J/ApJ/776/74ivo://CDS.VizieR/J/ApJ/776/74doi:10.26093/cds/vizier.17760074CDSLemonias J.J.Schiminovich D.Catinella B.Heckman T.M.Moran S.M.2015-05-18T11:11:46Z2015-04-22T14:56:05ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxiesultraviolet-astronomyh-i-line-emissionsurveysWe present the bivariate neutral atomic hydrogen (HI)-stellar mass function (HISMF) {phi}(M_HI_, M_{star}_) for massive (logM_*_/M_{sun}_>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% HI gas fraction, with an additional fractional contribution below that limit, is the best parameterization of the HISMF. We calculate {Omega}_HI,M_{star}__>10^10^ 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_HI_^*^, the characteristic H I mass, scales as M_{star}_^0.39^; {alpha}, the slope of the HISMF at moderate H I masses, scales as M_{star}_^0.07^; and f, the fraction of galaxies with HI gas fraction greater than 1%, scales as M_{star}_^-0.24^. The variation of f 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_HI_^*^ varies weakly with stellar mass and SFR (M_HI_^*^{prop.to}M_{star}_^0.22^, M_HI_^*^{prop.to}SFR^-0.03^), {alpha} is a stronger function of both stellar mass and especially SFR ({alpha}{prop.to}M_{star}_^0.47^, {alpha}{prop.to}SFR^0.95^). 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.2013ApJ...776...74Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/776/74CatalogResearchIsServedByTAP VizieR generic servicerelated-toII/312 : GALEX-DR5 (GR5) sources from AIS and MIS (Bianchi+ 2011)J/MNRAS/436/34 : GALEX Arecibo SDSS survey. Final release (Catinella+, 2013)J/MNRAS/427/3159 : Quantified HI morphology. VI. NUV/FUV (Holwerda+, 2012)J/A+A/544/A65 : GALEX Arecibo SDSS survey. VI. (Catinella+, 2012)J/AJ/142/170 : ALFALFA survey: {alpha}.40 HI source cat. (Haynes+, 2011)J/MNRAS/403/683 : GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)J/ApJS/173/293 : UV-Optical galaxy color-magnitude diagram I. (Wyder+, 2007)http://www.sdss.org/ : SDSS home pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/776/74https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/776/74http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/776/74https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/776/74https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/776/74http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/776/74GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVRadiodefaultJ/ApJ/776/74/table3Binned data for bivariate (HI)-stellar mass function (HISMF) {Phi}(M_HI_,M_*_)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintM*min[10/11.3] Start of stellar mass bin (StarMassSt)log(solMass)phys.massfloatM*max[10.2/11.5] End of stellar mass bin (StarMassEnd)log(solMass)phys.massfloatMHI[7.9/11] log(HI mass) bin (HIMass)log(solMass)phys.massfloatDenAll[-4.9/-2.8]? log10 of space density of all detections and upper limits log{Phi}(M_HI_,M_*_)log(Mpc**-3)phys.densityfloatnullablee_DenAll[0.07/0.5]? Poisson uncertainty in DenAlllog(Mpc**-3)stat.errorfloatnullableDenDet[-5/-2.9]? log10 of space density of detections log{Phi}(M_HI_,M_*_)log(Mpc**-3)phys.densityfloatnullablee_DenDet[0.1/0.5]? Poisson uncertainty in DenDetlog(Mpc**-3)stat.errorfloatnullable