adsabs/WIESP2022-NER huggingface dataset:
Paper: 2021ApJS..253...46P (fulltext)
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 line luminosity, in erg s −1 . (This table is available in its entirety in machine-readable form.) Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available. Table 4 The Spectral Parameters Associated with the Mg ii Emission Line Note. Column information is as follows: Column [1]: 4FGL name; Column [2]: redshift; Column [3]: log-scale continuum luminosity at 3000 Å; Column [4]: FWHM of Mg ii line, in km s −1 ; and Column [5]: log-scale Mg ii line luminosity, in erg s −1 . (This table is available in its entirety in machine-readable form.) Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available. Table 5 The Spectral Parameters Associated with the C iv Emission Line Note. Column information is as follows: Column [1]: 4FGL name; Column [2]: redshift; Column [3]: log-scale continuum luminosity at 1350 Å; Column [4]: FWHM of C iv line, in km s −1 ; and Column [5]: log-scale C iv line luminosity, in erg s −1 . (This table is available in its entirety in machine-readable form.) Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available. 3.2. Absorption-line Spectrum The optical spectra of 346 γ -ray blazars show prominent absorption lines, e.g., the Ca HK doublet, primarily originating from the stellar population in the host galaxy. It has been shown in various works that the mass of the central black hole significantly correlates with the stellar velocity dispersion ( σ * , see Ferrarese Merritt 2000 ; Gültekin et al. 2009 ; Kormendy Ho 2013 ). Therefore, we have used the penalized PiXel Fitting tool ( pPXF ; Cappellari Emsellem 2004 ) to derive σ * for blazars present in the sample. This software works in pixel space and uses a maximum penalized likelihood approach to calculate the line-of-sight velocity distribution (LOSVD) from kinematic data (Merritt 1997 ). A large set of stellar population synthesis models (adopted from Vazdekis et al. 2010 ) with a spectral resolution of FWHM = 2.5 Å and the wavelength coverage of [3525, 7500] Å (Sánchez-Blázquez et al. 2006 ) was used in this work. The pPXF code first creates a template galaxy spectrum by convolving the stellar population models with the parameterized LOSVD. To mimic the nonthermal power-law contribution from the central nucleus, we further added a fourth-order Legendre polynomial to the model. The regions of bright emission lines were masked prior to the fitting. The model was then fitted on the rest-frame galaxy spectrum, and σ * and the
Paper: 2019MNRAS.489.2079L (acknowledgments)
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 from an Alfred P. Sloan Fellowship. We gratefully acknowledge the support of NVIDIA Corporation with the donation of a Titan Xp GPU used in this research. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Centre for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org . 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.
Paper: 2020ApJ...901...37L (fulltext)
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 is indicated by the red dotted line. The upper state energy of each transition is given in the top-left corner. At a number of positions a handful of spectral features are identified that can be assigned to NH 2 C(O)NH 2 . The most and clearest lines are identified toward position MM1-v, see Figure 6 , with at least three unblended lines. While these lines are not enough for a secure detection, a tentative identification can be claimed. The tentative and upper-limit column densities of NH 2 C(O)NH 2 are presented in Table 3 . Figure 6. Overview of NH 2 C(O)NH 2 spectral features toward position MM1-v. The observed spectrum is plotted in black, with the synthetic spectrum overplotted in blue and the rest-frequency center of the transition is indicated by the red dotted line. The upper state energy of each transition is given in the top-left corner. 4. Discussion 4.1. Chemical Comparisons To get a better understanding of the chemical processes leading to amides, it is useful to compare molecular ratios of the positions within NGC 6334I, but also with other inter- and circumstellar sources. In the following subsections molecular ratios with respect to NH 2 CHO are discussed. Comparisons are made with the following works: IRAM 30 m and Green Bank Telescope (GBT) single-dish observations of G + 0.693-0.027 (hereafter G + 0.693), a quiescent giant molecular cloud (Zeng et al. 2018 ; Jiménez-Serra et al. 2020 ); ALMA observations of the incipient hot corino Barnard B1b-S (Marcelino et al. 2018 ); Northern Extended Millimeter Array observations of the low-mass protostars SVS13A, NGC 1333-IRAS4A2, NGC 1333-IRAS2A(1) (Coutens et al. 2018 ; Belloche et al. 2020 ); ALMA Protostellar Interferometric Line Survey (Jørgensen et al. 2016 ) observations of the low-mass protostar IRAS 16293B (Coutens et al. 2016 , 2018 ; Ligterink et al. 2018a ); GBT and IRAM 30 m single-dish observations of the Galactic center source Sgr B2 (Hollis et al. 2006 ; Belloche et al. 2013 ); ALMA observations of the HMSFR Orion KL (Cernicharo et al. 2016 ); the high-mass star AFGL 4176 (Bøgelund et al. 2019a ); and of Sgr B2 (Belloche et al. 2017 , 2019 ). One has to be aware that precise knowledge of the source size or emitting area of a certain molecule is essential for ratio comparisons. In particular, single-dish telescopes do not have the spatial resolution to determine the source size and these are often assumed or estimated, potentially resulting in large column density errors. Finally, mass spectrometric measurements of the Rosetta mission to comet 67P/C-G are used to compare with a solar system object (Goesmann et al. 2015 ; Altwegg et al. 2017 ). The
Paper: 2020ApJ...901...69C (fulltext)
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 s −1 . Dotted: turbulence 500 km s −1 . We also plot the line ratios at the turbulence of 500 km s −1 . Such a high value of the turbulence is not applicable in our region of interest, but may apply for gas in other environments such as merging galaxy clusters (Cassano Brunetti 2005 ). Optical depth can be expressed as a product of column density ( N ), and absorption cross section ( α ν ):where α ν is inversely proportional to the total Doppler velocity.where is the downward transition probability, is the oscillator strength and other symbols have their usual meaning (Mihalas 1970 ). If the temperature is held constant, an increase in the turbulent velocity decreases α ν , which decreases the overall optical depth. Ideally, to achieve the same optical depth at zero and higher turbulent velocity, a higher column density should be required for the latter case. However, this outcome gets reversed due to line interlocking of x, y, and z with other ions (e.g., Fe 23+ , Cr 22+ , and Fe 22+ ; see Paper I ). The higher the turbulent velocity is, the higher the Doppler width of a line and the more pronounced the line interlocking effects will be. Total line-center optical depth will therefore increase with turbulent velocity rather than decrease, as Equation ( 3 ) suggests. 6.4. Interplay between Column Density and Metallicity Figure 13 shows the line ratios relative to w as contour plots by varying the hydrogen column density and metallicity. In the low-column-density limit, the line ratios are minimally affected by the change in metallicity. Figure 6 shows the effects of metallicity on the line ratios at the reported value of hydrogen column density by Hitomi Collaboration et al. ( 2018b ) (). The uncertainties in temperature and collision strengths from the sources mentioned previously contribute to the uncertainties in the line ratios (shown with the solid enclosed lines in Figure 6 ). At the reported hydrogen column density, x, y, and z are optically thin (Paper I ). Therefore, the line ratios are minimally affected with change in metallicity as these lines are still optically thin for the metallicity range (0 ≤ Z (solar) ≤ 5) shown in the figure. Figure 13. Left, middle, and right panels show x/w, y/w, and z/w as a function of hydrogen column density and metallicity, respectively. Hitomi Collaboration et al. ( 2018a ) use deprojected heavy element abundances relative to solar in the inner 150 kpc region from Chandra data archive for a spherically symmetric Perseus model. At a distance of 30–60 kpc from the central AGN of the Perseus core, the reported range in metallicity is ∼0.5–0.75 of solar (see Figure 7 in their paper). We
Paper: 2020ApJ...889..154W (acknowledgments)
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. acknowledges support from NSF grant 1517819. M.C. and M.T. acknowledge support from the INAF PRIN-SKA 2017 program 1.05.01.88.04. We thank Francesca Annibali for useful discussions. We also thank the referee for many useful comments that improved the paper. Facility: HST .
Paper: 2016MNRAS.460.1457S (acknowledgments)
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 were partly carried out on Cray XC30 at Center for Computational Astrophysics, National Astronomical Observatory of Japan. SS is supported by a Grant-in-Aid for Young Scientists (Start-up) from the Japan Society for the Promotion of Science (JSPS) (No. 25887012). The MultiDark Database used in this paper and the web application providing online access to it were constructed as part of the activities of the German Astrophysical Virtual Observatory as result of a collaboration between the Leibniz-Institute for Astrophysics Potsdam (AIP) and the Spanish MultiDark Consolider Project CSD2009-00064. The Bolshoi and MultiDark simulations were run on the NASA's Pleiades supercomputer at the NASA Ames Research Center. The MultiDark-Planck (MDPL) and the BigMD simulation suite have been performed in the Supermuc supercomputer at LRZ using time granted by PRACE. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/ . SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.
Paper: 2016MNRAS.457.3266M (acknowledgments)
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 support from Chandra grants GO2-13160A, GO2-13102A, GO4-15115X and NASA grant NNX14AI29G. This work was made possible in part by a grant of high-performance computing resources and technical support from the Alabama Supercomputer Authority. We thank the anonymous referee for the careful reading of the manuscript and suggestions, which improved the presentation of our work.
Paper: 2017ApJ...834...89D (acknowledgments)
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 (SANSA) for partial financial support during his PhD studies. R.M. acknowledges partial financial support from The Italian Space Agency (ASI) under the program “Programma PAMELA—attivita” scientifica di analisi dati in fase E.” The authors would like to thank Dr. M. Boezio for the useful discussion and helpful suggestions. Part of this work is based on archival data provided by the ASI Science Data Center (ASDC).
Paper: 2016ApJ...822...61C (fulltext)
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 results are in agreement with those of Meakin Arnett ( 2007 ; see also Meakin et al. 2015 ; Cristini et al. 2016 ). In particular, we find a highly intermittent flow and mixing due to turbulent entrainment. In terms of the effects of rotation on the strength and properties of convection alone we find our 2D simulations suggest minimal impact and generally lead to an overall small reduction of the total convective power stored in solenoidal motions (“no-rot” versus “rot-2” models) regardless of the nature of convective burning (C, O, or Si shell). We suggest this is due to the effects of the centrifugal forces mildly expanding the star, and thus changing the locations of the convective shells over time, subjecting the shell material to lower temperatures that, in turn, trigger lower nuclear burning rates and weaker convection. That alone may lead to initial velocity perturbations of smaller amplitude than in the case of zero rotation which may have a small impact on the susceptibility to a successful SN explosion following iron core collapse (Couch Ott 2013 ). We emphasize that, to answer the question of whether the inclusion of rotation significantly changes the ICs to the core-collapse SN mechanism, self-consistent evolution with the effects of rotation included is the proper approach to take. In our analysis we have followed the evolution of a 20 M ⊙ SN progenitor with both the effects of rotation and magnetic fields included in the transport of angular momentum and chemical mixing using the MESA code (“rot-ST” models). We find differences in the sign of the effect depending on the nature of convective shell-burning: during C- O-shell burning there is more power stored in the solenoidal components than in the case of no rotation while during Si-shell burning the effects are very small, with hints of even reduction of the solenoidal mode power by the end of the simulation. We attribute this effect to differences in the initial MESA models for the two distinct shell-burning stages. A careful look in the upper panel of Figure 2 shows that the “rot-ST” nuc profile during C- O-shell burning has a secondary peak (due to O-burning) that is nearly an order of magnitude greater than the corresponding one for the “no-rot” model. On the contrary, in Figure 3 we see that during Si-shell burning the peaks in the nuc profile for the “no-rot” model in the region (4–6) × 10 8 cm are greater than the corresponding ones for “rot-ST.” This is due to the enhanced chemical mixing by the ST mechanism during the C- O-shell burning phase that effectively recycles fresh fuel from outer layers to deeper and hotter regions enabling faster specific
Paper: 2017ApJ...836...75D (fulltext)
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 bluer parts of the galaxy flux (see also Elmegreen Elmegreen 2014 ). Figure 9. Examples of galaxies with apparent spiral structures at different redshifts. The residual images, after removal of the bulge+disk model from the original galaxy image, allow for more effective detection of fine substructure. Table 5 Estimated Fraction of Massive Galaxies with a Prominent Stellar Disk Using Different Diagnostics Note. Column (1) Massive galaxies with bulge-to-total ratios less than 0.5. Column (2) Massive galaxies with visually detectable spiral structures. Column (3) Edge-on massive galaxies with e > 0.6. The conditions necessary for the formation of spiral arms are complex (see Dobbs Baba 2014 for a review), but one requirement is clear—the existence of a disk. Thus, from the point of view of one of the main themes of this paper, the clear detection of spiral features in high- z massive galaxies constitutes arguably the strongest, most model-independent evidence for the presence of a substantial disk component in these systems. We see the spiral features only in the star-forming galaxies and not in quiescent systems, but, by analogy with local S0 and spiral galaxies, this is not surprising. An edge-on view of a galaxy can reveal another indisputable signature of a prominent stellar disk. Figure 10 gives several examples of highly flattened ( e > 0.6) galaxies in our sample that are consistent with disk structures seen edge-on. Interestingly, most of them are relatively thick. The fraction of galaxies with a stellar disk can be inferred from the frequency of detected edge-on galaxies. For this estimation, we assume a uniform distribution of ellipticity with 0 e 0.8 for a population of bulge+disk systems. The inferred fraction of galaxies with a disk hovers around 40%–50% at 1.0 z 2.5, among both star-forming and quiescent galaxies, but the incidence of edge-on quiescent galaxies below z = 1 drops to zero (Table 5 ). Highly flattened systems (especially at high z ) can be hallmarks of a merger. However, considering the fact that the majority of these galaxies are compact, the chance of this degeneracy is low. Figure 10. Examples of massive galaxies with an edge-on disk at different redshifts. 5. Implications for Galaxy Evolution The discovery of red nuggets has captured much attention in recent years because it requires a new paradigm for the formation and evolution of massive elliptical galaxies. The observed compactness of red nuggets at z ≈ 2 initially raised the question of whether the massive red galaxies have indeed increased their sizes by a factor of roughly ∼3–5 while maintaining their passive state, or whether the size
Paper: 2016ApJ...832..125H (acknowledgments)
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 (GS-2011A-Q-91) obtained at the Gemini Observatory, processed using the Gemini IRAF package, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnologa e Innovacin Productiva (Argentina), and Ministrio da Cincia, Tecnologia e Inovao (Brazil). This paper uses observations made at the South African Astronomical Observatory (SAAO).