Red Fraction Among Satellite Galaxies with Disk-like Light Profiles: Evidence for Inflow in the H I Disk
- Creators
- Hester, J. A.
Abstract
The relationships between color, characterized with respect to the g – r red sequence; stellar structure, as determined using the i-band Sérsic index; and group membership are explored using the Sloan Digital Sky Survey (SDSS). The new results place novel constraints on theories of galaxy evolution, despite the strong correlation between color and stellar structure. Observed correlations are of three independent types—those based on stellar structure, on the color of disk-like galaxies, and on the color of elliptical galaxies. Of particular note, the fraction of galaxies residing on the red sequence measured among galaxies with disk-like light profiles is enhanced for satellite galaxies compared to central galaxies. This fraction increases with group mass. When these new results are considered, theoretical treatments of galaxy evolution that adopt a gas accretion model centered on the hot galactic halo cannot consistently account for all observations of disk galaxies. The hypothesis is advanced that inflow within the extended H I disk prolongs star formation in satellite galaxies. When combined with partial ram pressure stripping (RPS) of this disk, this new scenario is consistent with the observations. This is demonstrated by applying an analytical model of RPS of the extended H I disk to the SDSS groups. These results motivate incorporating more complex modes of gas accretion into models of galaxy evolution, including cold mode accretion, an improved treatment of gas dynamics within disks, and disk stripping.
Additional Information
© 2010 The American Astronomical Society. Received 2007 April 25; accepted 2010 July 7; published 2010 August 6. This project was advised by D. N. Spergel and funded by NASA Grant Award NNG04GK55G and NSF Grant 0707731. The author thanks A. Berlind, M. Blanton, and D. Hogg for the use of the SDSS group catalog and for useful discussions. The author also thanks the anonymous referees for useful comments and critiques. Funding for the SDSS has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Korean Scientist Group, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.Attached Files
Published - Hester2010p11426Astrophys_J.pdf
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Additional details
- Eprint ID
- 20215
- Resolver ID
- CaltechAUTHORS:20100929-104219289
- NNG04GK55G
- NASA
- 0707731
- NSF
- Created
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2010-09-29Created from EPrint's datestamp field
- Updated
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2021-11-08Created from EPrint's last_modified field