Journal
ASTROPHYSICAL JOURNAL
Volume 941, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/1538-4357/ac9ccb
Keywords
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Categories
Funding
- National Key R&D Program of China [2018YFA0404502]
- National Natural Science Foundation of China [11821303, 11733002, 11973030, 11673015, 11733004, 11761131004, 11761141012]
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy
- National Aeronautics and Space Administration
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- Astrophysical Research Consortium
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- University of Cambridge
- Case Western Reserve University
- University of Chicago
- Drexel University
- Fermilab
- Institute for Advanced Study
- Japan Participation Group
- Johns Hopkins University
- Joint Institute for Nuclear Astrophysics
- Kavli Institute for Particle Astrophysics and Cosmology
- Korean Scientist Group
- Chinese Academy of Sciences (LAMOST)
- Los Alamos National Laboratory
- Max Planck Institute for Astronomy (MPIA)
- Max Planck Institute for Astrophysics (MPA)
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
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We present a new H I mass estimator that provides unbiased H I mass estimates for optical samples like SDSS. We apply this estimator to study the H I mass function of local galaxies and the H I-halo mass relation. Our results show that the discrepancies between different measurements are primarily caused by cosmic variance.
We present a new H I mass estimator that relates log(10)(M-HI/M-*) to a linear combination of four galaxy properties: stellar surface mass density, color index u - r, stellar mass, and concentration index, with the scatter of individual galaxies around the mean H I mass modeled with a Gaussian distribution function. We calibrate the estimator using the xGASS sample, including both H I detection and nondetection, and constrain the model parameters through Bayesian inferences. Tests with mock catalogs demonstrate that our estimator provides unbiased H I masses for optical samples like SDSS. We apply our estimator to the SDSS spectroscopic sample to estimate the H I mass function (HIMF) of local galaxies, as well as the conditional H I mass function in galaxy groups and the H I-halo mass relation. Our HIMF agrees with the ALFALFA measurements at M-HI ? 5 x 10(9) M-(R), but with higher amplitude and a steeper slope at lower masses. We show that this discrepancy is caused primarily by the cosmic variance, which is corrected for the SDSS sample but not for ALFALFA. The total CHIMFs for all halo masses can be described by a single Schechter function, while those of central galaxies show a double-Gaussian profile. The total H I mass in a group increases monotonically with halo mass, but for central galaxies, the H I mass shows weak dependence on halo mass when M-h ? 10(12) M-?. The observed H I-halo mass relation is not reproduced by current hydrodynamic simulations and semianalytic models of galaxy formation.
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