Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 466, Issue 4, Pages 4795-4812Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx046
Keywords
galaxies: evolution; galaxies: fundamental parameters; galaxies: groups: general; galaxies: star formation; radio lines: galaxies; ultraviolet: galaxies
Categories
Funding
- Australian Research Council's Discovery Project funding scheme [DP150101734]
- Australian Research Council Future Fellowship [FT120100660]
- Royal Society through the award of a University Research Fellowship
- Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]
- NASA Office of Space Science [NNX09AF08G]
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy Office of Science
- Astrophysical Research Consortium
- 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
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We use deep HI observations obtained as part of the extended GALEX Arecibo SDSS survey (xGASS) to study the cold gas properties of central galaxies across environments. We find that below stellarmasses of 10(10.2) M circle dot, central galaxies in groups have an average atomic hydrogen gas fraction similar to 0.3 dex higher than those in isolation at the same stellar mass. At these stellar masses, group central galaxies are usually found in small groups of N= 2 members. The higher HI content in these low-mass group central galaxies is mirrored by their higher average star formation activity and molecular hydrogen content. At larger stellar masses, this difference disappears and central galaxies in groups have similar (or even smaller) gas reservoirs and star formation activity compared to those in isolation. We discuss possible scenarios able to explain our findings and suggest that the higher gas content in low-mass group central galaxies is likely due to the contributions from the cosmic web or HI-rich minor mergers, which also fuel their enhanced star formation activity.
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