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Whilst a reasonable harmonic fit to the ESPaDOnS data can be achieved using this period, it does not produce an acceptable phasing of all available 〈 B z 〉 measurements. Figure 1. Photometric (top) and magnetic 〈 B z 〉 (bottom) measurements, phased with periods determined from (left to right) K2 photometry, all 〈 B z 〉... | {
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comparison once the angular positions of the satellites are randomized around this point. From this tensor we compute its eigenvalues, λ 1 > λ 2 > λ 3, and corresponding eigenvectors,,,. We define the size of the three ellipsoidal axis as a = λ 1, b = λ 2, and c = λ 3. We also define as the vector perpendicular to the ... | {
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ACKNOWLEDGEMENTS The authors thank an anonymous reviewer for comments and suggestions that strengthened our manuscript. NWCL gratefully acknowledges support from the American Museum of Natural History and the Richard Guilder Graduate School, specifically the Kalbfleisch Fellowship Program, as well as support from a Nat... | {
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BDM gratefully acknowledges support from NASA Fermi grant NNX14AQ68G, NSF grant AST-1410950, and the Alfred P. Sloan Foundation. We thank the anonymous reviewer for several helpful suggestions and for emphasizing the applicability of our results to Type IIn supernovae. | {
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ACKNOWLEDGEMENTS We thank Dougal Mackey, Adrian Price-Whelan, David Hogg, Gurtina Besla, David Schiminovich, Alis Deason, and Sergey Koposov for illuminating discussions. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme ... | {
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I thank Duncan Galloway, Zac Johnston, and Hendrik Schatz for useful discussions, and acknowledge the instructive tutorials from Ed Brown, Andrew Cumming, and Rob Farmer located on the MESA Marketplace (http://cococubed.asu.edu/mesa_market/) that helped at the beginning stages of this work. Relevant MESA inputs for thi... | {
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Lasota (2007) have updated this work, for a sample of ten CVs. The importance of this test was revived by Schreiber Gänsicke (2002), who pointed out that the HST FGS parallax distance of SS Cyg, the archetypal dwarf nova, led to a revised mass transfer rate that placed this outbursting system in the stable region of th... | {
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an antenna with cos 2 beam would have a maximum temperature at the LST when the Galactic center is at zenith. This also corresponds to the spectrum having the largest rms residual among the various mock spectra considered here. For various large-area samplings of the sky, we have thus demonstrated that the foreground c... | {
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origin. Our findings from this Section for the radial metallicity distribution of red and blue GCs in massive ETGs are summarized in a schematic way in Fig. 2. This representative diagram shows the same radial metallicity gradient for the red (metal-rich) GCs and the blue (metal-poor) GCs, only offset by 1 dex in metal... | {
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of the CSM density profile and the forward shock evolution together determine the temporal behavior of the optically thin radio flux density. For s = 0 and, the flux density rises with time as once, the flux density evolution steepens to (visible as a kink in the model light curve of Figure 1 with cm −3 around 100 days... | {
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We first thank M.S. Ruderman for helpful comments. A.H. thanks the School of Mathematics and Statistics, University of Sheffield (UK) for the support received. R.E. is thankful to the NSF, Hungary (OTKA, Ref. No. K83133) and is grateful to STFC (UK) for the awarded Consolidated Grant, and, The Royal Society for the sup... | {
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where and are two cylindrical coordinates; is the axial ratio, is a structure parameter, and is a function of, such that becomes the density at radius, which defines a volume containing half of the total mass of the component (for details, see Tamm et al. 2012 ). The gravitational potential derivative of a component, n... | {
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version of the full table is available. Table 3 The Spectral Parameters Associated with the H β Emission Line Note. Column information is as follows: Column [1]: 4FGL name; Column [2]: redshift; Column [3]: log-scale continuum luminosity at 5100 Å; Column [4]: FWHM of H β line, in km s −1; and Column [5]: log-scale H β... | {
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ACKNOWLEDGEMENTS It is a pleasure to thank Frdric Arenou for helpful comments. HL and JB received support from the Natural Sciences and Engineering Research Council of Canada (NSERC; funding reference number RGPIN-2015-05235) and from an Ontario Early Researcher Award (ER16-12-061). JB also received partial support fro... | {
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identified toward these positions. Column densities of this species are presented in Table 3. Figure 5. Detected transitions of CH 3 NHCHO in the spectrum toward position MM1-nmf. The observed spectrum is plotted in black, with the synthetic spectrum overplotted in blue and the rest-frequency center of the transition i... | {
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core. Figure 12 shows that such a quiescent gas environment barely affects the line ratios, as the difference in the line ratios calculated at the turbulence 0 and 150 km s −1 is very small. Figure 12. Line intensity ratio relative to w vs. log of hydrogen column density. Solid: no turbulence. Dashed: turbulence 150 km... | {
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This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 526555. These observations are associated with program #13364. R.C. acknowled... | {
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We are grateful to Francisco Prada, Risa Wechsler, Chiaki Hikage, and Surhud More for useful discussions. We acknowledge Yu Lu and Andrew Benson for useful discussions related to SAMs. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. Numerical computations... | {
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We are indebted to Jimmy Irwin, Matthieu Roman, Jean-Baptiste Melin, Adam Mantz, Nabila Aghanim, Maxim Markevich, Erwin Lau and Daisuke Nagai for valuable comments. AM gratefully acknowledges the hospitality of the Harvard-Smithsonian Center for Astrophysics and of the NASA's Goddard Space Flight Center. We acknowledge... | {
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This work was supported by INFN and ASI under ASI-INFN Agreement No.2014-037-R.0. M.S.P. and E.E.V. acknowledge partial financial support from the the South African National Research Foundation (NRF) under their Research Cooperation Programme. E.E.V. thanks the Space Science Division of the South African Space Agency (... | {
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shells, with secondary typical scales as small as (0.5–1) × 10 9 cm. The slope of the VSH power spectra stays consistent over time regardless of the presence or absence of rotation. In all cases we find nearly circular shapes for the characteristic convective elements. In terms of the 2D convective flow properties, our... | {
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drops (to 30%) in the lowest redshift bin. This decline may not be reliable for two reasons. First, the size of the star-forming sample at 0.5 z 1.0 is very small (only 10 objects), and therefore the sample proportions are not statistically significant. Second, the H -band images for the low- z objects are missing the ... | {
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This material is based upon work supported by the National Science Foundation under grant No. AST-1109683. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation Based on observations (G... | {
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from stellar activity). The likelihood function is given by where i indexes the observations acquired with the I th instrument, is the nominal uncertainty of each RV measurement, and s I are the zero-point and extra noise parameters (also called jitter) of each instrument, and the Doppler signal from a companion on the... | {
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and planets with little Ly absorption but strong emission can be used to distinguish between these two classes of thermospheres. Based on the predicted strong absorption signals, WASP-80 b and GJ 3470 b are the most promising targets among our sample in the search for yet undetected escaping atmospheres. Appendix A: Ca... | {
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conditions requires equilibrium total pressure balance across each interface. This demands that the total (gas plus magnetic) pressure is constant:where μ is the permeability of free space. The sound speed in each region can be expressed as for. Here, γ is the adiabatic index, which is uniform across every domain, unde... | {
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Swift Observatory short GRBs suggests that of those with an X-ray afterglow, >30% have evidence for additional energy input at later times, most commonly in the form of a long-lived plateau, persisting at bright levels for hundreds to thousands of seconds (with the majority at the shorter end), or in the form of X-ray ... | {
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We thank Ralf-Dieter Scholz for constructive conversations during the preparation stage and the anonymous referee for indicating revisions that have improved our analysis and results. We also thank the Cambridge Astronomy Survey Unit (CASU) and the Wide Field Astronomy Unit (WFAU) in Edinburgh for providing calibrated ... | {
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would either require a larger sample of observed dwarf galaxies with smaller error bars and systematic errors of (a difficult prospect) or obtaining spatially resolved rotation curves for 400 pc (within the half-light radii) in small dwarfs, where Fig. 9 shows that CDM/WDM and SIDM/SIWDM could be differentiated. While ... | {
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all but one observation the exposure time was particularly low (i.e. 0.5–1 ks). We estimated the Bayesian 95 per cent upper limit (Kraft et al. (1991) to the source count rate from the observation with the longer exposure (4.2 ks, n. 4, obs ID 00087498001). It was equal to 0.0025 count s −1. Using WebPIMMS, it converts... | {
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component to the width. Dynamical studies of galaxies typically use Newton’s gravity. However, it has been argued that once galactic masses are considered, relativistic effects arising from large masses (rather than large velocities) may become important (Deur 2009, 2017, 2019 ). Their physical origin is that in genera... | {
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t b to be 23.0. Figure 3. Multi-band light-curve fitting of SN 2013dy using Equation (1) for estimating t 0. The value of is fixed to be 1.90 and t b is fixed to be 23.0 during the fitting procedure. Diamond-shaped data points are included in the fitting, while cross-shaped ones are excluded. After applying the t 0 fit... | {
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The project was partially supported by National Science Centre, Poland, grant no. 2017/26/A/ST9/00756 (Maestro 9). V.K. acknowledges Czech Science Foundation no. 17-16287S. | {
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ACKNOWLEDGEMENTS This work is based upon observations obtained with the Georgia State University (GSU) Center for High Angular Resolution Astronomy (CHARA) Array at Mount Wilson Observatory, and the University of Hawai‘i 2.2-m telescope on Maunakea. The authors wish to recognize and acknowledge the very significant cul... | {
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This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ); data from the Two Micron All Sky Survey, which is a joint project of the Univer... | {
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sample of SNe included in this data release, our adopted classifications and dates of peak brightness (if available), and the values we used to perform redshift and dust-reddening corrections. Table 3 provides a description of the spectra included in our sample. Our research group utilizes a database of observations an... | {
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Acknowledgements The authors would like to thank the referee Francisco-Shu Kitaura and Stefan Gottlöber for providing comments that helped clarified the paper as well as Sergey Pilipenko for very useful discussions. JS acknowledges support from the Astronomy ESFRI and Research Infrastructure Cluster ASTERICS project, f... | {
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in their targets. Hence, we can conclude that in stars belonging to the transitional branch, the cycle length and the rotation period are uncorrelated. 5.2. Relationship between <italic>P</italic><inline-formula specific-use="simple-math"><sub>cyc</sub></inline-formula> and global stellar parameters We investigated how... | {
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x -axis in all the panels are the observation wavelength. The horizontal dashed line in the lower right panel shows where τ obs = 0.6. On the other hand, we caution that the DSHARP opacity adopted here is for compact spheres without porosity, and that the mixture of different compositions are handled with the Bruggeman... | {
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of the mean pitch angle remains similar over the whole energy range. However, evolution timescales and peak amplitudes change as expected. Next, the influence of the amplitude of the magnetic field of the plasma wave has been studied (Section 5 ). Again, simulation results and analytic predictions have been compared. S... | {
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outward flux is not conserved; its losses are a source for the photon angular momentum flux (Fig. 4 ). But in the model solution, the disc can only supply the flux from the relatively small amount of material within the ISCO, because just outside the ISCO the disc velocity is outward: it is not accreting! This cannot g... | {
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becomes more and more noisy toward higher frequencies and therefore the de-convolved power spectrum will be more and more uncertain toward higher and higher frequencies. Figure 15. (a) Simulated red-noise light curve (a = 2), containing 1000 data points with a sampling interval of one day (blue open circles), along wit... | {
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are quite discrepant (0.2 dex and 0.8 dex in our two stars, respectively). The 4215.5 Å line of the star S11–97 is affected by the CN molecular band in this region. Spectral synthesis taking into account the carbon abundance derived in the CH band led to an abundance that agrees better with the 4077.7 Å line. Yttrium. ... | {
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We are grateful to the referee, Brent Groves, for very constructive comments that helped to improve the manuscript. We thank Stefanie Komossa (MPIfR), Pavel Kroupa (University of Bonn), Thomas Krichbaum (MPIfR), Madeleine Yttergren (University of Cologne), Bozena Czerny (CFT PAN), Mary Loli Martinez-Aldama (CFT PAN), a... | {
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to account for the radiative recombination continuum and lines, a cutoff power-law model to account for the off-nuclear X-ray sources, in addition to the AGN-related emission, which is parametrized by two different MYTorus scattered and line components, in addition to the transmitted one described by the zeroth-order c... | {
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We are grateful to the STScI staff members for help in scheduling the intricate STIS observations. We thank the Paranal Observatory for conducting the UVES observations. Stony Brook’s continuing involvement in the SMARTS Consortium is made possible by generous support from the Provost of Stony Brook University. A.M. wa... | {
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component of Fe K α emission (log ξ = 0). A very similar result is reached by performing the same test on the 2014 mean EPIC-pn + NuSTAR spectrum (Δ χ 2 = 52), resulting in a modest reflection strength, R ∼ 0.6, while the photon index and Fe abundance remain unchanged: Γ ∼ 1.8; A Fe ∼ 3. The remaining key parameters in... | {
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other words, the PDFs are equal, because the system self-adjusts, not because glitch sizes are correlated with forward waiting times, as in the α ≪ α c (β) regime in Section 4. The explanation for the qualitative behaviour seen in Fig. 20 is the same as for Fig. 13. Figure 20. Correlation between sizes and forward/back... | {
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where the rise speed of the flux tube at a depth of 20 Mm is more than about 150 m s −1 produce preemergence diverging flows that are not consistent with the observations. Norton et al. (2017) found from HMI vector magnetograms that the surface magnetic flux increases during the emergence process more slowly than predi... | {
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This is well in the range of those measured for UCXBs. 4.2. The nature of the accretor Determining the nature of the compact object in an unclassified LMXB is often challenging. It can be assessed based either on a dynamical measurement of the mass of the compact object (via optical and near infrared spectroscopy durin... | {
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Acknowledgements I would like to thank the anonymous referee for valuable comments that improved this work. The author is supported by the Grants-in-Aid for Scientific Research of the Japan Society for the Promotion of Science (16H07413, 17H02864). | {
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velocity distribution of the gas within the velocity range from 495 to 495kms 1 (1kms 1 steps). The emission for one square degree centred on the SMCNOD exhibits two main peaks: 94 and 186kms 1 (which are shown in Figs 8 and 9, respectively). These velocities agree with the velocity field related to the MS at the SMCNO... | {
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ACKNOWLEDGEMENTS We are very grateful to the constructive and detailed review carried out by our anonymous referee. His/her numerous and wise comments have helped to significantly improve this paper. We thank Manuel Peimbert, Jairo Méndez-Abreu, Leticia Carigi, and Rolf Kudritzki for their useful comments. This paper i... | {
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the stepwise trajectories of incident CH ions within Titan’s upper atmosphere, all starting at an energy of 50 keV under normal incidence. Three different cases are indicated in the upper panel. For each incident ion, the portion of its trajectory between two consecutive collisions is displayed as the projection to the... | {
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The authors thank the referee for useful feedback which helped improve the final manuscript. This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, and with XMM-Newton, an ... | {
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This work was supported by the Basic Science Research (2013R1A1A2061842) program through the National Research Foundation of Korea (NRF). | {
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to a redshift. The statistical uncertainty associated with estimation of the source-frame masses is increased relative to that of the detector-frame masses owing to these dependencies. From the inferred posterior distribution of D L we compute redshift assuming a Planck 2015 ΛCDM cosmology with Hubble parameter H 0 = 6... | {
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But note that, as discussed above in Section 4.1, a direct comparison of our results with the models of Madau Haardt (2015 ), Khaire Srianand (2015 ), and Puchwein et al. (2019) is difficult because of the inhomogenous redshift-dependent integration limits adopted by these authors. Before considering the deficit in the... | {
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A typical peculiar velocity of 300 km s −1 equates to a proper motion of 6.3 μ as yr −1 at 10 Mpc. A sample of objects with proper motion uncertainty σ μ = 100 μ as yr −1 would require roughly 250 independent measurements to reach this proper motion value and roughly 2300 measurements to achieve 3 σ significance. Such ... | {
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We thank the anonymous referee for useful comments that helped us to improve the content of the paper. Based on observations made with the GTC, installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. We acknowledge support from Mexican CON... | {
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The authors thank the anonymous referee for the valuable comments. This work is partially supported by the National Basic Research Program (973 Program) of China under grant No. 2014CB845800. | {
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sensitivity of COSIMA to D and H, as described in the next section. 2.2 Instrument mass fractionation The effect of instrument mass fractionation (hereafter IMF) varies from element to element. For sulphur isotopes, the effect was too small to be measured with COSIMA. For oxygen isotopes, the effect was a few per cent.... | {
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The authors thank F. Halzen and A. Kheirandish for inspiring discussions that led to the section on neutrinos and G. Sigl for comments and feedback on the anisotropy of the arrival direction. Furthermore, the authors would like to thank the referee for their comments, which helped to clarify certain parts of this work.... | {
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We acknowledge the dedicated team behind the Kepler and K2 missions, without whom this work would not have been possible. We thank Daniel Huber and Benoit Mosser for useful comments on an earlier version of the paper. MNL acknowledges the support of The Danish Council for Independent Research | Natural Science (Grant D... | {
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This work has been financially supported by the Programme National Hautes Énergies (PNHE). The research leading to these results has received funding from the European Union Seventh Framework Program (FP7/2007-2013) under grant agreement No. 312789. The XMM-Newton project is an ESA Science Mission with instruments and ... | {
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given the age determined by Burgasser Mamajek (2017 ), the activity index described in Section 3.2, and the XUV fluxes that have been measured for the star (Bolmont et al. 2017; Bourrier et al. 2017; Wheatley et al. 2017 ). As noted earlier, the combination of these stellar attributes ensures that the TRAPPIST-1 planet... | {
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We thank Anvar Shukurov and Andrew Fletcher for valuable discussions and for helpful comments on an early draft of the manuscript, and David Moss for useful feedback on a later version. We are also grateful to Romeel Davé Oliver Gressel, Marita Krause, Jonathan Zwart, Nathan Deg, Prasun Dutta, Pallavi Bhat, and especia... | {
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flow direction forms with the grain’s velocity. The first part of Eq. (9) is the sum of radiation pressure force with the corpuscular pressure force split into its radial and transverse component. The latter part of Eq. (9) is the sum of the classical PR drag with the solar wind drag (Marzari Vanzani 1994 ). The adopte... | {
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We thank the referee for his/her accurate revision of the paper. B.B. acknowledges support from grant PRIN-INAF 2011 “Black hole growth and AGN feedback through the cosmic time”. M.B. acknowledges support from the FP7 Career Integration Grant “eEASy”: “supermasssive black holes through cosmic time: from current surveys... | {
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with 10% and 30% of binaries. In the latter ones, the peak density is around the (0,0) point. The binaries contribute to producing an elongated structure with a lower density (which increases with the binary fraction). In NGC 5272 3, the P1 sequence is relatively homogeneously populated with barely a very small overden... | {
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We are grateful to the staff of the IRAM facilities for the continuing excellent support of the large CO survey programs we have been analyzing in this paper. We also thank Albrecht Poglitsch and Matt Griffin, the PACS and SPIRE teams, and ESA for their excellent work on the Herschel instruments and mission. Finally, w... | {
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unavoidable; that is, first-principles numerical simulations that address this plasma regime with adequate separation between the ion and the electron scales may inevitably satisfy the conditions for nonlinear reconnection in turbulent eddies at sub-ion scales. Indeed, the biggest such simulation that we are familiar w... | {
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ACKNOWLEDGEMENTS We acknowledge support from the National Science Foundation through grant NSF-1108957. Support for Program numbers 12634 and 12575 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporate... | {
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are compatible with the literature data and achieve an accuracy similar or better with respect to the published measurements, which is a good test for this new instrument. The orbital fit is a minimum fitting, as described in Esposito et al. (2013), where all the four orbits are simultaneously taken into consideration,... | {
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can also be seen for physisorption at very low temperature (≤6 K), when the grain can be full of immobile atoms (Katz et al. 1999 ). A corollary of this behavior is that in case the accretion is very efficient, the dust grain could have a large abundance (∼10 −6) of a particular species depending upon its desorption en... | {
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strengths where Proca stresses can be significant. As emphasized above, the model considered in this report is not that of dark matter; it may, however, account for the conjectured dark-matter effects in astrophysical settings even beyond galactic rotation curves. It may also be tempting to explore the influence of the... | {
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channels, thus the results are extremely sensitive to the cross-section of the 27 Al( p, γ) 28 Si reaction: the comparison with the Al measured in E stars seems to require slightly lower rates, but the differences are not sufficiently significant to require a supplementary analysis on this argument. Sodium is the most ... | {
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ii regions are sensitive to time since the onset of the most recent burst, driving scatter from the average relationships. Henry et al. (2000) found that chemical evolution models differing only by their assumed star formation efficiencies (SFEs) produced a range of primary N/O plateaus. We illustrate the effect of var... | {
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The initial sample contains 777 spectroscopically unobserved SuperWASP/ ROSAT objects, with rotation periods ≲ 5 d, declinations >−20°, 8 V 15 and spectral-types FGK, corresponding to 0.7 V − K s 3.8. Targets in the first list are selected from the parent sample. A second list comprised of a subset of 160 targets whose... | {
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kinematics study of Clarkson et al. (2008 ). Awiphan et al. (2016) presented a more recent version of the model (variant BGM1307) and compared it with a large ensemble of 470 events from the MOA-2 survey (Sumi et al. 2013 ). Awiphan et al. (2016) concluded that there was a reasonable level of agreement once allowance w... | {
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ACKNOWLEDGEMENTS DFT and FCZ acknowledge support from the Spanish Ministry of Economy, Industry and Competitiveness grants PGC2018-095512-B-I00, SGR2017-1383, and AYA2017- 92402-EXP. DV acknowledges support from the Spanish Ministry of Economy, Industry and Competitiveness grants AYA2016-80289-P and AYA2017-82089-ERC (... | {
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"text": "DV",
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"text": "FCZ",
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S.M.H. acknowledges support from Ramanujan Fellowship SB/S2/RJN-73 and the Max-Planck Partner group program. S.M.H. is grateful to Martin Woodard, with whom many useful conversations were had, for helping resolve several technical issues. This research was supported in part by the International Centre for Theoretical S... | {
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This paper is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We thank the anonymous referee for helpful suggestions and Takashi Hattori for taking the data for us. This research was supported in part by the National Natural Science Foundation of Chi... | {
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efficiency of sublimation in this context, compared with the incidence of “dry rain” in the Earth’s atmosphere, can be ascribed to a combination of two factors: the relatively high silicate vapor mass fraction (typically X sil ∼ (0.3–1) X H when refluxing of pebble debris from the envelope begins to balance pebble accr... | {
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larger than the PSF FWHM (orange dashed line). The 3D half-light radii agree with the two observational methods for the bright galaxies. The sizes of faint galaxies show a steeper decline than the observational data, indicating potential systematic errors in observations below the instrumental resolution limits. We exa... | {
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{
"text": "F115... | [] |
a systemic velocity for the SNR. The broad range of ejecta space velocities and expansion indices (see Table 1) that we measure in our sample may be characteristic for an SNR transitioning from the free-expansion phase to the Sedov–Taylor phase. Measurements of the proper motion at various locations along Kepler’s forw... | {
"entities": {
"model": [
{
"text": "Sedov–Taylor phase.",
"start": 226,
"end": 245
},
{
"text": "Sedov–Taylor phase,",
"start": 460,
"end": 479
},
{
"text": "Sedov–Taylor dynamics.",
"start": 807,
"end": 829
... | [] |
at 10 to 20%. However, a much larger bias has been invoked to reconcile cosmological parameters derived from the cosmic microwave background and cluster counts (Planck Collaboration XX 2014 ), although the calibration of the bias by Planck team has been amply discussed (von der Linden 2014; Andreon 2014; Smith et al. 2... | {
"entities": {
"citation": [
{
"text": "(Planck Collaboration XX 2014",
"start": 160,
"end": 189
},
{
"text": "(von der Linden 2014",
"start": 270,
"end": 290
},
{
"text": "Andreon 2014",
"start": 292,
"end": 30... | [] |
et al. 1993; Steiner et al. 2010 ), which is determined by black hole mass and spin. In the case of non-rotating black holes, ISCO is equal to three times the Schwarzschild radius. Thus, from the average innermost radius of the disk, km, the black hole mass M BH is estimated to beThe expected distance–mass relation in ... | {
"entities": {
"citation": [
{
"text": "et al. 1993",
"start": 0,
"end": 11
},
{
"text": "Steiner et al. 2010",
"start": 13,
"end": 32
},
{
"text": "Shidatsu et al. 2019",
"start": 1141,
"end": 1161
},
... | [] |
described in Section 3.2, 417 out of 47,125 galaxies have AGN-like variability, for an overall variable AGN fraction of 0.9%. In Figure 3, we show the light-curve standard deviation versus the PTF R -band magnitude for the full sample. In general, the scatter about the median magnitude for a given light curve increases... | {
"entities": {
"survey": [
{
"text": "PTF",
"start": 193,
"end": 196
},
{
"text": "PTF",
"start": 646,
"end": 649
},
{
"text": "DECaLS Legacy Survey",
"start": 1221,
"end": 1241
},
{
"text": ... | [] |
This publication is based upon work supported by the National Science Foundation under grant AST-1108811. We thank Dan Kelson for helpful conversations, Anna Frebel for providing the MIKE spectrum of HD 122563, and Becky Canning and Jimmy for helpful conversations on the reduction of VLT spectra. We also thank the anon... | {
"entities": {
"organization": [
{
"text": "National Science Foundation",
"start": 53,
"end": 80
},
{
"text": "PAPDRJ.",
"start": 449,
"end": 456
},
{
"text": "CAPES",
"start": 530,
"end": 535
},
{
... | [] |
(top) WC/WN versus metallicity. Blue lines correspond to BPASS binary models and red dashed lines the single models. The black star shows the averaged WC/WN estimation for the Antennae. For comparison, we also show the values for the Magellanic Clouds and the Milky Way taken from Rosslowe Crowther (2015 ), shown with o... | {
"entities": {
"model": [
{
"text": "BPASS",
"start": 57,
"end": 62
},
{
"text": "Gaussian fitting",
"start": 2160,
"end": 2176
},
{
"text": "BPASS",
"start": 2951,
"end": 2956
}
],
"celestialobjec... | [] |
Larson core. We focus on niMHD calculations; iMHD calculations are discussed in Sect 5. Fig. 8 Visualisation of the disk structures. Top row: panels a) and b) show side and top views, respectively, of the disk density (orange), with the velocity vectors superimposed for. Panels c) and d) are the same side and top views... | {
"entities": {
"model": [
{
"text": "niMHD",
"start": 25,
"end": 30
},
{
"text": "iMHD",
"start": 45,
"end": 49
},
{
"text": "Keplerian",
"start": 884,
"end": 893
},
{
"text": "Keplerian",
... | [] |
software based on the analytical equation applied to spot modeling by Budding (1997), assuming circular spots. Fixed parameters were the effective wavelengths of the filters used, linear limb darkening coefficients (Howarth 2011) taking into account the stellar parameters, and the unspotted brightness in all bandpasses... | {
"entities": {
"citation": [
{
"text": "Budding (1997)",
"start": 70,
"end": 84
},
{
"text": "Howarth 2011",
"start": 216,
"end": 228
}
],
"mission": [
{
"text": "K2",
"start": 894,
"end": 896
}
... | [] |
We thank the referee for the constructive comments that helped to clarify the text. DH and BAG thank Marie Hrudkova and Raine Karjalainen for their help during the WHT observations, and Elyar Sedaghati and Boris Haeussler for their help during the VLT observations. FM thanks the Centre national d’études spatiales (CNES... | {
"entities": {
"person": [
{
"text": "DH",
"start": 84,
"end": 86
},
{
"text": "BAG",
"start": 91,
"end": 94
},
{
"text": "Marie Hrudkova",
"start": 101,
"end": 115
},
{
"text": "Raine Karjal... | [] |
ACKNOWLEDGEMENTS The authors are supported by the project grant 2014.0017 ‘IMPACT’ from the Knut and Alice Wallenberg Foundation. AJ was supported by the European Research Council under ERC Consolidator Grant agreement 724687-PLANETESYS, the Swedish Research Council (grant 2014-5775), and the Knut and Alice Wallenberg ... | {
"entities": {
"grant": [
{
"text": "2014.0017 ‘IMPACT’",
"start": 64,
"end": 82
},
{
"text": "Consolidator Grant agreement 724687-PLANETESYS,",
"start": 190,
"end": 237
},
{
"text": "2014-5775),",
"start": 274,
... | [] |
This paper is based on observations collected at the European Southern Observatory Very Large Telescope, Cerro Paranal, Chile–Programs 166.A-0106, 079.B-0469, 185.A-0745, 092.A-0170. We are indebted to an anonymous referee for helpful comments that clarified several points in the paper. VD is grateful to Gwen Rudie for... | {
"entities": {
"observatory": [
{
"text": "European Southern Observatory",
"start": 53,
"end": 82
}
],
"telescope": [
{
"text": "Very Large Telescope,",
"start": 83,
"end": 104
}
],
"location": [
{
"text": "Cerr... | [] |
Acknowledgements We thank G. Dashyan, M. Lemoine, C. Pfrommer, R. Teyssier, and A. Wagner for enlightening discussions. We warmly thank S. Rouberol for smoothly running the Horizon cluster on which several simulations were run. This work was supported by the ANR grant LYRICS (ANR-16-CE31-0011) and the CNRS programs “Pr... | {
"entities": {
"person": [
{
"text": "G. Dashyan,",
"start": 26,
"end": 37
},
{
"text": "M. Lemoine,",
"start": 38,
"end": 49
},
{
"text": "C. Pfrommer,",
"start": 50,
"end": 62
},
{
"text": ... | [] |
might be candidates of prestellar cores or simply overdensities of molecular gas flows. 4.2. Gas Temperatures in Dense Cores We estimated gas temperatures in dense cores using the VLA (1, 1) and (2, 2) lines. The temperatures were then used to calculate core masses below. Line widths, column densities, and optical dept... | {
"entities": {
"telescope": [
{
"text": "VLA",
"start": 180,
"end": 183
},
{
"text": "VLA",
"start": 1496,
"end": 1499
},
{
"text": "Herschel",
"start": 2768,
"end": 2776
},
{
"text": "SMA",
... | [] |
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