ and Z = z−z′.",2
+3608,"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",0
+3609,"Indeed, other studies confirm that abiotic buildup of ozone is possible",0
+3610,"however, detectable levels are unlikely if liquid water is abundant, as e.g. rainout of oxidized species would keep atmospheric O2 and O3 low",0
+3611,", unless the CO2 concentration is high and both H2 and CH4 emissions are low",0
+3612,"For instance,",0
+3613,and RFs are associated with energy conversion from electromagnetic fields to particles,0
+3614,"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",2
+3615,"Even modest changes in direction (e.g.,",0
+3616,have long been recognized as one way to produce significant changes in the flux and polarization,0
+3617,"Vacuum birefringence dramatically increases the linear polarization of the observed radiation, from a level of a few  per cent up to even ∼100 per cent, depending on the viewing geometry and the surface emission mechanism",0
+3618,"In addition,",0
+3619,recalled several issues that should be taken into account when considering the Si iv/O iv density diagnostic. The main ones were: (1) O iv and Si iv ions are formed at quite different temperatures in equilibrium and hence a change in the O iv/Si iv 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 iv/O iv relative intensities by a factor of roughly three to four.,0
+3620,So-called Type-C low-frequency QPOs,0
+3621,"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",0
+3622,This latter assumption does not perfectly reflect spacecraft observations of the same,1
+3623,", but leads to relatively simple, tractable expressions for the parallel and perpendicular MFPs.",1
+3624,"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",0
+3625,"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",5
+3626,"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 ϕ is the phase of the wave",2
+3627,", annexure B therein",2
+3628,"Indeed, Terzan 5 hosts the largest population of MSPs among all Galactic GCs",3
+3629,"Still, in four dimensions, hairy BHs have been described in different theories of gravity, such as Einstein–Yang–Mills",0
+3630,Originally it was proposed that due to mutual gravitational interactions that all black holes would have been ejected from globular clusters,0
+3631,These differences,0
+3632,do not seem to be related to unaccounted variation in the CO-to-H2 conversion factor,0
+3633,but has been interpreted as evidence that SiO disappears from the gas phase at high densities to be incorporated into dust grains,1
+3634,This method has been intensively implemented with updated observations,0
+3635,To limit the ISGRI calibration uncertainties,2
+3636,This is within the range of the equipartition magnetic fields of 17 HFP radio sources,5
+3637,and 5 HFPs at 0.084   z   1.887 (18–160 mG,5
+3638,These values are in very good agreement with those measured from the average long-term Swift/BAT (Burst Alert Telescope) spectrum,5
+3639,"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",0
+3640,that die as electron-capture supernovae,0
+3641,"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–satellite line. They produce E12 = (V1−V2)/3.5 and E34 = (V3−V4)/3.5, which are then rotated into the spacecraft coordinate system to produce EX and EY. The direction, X, is perpendicular to the Sun–spacecraft 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",2
+3642,No Compton reflection hump has been detected with,1
+3643,or NuSTAR,1
+3644,despite the presence of a complex Fe Kα line.,1
+3645,"The initial dispersion of the LUV − LX relation is relatively large (δ ∼ 0.35−0.4,",1
+3646,"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.",1
+3647,We use an α approximation for the turbulent viscosity,2
+3648,"when the (rφ) component of the stress tensor trφ is written as (5)\begin{equation} t_{r\phi}=\alpha\, P, \label{trphi} \end{equation}trφ=α P,where the phenomenological non-dimensional parameter α ≤ 1.",2
+3649,"Early on, the MUSE Guaranteed Time Observations (GTO) team established surveys including MUSE-QuBES",0
+3650,to relate gas traced by absorbers to galaxies.,0
+3651,"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",0
+3652,"These microlensing magnification estimates are calculated after subtracting the emission line flux ratios, which are little affected by microlensing (see, e.g.,",2
+3653,"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).",2
+3654,"Furthermore, well-defined large samples of white dwarfs are an extremely useful starting point for identifying rare white dwarf types like",3
+3655,or white dwarfs with dusty or gaseous planetary debris discs,3
+3656,Observations have shown that the AGN fraction does increase with decreasing distance between two merging galaxies,0
+3657,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.,3
+3658,"Moreover, c-C3HD and c-C3D2 have been surveyed in a sample of low-mass prestellar and protostellar cores",0
+3659,"finding that the corresponding isotopic ratios are relatively uniform, within a factor of a few, and similar to those in L1544 and L483.",0
+3660,"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",6
+3661,for an explanation of the difference).,6
+3662,This results in different spatial distributions in which tiny grains are present at the disk surfaces,1
+3663,and in the cavity or gaps from which the pebbles are missing (e.g.,1
+3664,We expect the centroid of a blended source to be determined with poor accuracy (see e.g.,2
+3665,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.,2
+3666,"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",0
+3667,"Using their spectroscopic catalog with radial velocities measured with an external accuracy of 7–10 km s-1 and applying photometric parallax relations, the SDSS teams have traced K–M 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",0
+3668,as well as on the luminosity and mass functions of low-mass dwarfs in the Galactic disk,0
+3669,"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",1
+3670,"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",0
+3671,"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",0
+3672,detected INV during three nights out of three using C- and F-tests (a total monitoring duration of 16 h in the R-band).,1
+3673,Fornasier et al. (2015) obtained results for the 67P nucleus surface reflectivity applying a HG-type phase function,2
+3674,with a best-fitting G of −0.13. Fig. 5 shows the phase angle-corrected afρ values of 67P for the various phase function solutions.,2
+3675,Asymmetric inflow reconnection has also been investigated in,0
+3676,laboratory experiments,0
+3677,"The LMC star cluster formation history is believed to be three-staged, including a period of rapid cluster star formation in the early universe (τ ≳ 10 Gyr), followed by a long quiescent period between ∼10 and ∼2–4 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",0
+3678,Hydrodynamic simulations using the code HYADES,2
+3679,"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 0.3−1 keV band.",0
+3680,The X-ray luminosity of GRBs is given by the energy input from the electromagnetic and gravitational waves into the surrounding medium,2
+3681,"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).",2
+3682,"For the three first cases, we assumed ISM[M/H](R⊙) = 0.0 to estimate Rbirth from the stellar metallicity. However,",6
+3683,"have their own zero point, defined as: [Fe/H] = −0.06 * Rg + 0.57, with a clear shift in the relation compared to the other ones assumed in this work.",6
+3684,Single-case studies reported some EIT waves covering a whole solar hemisphere,0
+3685,"For the Bernard-Salas et al. (2009),",2
+3686,"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 μm.",2
+3687,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,2
+3688,"The most rapid changes of surface temperature occur early,",0
+3689,"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",0
+3690,"For PN in O-rich AGB atmospheres, the disagreement between the observed abundances, (1–2) × 10−8",6
+3691,and the calculated maximum chemical equilibrium abundance is almost three orders of magnitude.,6
+3692,Compact starbursts containing hot O stars offer an alternative explanation for the relative intensities of LINER emission lines,1
+3693,", but have difficulty explaining the broad Balmer emission wings often seen in LINER spectra",1
+3694,", since this would require long-lived supernova remnants.",1
+3695,"The Hα 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 ±200 km s−1",1
+3696,as seen here in PTFO 8-8695.,1
+3697,L.A. Cosmic,2
+3698,was used to clear the image of cosmic rays to produce the final Hα and final R image.,2
+3699,"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",0
+3700,and in the X-ray band (see e.g.,0
+3701,"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.",0
+3702,Different column densities of para-H2CO only weakly affect derived kinetic temperatures (see Fig. 3 in,2
+3703,as long as all lines are optically thin.,2
+3704,The spectra of the AGNs to be compared are taken from those of the IR galaxies observed by Spitzer/IRS,2
+3705,"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),",3
+3706,"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",2
+3707,and continue to attract much attention in the quest for unraveling quantum effects such as the geometric phase (GP) in chemical reactions,0
+3708,"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",0
+3709,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),0
+3710,"Accounting for the ramp up of the driver and scaling the values, this corresponds to an energy injection rate of ≈5.6 × 1023 erg s−1 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 1023–1024 erg s−1 for bright points",5
+3711,A possible fix of this proposal is to introduce rapidly spinning magnetars born from binary neutron star (BNS) mergers,0
+3712,"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.",0
+3713,For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm−3 is assumed,2
+3714,"Generally, the spectrum hardens when the flux increases",0
+3715,but photon indices can saturate at higher fluxes,0
+3716,"It is not yet clear which process is the dominant source of the elements in the early Universe (see discussions by, e.g.,",3
+3717,"As a consequence, mergers are also expected to play a significant role in driving the evolution of galaxy properties, for example,",0
+3718,star formation in the host galaxy or by driving its morphological evolution (e.g.,0
+3719,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 – e.g.,3
+3720,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).,3
+3721,We have now access to the size evolution up to z ~ 10 from the deepest HST imaging data,0
+3722,There is a debate about the extent to which DIG affects measurements of gas-phase metallicity and its radial slope,3
+3723,as some observations indicate lower metallicity (up to 1 dex) in DIG compared to nearby H ii regions.,3
+3724,"For example, if G1.75-0.08 follows the line width–size relation in the central molecular zone, or CMZ, which for HCN is found to be σ ∝ R0.62",1
+3725,", the aforementioned HCN(1 – 0) line width would be expected to be only ~2.5 km s−1 on the ~0.1 pc scale, which is a typical inner width (FWHM) of filamentary molecular clouds",1
+3726,"In particular, classification by ML (e.g.,",7
+3727,can avoid time-consuming visual inspections and will be helpful for the visual classification of galaxy−galaxy interactions from the forthcoming large surveys.,7
+3728,We stress that our SOFIA/FORCAST images do not detect the outer polar rings seen in Spitzer IRAC images,6
+3729,"For the sake of simplicity, the specific heat capacity c was assumed constant, c = 560 J kg−1 K−1, and the regolith grain density obtained for C-type meteorites was used, ρ = 3.11 g cm−3 (both from",2
+3730,We collect the total radio flux density from literature,2
+3731,We estimate the fluxes Fx (see Table 1) of LHS and HIMS of the 1999 outburst of the source,2
+3732,"There are examples of merging clusters that show presence of X-ray–SZ offsets, such as",0
+3733,and Bullet cluster,0
+3734,For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm−3 is assumed,2
+3735,"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",1
+3736,Analogously to previous ANTARES searches,1
+3737,"MC simulations of the signal predicted by NeuCosmA were performed, while the respective background was estimated directly from off-source data collected by ANTARES.",1
+3738,"Following Rosdahl et al. (2018), we have calibrated the SN feedback in order to reproduce the high-redshift stellar mass–halo mass relation from abundance matching",2
+3739,"The same source was followed up and consistently localized at other wavelengths (e.g.,",0
+3740,"On the one hand, it is more energetically favorable for the system to populate new degrees of freedom, such as hyperons",1
+3741,in order to lower its Fermi energy (starting at about two times the saturation density).,1
+3742,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,0
+3743,May 1921,0
+3744,"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",2
+3745,"With ALMA and NOEMA, ground-based observations of the [C II] 158 μm line in high redshift galaxies have come into reach and such data are routinely used to infer SFRs",0
+3746,based upon validations of this relationship in the nearby Universe,0
+3747,A common interpretation of the MS is that the location of galaxies relative to the MS follows a different time evolution of SFR,0
+3748,Several studies have already measured the distance ratios (e.g.,0
+3749,"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.",6
+3750,The ESPRESSO DFS concept,0
+3751,"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.",0
+3752,"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",3
+3753,which requires sophisticated microphysics in terms of finite-temperature equations of state (EOS) satisfying recent observational constraints,3
+3754,"Indeed, the Hβ",2
+3755,"and Mg II lines seem to arise from the same part of the BLR in various quasars (e.g.,",2
+3756,and should both yield similar sizes; whereas the Fe II line is thought to arise from a larger part of the BLR,2
+3757,"Therefore, the combination of the two signals modelled as a single BLR emission could broaden our measurement and induce its slight bi-modality.",2
+3758,"In the solar wind, the evaluation of turbulence is well described by magnetohydrodynamic (MHD) theory",0
+3759,"and the turbulence transport throughout the heliosphere has been studied over the years (e.g.,",0
+3760,"As mentioned above, after its discovery in 2010, V2492 underwent a long-lasting period of strong activity with intermittent burst and fading events",0
+3761,and reached its maximum recorded brightness in 2017,0
+3762,"This equation, usually referred to as the Landau–Lifshitz (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",0
+3763,"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.,",0
+3764,"For some Cepheids (OGL0434, OGL0501, OGL0510, OGL0512, OGL0528, OGL0545, OGL0590, OGL0712, OGL0757, OGL0966, and OGL0992), we also included V-band light curves from the",2
+3765,and/or ASAS-SN survey,2
+3766,to increase the baseline coverage.,2
+3767,This model can naturally fit the observational positive relationships between αOX and λO as well as Γ and λO in RQAGNs,1
+3768,"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",1
+3769,"This crude selection of cluster member candidates is obviously prone to contamination by interlopers. So, we further refine it using the shifting gapper method",2
+3770,"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.",0
+3771,"The observed ratios of the infrared fine-structure ionic lines (Ne ii, Ar iii, and S iv;",2
+3772,indicate that at least eight O7.5V stars are necessary to account for the ionization of the region.,2
+3773,With the large number of newly discovered exoplanets expected in the next 10 years by ground-based surveys such as,0
+3774,as well as the ongoing Transiting Exoplanet Survey Satellite (TESS) space survey,0
+3775,a rapid characterization scheme of the interior structure of these planets will become increasingly necessary to further our understanding of planetary populations.,3
+3776,"To take the contribution of f–f and f–b radiations into account and estimate the corresponding spectra, we used the chianti package",2
+3777,"The Largest Linear Sizes (LLS) and radio powers of relics are correlated, as well as the integrated spectral index and the radio power",0
+3778,"Since the light curve inversion produced convex shape models only, then shadowing and self-heating effects inside global-scale concavities (see",6
+3779,) were not possible to model.,6
+3780,"Through the work of Švestka & Fritzová-Švestková (1974), Kahler et al. (1978, 1984)",0
+3781,(1982,0
+3782,"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.",0
+3783,"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–Cooper–Schrieffer superfluids, with 3PF2 and 1S0 Cooper pairing, respectively",2
+3784,"where Φmad ≈ 50Φmad,1.7 is the saturated magnetic flux",2