adsabs/WIESP2022-NER huggingface dataset:
Paper: 2016A&A...592A..83K (fulltext)
sources HD 100546 and TW Hya. 2. For both disks, we fitted fully parametric physical models to the spectral energy distribution, spatially resolved CO emission, and a range of far-infrared emission lines. The most important difference from past physical models is that spatially resolved CO line emission is also reproduced. 3. We confirm earlier findings that the HD 100546 disk atmosphere has either an interstellar gas-phase carbon abundance ([C]/[H] , if = 10) or is moderately depleted ([C]/[H], if = 100); and that the TW Hya disk atmosphere is two orders of magnitude deficient in gas-phase volatiles ([C]/[H], [O]/[H], and ). 4. Upper limits on HD emission for HD 100546 put an upper limit of on the gas to dust ratio in the disk. 5. The star HD 100546 has solar-like photospheric abundances of volatile elements (C, N, O) but a strong depletion of rock-forming elements (e.g. Fe, Mg, Si). 6. Most carbon atoms in the HD 100546 disk gas have not passed through a hydrocarbon more complex than CH during the lifetime of the system. 7. An underabundance of volatile elements in the disk atmosphere can develop when gas is mixed through the midplane and the temperature there allows freeze-out of major carrier species onto settled grains. An analytical formulation of this process is presented in Sect. 6.2 . 8. The volatiles return to the gas in the inner disk, as evidenced by their enhanced abundance relative to refractory elements in the gas accreting onto both stars. Appendix A: HD 100546 photospheric abundances Table A.1 Photospheric abundances derived for HD 100546. Notes. Number of lines used in the abundance fitting is shown in Col. 4. Asterisks denote very uncertain results. Solar abundances are from Asplund et al. (2009) . The photospheric properties of HD 100546 were derived through directly fitting synthetic spectra to the optical spectrum of the star. This process gives a measurements of , , , and chemical abundances. The synthetic spectra were calculated using the Z eeman spectrum synthesis program ( Landstreet 1988 ; Wade et al. 2001 ), using model stellar atmospheres from ATLAS9 ( Kurucz 1993 ), and atomic data from the Vienna Atomic Line Data Base (VALD; Kupka et al. 1999 ). The best-fit stellar parameters were derived using and automatic minimization routine, in which all parameters were fitted simultaneously ( Folsom et al. 2012 ). This fitting process was performed on none independent spectral windows (416427, 440460, 460480, 490510, 510520, 520540, 540560, 620650, and 710750 nm). The final best fit parameters are the averages of the individual windows, and the uncertainties are the standard deviations. In cases where a chemical abundance for an element was derived in only three or fewer windows, the uncertainties were increased to account for the full window-to-window variation, as well as any potential uncertainties due to line blending and continuum normalization. Great care was taken to avoid any lines contaminated by emission. Weak
Paper: 2020MNRAS.492.3032K (acknowledgments)
ACKNOWLEDGEMENTS We thank the anonymous referee for the useful comments that allowed us to improve this paper. We also thank P. Bergeron for providing cooling tracks for WDs with mixed atmospheres. The work is based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. iraf is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. 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 ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work also used public data from the North American Nanohertz Observatory for Gravitational Waves (NANOGrav; http://nanograv.org ), which is designated as a ‘Physics Frontiers Center’ by the National Science Foundation (award # 1430284). DAZ thanks Pirinem School of Theoretical Physics for hospitality. The work of AYuK, AVK, and DAZ was supported by the Russian Foundation for Basic Research, project no. 18-32-20170 mol_a_ved. The work of SVZ was supported by PAPIIT grants IN-100617 and IN-102120.
Paper: 2015ApJ...812..139K (acknowledgments)
We thank the Ulysses project at ESA and NASA/JPL for effective and successful mission operations and an anonymous referee for improving the presentation of our results. H.K. is also grateful to Klaus Hornung for valuable discussions during the preparation of this manuscript. This research was supported by the German Bundesministerium für Bildung und Forschung through Deutsches Zentrum für Luft-und Raumfahrt e.V. (DLR, grant 50 QN 9107). H.K. and P.S. gratefully acknowledge support by MPI für Sonnensystemforschung. P.S. acknowledges support by Deutsche Forschungsgemeinschaft (DFG) grant KR 3621/1-1. Facility: Ulysses .
Paper: 2020MNRAS.497.2899M (fulltext)
the 2MASS All Sky Data Release. 4 The zero-points with their standard errors are taken from Maíz Apellániz Pantaleoni González ( 2018 ). For the WISE photometry, we calculate synthetic magnitudes on the AB magnitude scale and then apply the corrections to Vega magnitudes from Jarrett et al. ( 2011 ) for which the estimated error is 1.45 per cent (0.016 mag). For the IUE NEWSIPS spectra, we adopted a zero-point error of 4 per cent from Nichols Linsky ( 1996 ). 3.3 Interstellar reddening Fig. 3 shows a selection of HARPS spectra of AI Phe obtained from the ESO Science Archive Facility in the region of the Na i doublet. There are no detectable interstellar absorption lines in this region and so the reddening towards AI Phe must be very close E ( B − V ) = 0 (Karataş Schuster 2010 ). Accordingly, we set a Gaussian prior on the reddening E ( B − V ) = 0 ± 0.005 and set a lower limit E ( B − V ) ≥ 0. Figure 3. HARPS spectra of AI Phe in the region of the Na i doublet. The spectra have been normalized and vertically offset for clarity. The rest wavelengths of the Na i lines are indicated by vertical dashed lines. 3.4 Priors on infrared flux ratios The near-infrared (NIR) flux from solar-type stars compared to the total flux or the flux at optical wavelengths shows a well-defined relationship with T eff that is almost linear and that has little dependence on metallicity or surface gravity. This is the basis of the infrared flux method (Blackwell, Shallis Selby 1979 ; Casagrande et al. 2010 ) or the use of colours such as () to estimate effective temperatures for FGK-type stars (Boyajian et al. 2013 ). There is only one direct measurements of the flux ratio for AI Phe at wavelengths longer than 1 μm. We were concerned that not imposing any additional constraints on the flux ratio at these wavelengths could mean that the resulting models become unrealistic, e.g. the () colours computed using samples from P ( M | D ) might show a much large scatter than is observed in real stars. This could happen if the use of distortion coefficients allows for models where the flux from one star is unrealistically high at NIR wavelengths while the other is too low, unless some constraint is placed on the flux ratio at these wavelengths. We address this concern by making the assumption that the stars in AI Phe behave similarly to other dwarf and sub-giant FGK-type stars in the solar neighbourhood in order to put some constraint on the flux ratio in the 2MASS J, H , and K s bands, and the WISE W 1, W 2, W 3, and W 4 bands. We use stars from the Geneva–Copenhagen survey (Holmberg et al. 2009 ) to define relationships between T eff and ( V − J ), ( V − H ), etc. The values of T eff , E ( B − V ), log g , and [Fe/H] for each star are taken from Casagrande et al. ( 2011 ). We define separate relations for the F7 V star and the K0 IV star based on a different subsample of stars with similar properties to each. For the F7 V star, the subsample is defined by the following
Paper: 2017ApJ...840....6R (acknowledgments)
It is a pleasure to thank G. Bodo, M. Chandra, S. Davis, J. Dolence, J. Goodman, G. Lesur, V. Paschalidis, J. Simon, and J. Stone for useful discussions. We also thank the anonymous referee for a very useful report. The numerical calculations presented here were performed on the Blue Waters supercomputer at NCSA. B.R.R. was supported by an Illinois Distinguished Fellowship and by NSF grant AST-1333612. Work at Los Alamos National Laboratory was done under the auspices of the National Nuclear Security Administration of the US Department of Energy. C.F.G.’s work was also supported in part by a Romano Professorial Scholar appointment, a Simons Fellowship in Theoretical Physics, and a Visiting Fellowship at All Souls College, Oxford.
Paper: 2016ApJ...831..162R (acknowledgments)
We thank the referee for their insightful suggestions, which led to improvements in the presentation of the paper. IR also thanks F. Cattaneo for his important and informative discussions about magnetic field generation during WD smoldering. This work was supported by NSF Grant AST-0709181 and by NSF Graduate Research Fellowship Grant DGE-1144082.
Paper: 2020ApJ...897...84T (fulltext)
from the Kerr solution is found, this approach is not suitable to measure the deviation from the Kerr geometry and it is necessary to use a different method. Among the many proposed parametric black-hole spacetimes in literature, here we use the Johannsen metric (Johannsen 2013 ). In its simplest form, which is the version employed in our work, the Johannsen metric has only one deformation parameter, named α 13 (see Johannsen 2013 for the origin of this parameter). In Boyer–Lindquist coordinates, the line element reads (we use units in which G N = c = 1)where , , , andFor α 13 = 0, we recover the Kerr metric. In order to have a regular exterior region, we have to impose (as in the Kerr metric, for there is no event horizon and the central singularity is naked) and the following restriction on α 13 (Tripathi et al. 2018 ) Note that α 13 enters the metric coefficients g tt , g tφ , and g φφ . It thus affects the structure of the accretion disk, modifying the Keplerian gas motion and moving the ISCO radius. Qualitatively speaking, α 13 > 0 ( 0) increases (decreases) the strength of the gravitational force, so it moves the ISCO radius to higher (lower) values and this explains the strong correlation with the spin parameter in the plots that will be presented in the next sections. 3. Data Reduction and Analysis LMC X-1 was discovered in 1969 as the first extragalactic X-ray binary (Mark et al. 1969 ; Price et al. 1971 ). The system consists of a stellar-mass black hole and an O-giant companion star. The distance of the source, the black-hole mass, and the inclination angle of the orbit, which are three key-quantities in the continuum-fitting method, have been estimated to be D = 48.10 ± 2.22 kpc, M = 10.91 ± 1.54 M ⊙ , and i = 3638 ± 202, respectively (Gou et al. 2009 ; Orosz et al. 2009 ). LMC X-1 is characterized by a quite stable bolometric luminosity, which is about 16% of its Eddington luminosity L Edd (Gou et al. 2009 ) and thus nicely meets the standard criterion required to use the continuum-fitting method: sources with an accretion luminosity in the range 5%–30% L Edd (McClintock et al. 2014 ). The measurement of the spin parameter of the black hole in LMC X-1 using the continuum-fitting method was presented in Gou et al. ( 2009 ), and here we follow that study. There are 55 pointed observations of LMC X-1 with the Proportional Counter Array (PCA) on board RXTE (Swank 1999 ). To use the continuum-fitting method, it is desirable to choose thermal dominant spectral data, which are defined by three conditions (Remillard McClintock 2006 ): (i) the flux of the thermal component accounts for more than 75% of the total 2–20 keV unabsorbed flux, (ii) the root mean square (rms) variability in the power density spectrum in the 0.1–10 Hz range is lower than 0.075, and (iii) quasi-periodic oscillations are absent or very weak. Imposing these three conditions, we only have three observations, which are named “gold spectra” in Gou et al. ( 2009 ) as
Paper: 2016ApJ...825..116F (acknowledgments)
The authors are grateful for useful suggestions from the CBC group of the LIGO Scientific–Virgo Collaboration. In particular, we are grateful to Walter Del Pozzo for useful advice, Vivien Raymond for helpful discussions, Simon Stevenson for careful reading, and Neil Cornish for beneficial comments. B.F. was supported by the Enrico Fermi Institute at the University of Chicago as a McCormick Fellow. This work was supported in part by the Science and Technology Facilities Council. P.B.G. acknowledges NASA grant NNX12AN10G. S.V. acknowledges the support of the National Science Foundation and the LIGO Laboratory. J.V. was supported by STFC grant ST/K005014/1. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-0757058. This work used computing resources at CIERA funded by NSF PHY-1126812, as well as the computing facilities of the LIGO Data Grid including: the Nemo computing cluster at the Center for Gravitation and Cosmology at the University of Wisconsin–Milwaukee under NSF Grants PHY-0923409 and PHY-0600953; the Atlas computing cluster at the Albert Einstein Institute, Hannover; the LIGO computing clusters at Caltech, and the facilities of the Advanced Research Computing @ Cardiff (ARCCA) Cluster at Cardiff University. Some results were produced using the post-processing tools of the plotutils library at http://github.com/farr/plotutils and skyarea library at https://github.com/farr/skyarea . This paper has been assigned LIGO document reference LIGO-P1500117.
Paper: 2021MNRAS.504.3909C (fulltext)
energy. Figure 7. Drift along time of the CoM of the bound core with respect to the CoM of the whole system, for one of the simulations of set 1A. The Lagrangian radii are evaluated in percentage of the total mass of the cluster and so all the bodies, including possibly escaping IMBHs and growing (in mass) objects, are taken into account. Of course, the escaping IMBHs lead to a natural increase of the high-percentage Lagrangian radii so that in Fig. 5 we display only up to the 50 percent Lagrangian radius ( R 1/2 ). Note that growing massive objects, although they remain inside the bound core of the system and close to its CoM, do not a priori coincide with this CoM (see Fig. 8 that shows, also, how the growing BH movement is since the beginning well within the half-mass radius) and could, consequently, induce sharp variations in the latter evolution of the low-percentage Lagrangian radii. Figure 8. Black line gives the distance ( r smo ) of the growing supermassive object to the CoM of the bound ‘core’ of the system, for one arbitrarily chosen simulation of set 1A, taken as example. For comparison, we also give in purple the half-mass radius of the system. The curves are plotted starting from the time when the SMBH ‘seed’ is already grown by 42 IMBH mergers. The late time evolution of the average half-mass radius R 1/2 (50 percent Lagrangian radius), which is a good definition of the system radial scale, is well fitted by a linear relation: For set 1 and t > 15 yr, the values of the parameters are leading to a root mean square error of the fit equal to 0.8 mpc for R 1/2 . For set 2 and t > 500 yr, the values are giving a root mean square error equal to 5 mpc. The average half-mass radius at the final simulation time for set 1 is equal to 24 mpc (37 mpc for set 2), that is 50 times (8 times for set 2) the initial half-mass radius, R 1/2 (0) = 2 −1/3 R 0 . Even with our original safety margin of one order of magnitude for the initial cluster radial size, at the end of the simulation the core of the cluster extends much farther out than the area allowed for our purpose of mimicking the presence of an SMBH by a dense cluster of IMBHs. This is true for every simulation of set 1 and not only on average. This is even more the case for set 2, where no safety margin was taken. This result is not surprising: We actually expected that the extreme conditions required (a stable system of IMBHs of total mass and maximal size ≤5 mpc) were very unlikely to be reached. As we see in the next section, in both set 1 and set 2 the IMBH cluster undergoes various merger episodes. This has relevant consequences, whose main result is the formation of a very massive BH as coming out from the dominant object growing up after successive merger events. Hence, we conclude that, as expected on basic theoretical understanding, the answer to the first of the issues we raised in introduction is negative: A cluster of IMBHs dense enough to mimic the dynamical role of an
Paper: 2018A&A...610A..35H (acknowledgments)
Acknowledgements The authors thank the referee for their comments that allowed us to improve the article. D. Hypolite and S. Mathis acknowledge funding by the European Research Council through ERC SPIRE grant 647383 and the CNES PLATO grant at CEA Saclay. The authors also wish to thank the MESA website. M. Rieutord acknowledges funding by the French Agence Nationale de la Recherche (ANR), under grant ESRR (ANR-16-CE31-0007-01). This work was also supported by the Centre National de la Recherche Scientifique (CNRS, UMR 5277), through the Programme National de Physique Stellaire (PNPS), and by the CNES PLATO grant at IRAP.
Paper: 2015ApJ...806..212D (acknowledgments)
The authors wish to thank the anonymous referee, whose helpful comments greatly improved the quality of this manuscript. This work was supported by Kepler Cycle 2 GO grant NNX11AB71G and Cycle 3 GO grant NNX12AC79G and NSF grant AST13-11678. We are pleased to thank John Gizis for advance use of his GO program’s long-cadence data on GJ 1243. We thank John P. Wisniewski and Adam F. Kowalski for continuing discussions on stellar activity, and Rakesh Yadav for very useful comments on an early draft of this manuscript. J.R.A. Davenport thanks Morgan Fouesneau for help with Python code. Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA’s Science Mission Directorate.
Paper: 2017ApJ...851...26V (acknowledgments)
We thank the anonymous referee for their thoughtful comments and useful suggestions. This material is based upon work supported by the National Science Foundation under grant No. 1716260. Additional support for this work was provided by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institutem and by the Department of Astronomy and the Institute for Astrophysical Research at Boston University. A.W.M. is supported through Hubble Fellowship grant 51364 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. F.A. received funding from the French “Programme National de Physique Stellaire” (PNPS) and the “Programme National de Planetologie” of CNRS (INSU). D.H. is supported by the Collaborative Research Centre SFB 881 “The Milky Way System” (subproject A4) of the German Research Foundation (DFG). This research made use of the Massachusetts Green High Performance Computing Center in Holyoke, MA. The data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
Paper: 2016A&A...592L...9M (acknowledgments)
We would like to thank Carlos de Breuck and Theresa Nilsson for their support for the observations. This publication is based on data acquired with the Atacama Pathfinder EXperiment (APEX) which is a collaboration between the Max-Planck-Institut für Radioastronomie, ESO, and the Onsala Space Observatory. We acknowledge the use of the GILDAS software for the data reduction. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Advanced Grant RADIOLIFE-320745.
Paper: 2016MNRAS.460.2779C (acknowledgments)
We acknowledge the comments received from an anonymous referee, which helped to improve the quality of this paper. GALC acknowledges the support of an STFC PhD studentship. This research utilised Queen Mary's MidPlus computational facilities, supported by QMUL Research-IT and funded by EPSRC grant EP/K000128/1.
Paper: 2015ApJ...804...98K (acknowledgments)
The authors acknowledge the continuous and fruitful interactions with Jorma Harju, and an anonymous referee for helping improve the manuscript. S.K. acknowledges support from Xueying Tang and an NRAO Student Observing Support grant. J.C.T. acknowledges support from the University of Florida Research Opportunity Seed Fund and the Florida Space Inst. V.W. acknowldeges funding by the French INSU/CNRS program PCMI, the Observatoire Aquitain des Sciences de l’Univers and the European Research Council (ERC Grant 336474: 3DICE).
Paper: 2019MNRAS.482..758S (acknowledgments)
ACKNOWLEDGEMENTS We thank Robert Izzard and Conor Byrne for helpful discussions. The Armagh Observatory and Planetarium is funded by direct grant from the Northern Ireland Dept for Communities. The authors acknowledge support from the UK Science and Technology Facilities Council (STFC) Grant No. ST/M000834/1.