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Please use this identifier to cite or link to this item: http://hdl.handle.net/1959.3/47758
- Title
- Strangulation in galaxy groups
- Author(s)
- Kawata, Daisuke; Mulchaey, John S.
- Abstract
- We use a cosmological chemodynamical simulation to study how the group environment impacts the star formation ( SF) properties of disk galaxies. The simulated group has a total mass of M similar to 8 x 10(12) M-circle dot and a total X-ray, luminosity of L-x similar to 10(41) erg s(-1). Our simulation suggests that ram pressure is not sufficient in this group to remove the cold disk gas from a V-rot similar to 150 km s galaxy. However, the majority of the hot gas in the galaxy is stripped over a timescale of approximately 1 Gyr. Since the cooling of the hot-gas component provides a source for new cold gas, the stripping of the hot component effectively cuts off the supply of cold gas. This in turn leads to a quenching of SF. The galaxy maintains the disk component after the cold gas is consumed, which may lead to a galaxy similar to an S0. Our self-consistent simulation suggests that this strangulation mechanism works even in low-mass groups, providing an explanation for the lower SF rates in group galaxies relative to galaxies in the field.
- Publication type
- Journal article
- Research centre
- Swinburne University of Technology
- Source
- Astrophysical Journal Letters, Vol. 672, no. 2 (Jan 2008), pp. L103-L106
- Publication year
- 2008
- FOR Code(s)
- 0201 Astronomical and Space Sciences; 020103 Cosmology and Extragalactic Astronomy
- Keyword(s)
- Cluster galaxies; Cosmological simulations; Digital sky survey; Disk galaxies; Dynamics; Galaxies; Elliptic galaxies; Evolution; Intracluster medium; Kinematics; Numerical methods; RAM-pressure; S0; Star formation; Statistical properties; Stellar content
- Publisher
- University of Chicago Press
- ISSN
- 0004-637X
- Publisher URL
- http://dx.doi.org/10.1086/526544
- Copyright
- Copyright © 2008 The American Astronomical Society. All rights reserved.
- Additional information
- Additional colour figures supporting this paper are available online at: http://dx.doi.org/10.1086/526544.
- Peer reviewed
