THE GALEX ARECIBO SDSS SURVEY. VII. THE BIVARIATE NEUTRAL HYDROGEN-STELLAR MASS FUNCTION FOR MASSIVE GALAXIES

THE GALEX ARECIBO SDSS SURVEY. VII. THE BIVARIATE NEUTRAL HYDROGEN-STELLAR MASS FUNCTION FOR MASSIVE GALAXIES

We present the bivariate neutral atomic hydrogen (H I)-stellar mass function (HISMF) [phi](M sub(H I), M[low *]) for massive (log M[low *]/M sub([middot in circle]) > 10) galaxies derived from a sample of 480 local (0.025 < z < 0.050) galaxies observed in H I at Arecibo as part of the GALEX...

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Bibliographic Details
Published in:The Astrophysical journal 2013-10, Vol.776 (2), p.1-25
Main Authors: LEMONIAS, JENNA J, Schiminovich, David, Catinella, Barbara, Heckman, Timothy M, Moran, Sean M
Format: Article
Language:eng
Subjects:
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COMPUTERIZED SIMULATION
COSMOLOGY
Density
GALAXIES
HYDROGEN
HYDROGEN 1
LIMITING VALUES
MASS
Mathematical analysis
Mathematical models
Parametrization
STAR EVOLUTION
STARS
Stellar mass
Trends
UNIVERSE
VARIATIONS
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Summary:We present the bivariate neutral atomic hydrogen (H I)-stellar mass function (HISMF) [phi](M sub(H I), M[low *]) for massive (log M[low *]/M sub([middot in circle]) > 10) galaxies derived from a sample of 480 local (0.025 < z < 0.050) galaxies observed in H I at Arecibo as part of the GALEX Arecibo SDSS Survey. We fit six different models to the HISMF and find that a Schechter function that extends down to a 1 % H I gas fraction, with an additional fractional contribution below that limit, is the best parameterization of the HISMF. We calculate ohm sub(H I,M[low *] > 10) super(10) and find that massive galaxies contribute 41% of the H I density in the local universe. In addition to the binned HISMF, we derive a continuous bivariate fit, which reveals that the Schechter parameters only vary weakly with stellar mass: M* sub(H I), the characteristic H I mass, scales as M super(0.39)[low *]; alpha , the slope of the HISMF at moderate H I masses, scales as M super(0.07)[low *]; and [functionof], the fraction of galaxies with H I gas fraction greater than 1%, scales as M super(-0.24)[low *]. The variation of [functionof] with stellar mass should be a strong constraint for numerical simulations. To understand the physical mechanisms that produce the shape of the HISMF, we redefine the parameters of the Schechter function as explicit functions of stellar mass and star formation rate (SFR) to produce a trivariate fit. This analysis reveals strong trends with SFR. While M* sub(H I) varies weakly with stellar mass and SFR (M* sub(H I) [is proportional to] M super(0.22)[low *], M* sub(H I) [is proportional to] SFR super(-003)), alpha is a stronger function of both stellar mass and especially SFR ( alpha [is proportional to] M super(0.47)[low *], alpha [is proportional to] SFR super(095)). The HISMF is a crucial tool that can be used to constrain cosmological galaxy simulations, test observational predictions of the H I content of populations of galaxies, and identify galaxies whose properties deviate from average trends.
ISSN:0004-637X
1538-4357