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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



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ID: 421619.0, MPI für Astronomie / Publikationen_mpia
New constraints on the efficiencies of ram pressure stripping and the tidal disruption of satellite galaxies
Authors:Kang, X.; van den Bosch, Frank C.
Language:English
Date of Publication (YYYY-MM-DD):2008
Title of Journal:The Astrophysical Journal
Journal Abbrev.:ApJ
Volume:676
Start Page:L101
End Page:L104
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:Using data from the Sloan Digital Sky Survey (SDSS) it has recently been shown that the red fraction of satellite galaxies increases with stellar mass. Semianalytical models, however, predict red satellite fractions that are independent of stellar mass, and much higher than observed. It has been argued that this discrepancy is due to the fact that the models assume that satellite galaxies are instantaneously stripped of their hot gas reservoirs at the moment they are accreted into a bigger halo. In this Letter we show that the fraction of red satellites can be brought into better agreement with the data by simply decreasing this stripping efficiency. However, this also results in a red fraction of massive centrals that is much too low. This is because the massive centrals now accrete satellite galaxies that are bluer and more gas-rich. However, if a significant fraction of low-mass satellite galaxies is tidally disrupted before being accreted by their central host galaxy, as suggested by recent studies, the red fractions of both centrals and satellites can be reproduced reasonably well. A problem remains with the red fraction of centrals of intermediate mass, which is likely to reflect an oversimplified treatment of AGN feedback.
Free Keywords:Galaxies: Formation; Galaxies: General; Galaxies: Intergalactic Medium
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/abs/2008ApJ...676L.101K [ID No:1]
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