The GALEX Arecibo SDSS Survey I: gas fraction scaling relations of massive galaxies and first data release

By B. Catinella, David Schiminovich, G. Kauffmann, S. Fabello, Jing Wang, Cameron Hummels, J. Lemonias, S. M. Moran, R. Wu, R. Giovanelli and 16 more. 2009

356 citations recorded by the source corpus.

We introduce the GALEX Arecibo SDSS Survey (GASS), an on-going large programme that is gathering high quality H i-line spectra using the Arecibo radio telescope for an unbiased sample of ~1000 galaxies with stellar masses greater than 10^(10) M_⊙ and redshifts 0.025 < z < 0.05 , selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and Galaxy Evolution Explorer (GALEX) imaging surveys. The galaxies are observed until detected or until a low gas mass fraction limit (1.5–5 per cent) is reached. This paper presents the first Data Release, consisting of ~20 per cent of the final GASS sample. We use this data set to explore the main scaling relations of the H i gas fraction with galaxy structure and NUV−r colour. A large fraction (~60 per cent) of the galaxies in our sample are detected in H i. Even at stellar masses above 10^(11) M_⊙, the detected fraction does not fall below ~40 per cent. We find that the atomic gas fraction M_(HI)/M★ decreases strongly with stellar mass, stellar surface mass density and NUV−r colour, but is only weakly correlated with the galaxy bulge-to-disc ratio (as measured by the concentration index of the r-band light). We also find that the fraction of galaxies with significant (more than a few per cent) H I decreases sharply above a characteristic stellar surface mass density of 10^(8.5) M_⊙ kpc^(−2). The fraction of gas-rich galaxies decreases much more smoothly with stellar mass. One of the key goals of GASS is to identify and quantify the incidence of galaxies that are transitioning between the blue, star-forming cloud and the red sequence of passively evolving galaxies. Likely transition candidates can be identified as outliers from the mean scaling relations between M_(HI)/M★ and other galaxy properties. We have fitted a plane to the two-dimensional relation between the H I mass fraction, stellar surface mass density and NUV−r colour. Interesting outliers from this plane include gas-rich red sequence galaxies that may be in the process of regrowing their discs, as well as blue, but gas-poor spirals.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

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Citations in the corpus

A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION (2012, background): “M∗ relation of the COLD GASS parent sample (Catinella et al. 2010).”
Molecular and atomic gas along and across the main sequence of star-forming galaxies (2016, methodology): “We calculate SFRUV as SFRUV = 6.84× 10 −29LNUV (1) where LNUV is the luminosity in theGALEX NUV band using the photometric measurements derived for the purposes of the GASS survey, uncorrected for dust extinction (Wang et al. 2010; Catinella et al. 2010).”
THE IMPACT OF COLD GAS ACCRETION ABOVE A MASS FLOOR ON GALAXY SCALING RELATIONS (2009, background): “…we learn from all-sky H i surveys (e.g. Zwaan & et al. 2003; Rosenberg & Schneider 2003; Meyer et al. 2004; Giovanelli et al. 2005; Wong et al. 2006; Catinella et al. 2010) that the gas fractions in SFGs vary systematically with stellar mass (e.g. Baldry et al. 2008, and references therein).”
Evolution of the atomic and molecular gas content of galaxies (2013, background): “The Hi content and its relationship with other galaxy properties (such as stellar mass, stellar surface density, color, and concentration) have been quantified for a fairly large, homogeneously selected sample of nearby galaxies by GASS (Galex Arecibo SDSS survey: Catinella et al. 2010, 2012, 2013).”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, methodology): “Late-type galaxies generally have gas fractions that increase with decreasing stellar mass or luminosity (e.g., McGaugh & de Blok 1997; Kannappann 2004, Geha et al. 2006, Baldry et al. 2008, Catinella et al. 2010).”
THE METALLICITY EVOLUTION OF INTERACTING GALAXIES (2011, background): “…current observations suggest that galaxies contain significantly higher gas fractions (Tacconi et al. 2010; Erb et al. 2006b) and suppressed metallicity at fixed galaxy mass (Erb et al. 2006a; Maiolino et al. 2008) or for less–massive gas–rich galaxies in the local universe (Catinella et al. 2010).”
Cold gas properties of the Herschel Reference Survey - II. Molecular and total gas scaling relations (2014, methodology): “…team, who defined and observed a statistically significat sample of nearby massive galaxies in the Hi and CO lines (Mstar & 1010 M⊙) extracted from the SDSS with available UVGALEX data necessary to quantify the star formation activity (Catinella et al. 2010, 2012; Saintonge et al 2011a, 2011b).”
THE SINS/zC-SINF SURVEY of z ∼ 2 GALAXY KINEMATICS: OUTFLOW PROPERTIES (2012, neutral): “For z∼0 normal SFGs with fg ∼0.07 and Σd ∼500 M⊙pc −2 (Catinella et al. 2010), Equation 4 suggests a critical break-out star formation surface density of ∼0.1 M⊙yr −1kpc−2.”
The GALEX Arecibo SDSS Survey - VIII. Final data release. The effect of group environment on the gas content of massive galaxies (2013, methodology): “…galaxies as a func- ⋆ bcatinella@swin.edu.au tion of their star formation, mass and structural properties, and across all environmental densities (e.g. Catinella et al. 2010; Huang et al. 2012), are necessary to explain the variety of systems observed today in the local Universe, and to provide…”
Morphologies of z ∼ 0.7 AGN host galaxies in CANDELS: no trend of merger incidence with AGN luminosity (2014, background): “This corresponds to about 1 per cent of the total gas mass in typical massive galaxies (Catinella et al. 2010; Saintonge et al. 2011).”
Molecular hydrogen abundances of galaxies in the EAGLE simulations (2015, background): “Recently, H2 and H I have been studied in homogeneous samples of relatively massive galaxies by Saintonge et al. (2011) and Catinella et al. (2010), respectively, with the aim of measuring the fundamental relations between the stellar content of galaxies and their cold gas mass.”
Cold gas stripping in satellite galaxies: from pairs to clusters (2016, methodology): “In addition to blind surveys, the GALEX Arecibo SDSS Survey (Catinella et al. 2010) provides the largest complement of targeted observations for a stellar-mass-selected sample, probing almost 1000 galaxies (log M /M ≥ 10) across the entire gas fraction spectrum.”
THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5 ⩽ z < 0.8 IN THE DEEP2/AEGIS SURVEY (2012, background): “This is confirmed by the GASS H I survey at Arecibo of∼ 1000 slightly more distant massive galaxies withM∗ > 1010 M⊙ (Catinella et al. 2010), which shows that the average H I fractions of red sequence galaxies are at least ten times lower than galaxies of similar mass on the star-forming main…”
FORMING REALISTIC LATE-TYPE SPIRALS IN A ΛCDM UNIVERSE: THE ERIS SIMULATION (2011, result): “The H I-tostellar mass ratio, 1.9× 109 M /3.9× 1010 M = 0.049, is equal to the median value observed in the GASS survey (Catinella et al. 2010) for galaxies of comparable stellar mass. Eris’ H I disk extends out to about 15 kpc (6 stellar disk scale lengths), similar to the size of the H I disk of…”
Theoretical Challenges in Galaxy Formation (2016, background): “More massive early-type galaxies typically have significantly lower cold gas fractions, although they are not devoid of cold gas, contrary to the traditional picture (Catinella et al. 2010, Saintonge et al. 2011, Serra et al. 2012, Young et al. 2011).”
The dust scaling relations of the Herschel Reference Survey (2012, background): “…assumptions on the dust properties of the HRS. Recently, Cortese et al. (2011) have shown that the HI scaling relations for the whole HRS are slightly biased towards lower gas content, with respect to the average scaling relation oflocal galaxies (e.g., Catinella et al. 2010; Fabello et al. 2011).”
COLD GASS, an IRAM legacy survey of molecular gas in massive galaxies – I. Relations between H2, H i, stellar content and structural properties (2011, methodology): “9(d) shows that Rmol is an increasing function (r = 0.25) of NUV − r colour for galaxies with detections of both H I and CO. Catinella et al. (2010) reported a strong anticorrelation between H I mass fraction and colour.”
THE ARECIBO LEGACY FAST ALFA SURVEY: THE GALAXY POPULATION DETECTED BY ALFALFA (2012, methodology): “The GASS observing strategy (Catinella et al. 2010) is specifically designed to probe to constantfHI by conducting significantly longer but targeted HI observations.”
PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions (2017, background): “In massive z~0 SFGs the integrated atomic molecular hydrogen content dominates the total mass of the neutral ISM, MHI~2-3 Mmolgas (e.g. Saintonge et al. 2011a and references therein, Catinella et al. 2010, 2013).”
THE IMPACT OF INTERACTIONS, BARS, BULGES, AND ACTIVE GALACTIC NUCLEI ON STAR FORMATION EFFICIENCY IN LOCAL MASSIVE GALAXIES (2012, methodology): “In order to quantify gas scaling relations across the entire galaxy population, the sample selected for gas observations (both HI and CO) is constructed to have a flat M∗ distribution (Catinella et al. 2010; Saintonge et al. 2011a).”