Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 452, Issue 3, Pages 2479-2489Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv1311
Keywords
galaxies: evolution; galaxies: fundamental parameters; galaxies: ISM; galaxies: photometry; radio lines: galaxies
Categories
Funding
- Australian Research Council Future Fellowship [FT120100660]
- Australian Research Council's Discovery Projects [DP130100664, DP150101734]
- NSF [AST 1107390]
- Brinson Foundation
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica de Canarias
- 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
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1107390] Funding Source: National Science Foundation
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We revisit the main HI-to-stellar mass ratio (gas fraction) scaling relations, taking advantage of the H I spectral stacking technique to understand the dependence of gas content on the structural and star formation properties of nearby galaxies. This work uses a volume-limited, multiwavelength sample of similar to 25 000 galaxies, selected according to stellar mass (10(9) M-circle dot <= M-star = 10(11.5) M-circle dot) and redshift (0.02 <= z <= 0.05) from the Sloan Digital Sky Survey, and with HI data from the Arecibo Legacy Fast ALFA survey. We bin according to multiple parameters of galaxies spanning the full gas-poor to -rich regime in order to disentangle the dominance of different components and processes in influencing gas content. For the first time, we show that the scaling relations of gas fraction with stellar mass and stellar surface density are primarily driven by a combination of the underlying galaxy bimodality in specific star formation rate and the integrated Kennicutt-Schmidt law. Finally, we produce tentative evidence that the time-scales of HI depletion are dependent upon galaxy mass and structure, at fixed specific star formation rate.
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