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PRODID:-//AT Content Types//AT Event//EN
VERSION:1.0
BEGIN:VEVENT
DTSTART:20120611T180000Z
DTEND:20120611T185500Z
DCREATED:20120601T145612Z
UID:ATEvent-4b19a41cfde94e3eb82262077a6b00ff
SEQUENCE:0
LAST-MODIFIED:20120608T150650Z
SUMMARY:cosmology seminar\: Andrew Wetzel\, Yale
DESCRIPTION:Title\:\nGalaxy evolution in groups and clusters\n\nAbstra
 ct\:\nSatellite galaxies in groups and clusters are more likely to hav
 e low star formation rates (SFR) and lie on the `red-sequence' than ce
 ntral (`field') galaxies. Using galaxy group/cluster catalogs from the
  Sloan Digital Sky Survey\, I examine in detail the SFR distribution o
 f satellite galaxies and its dependence on satellite mass\, halo mass\
 , and halo-centric radius. Using a high-resolution\, cosmological N-bo
 dy simulation to track satellite orbits\, I constrain the star formati
 on histories of satellites that fit these observed dependencies\, demo
 nstrating a `delayed-then-rapid' quenching scenario\: satellite SFRs e
 volve unaffected for 2 - 4 Gyr after infall\, after which star formati
 on quenches rapidly\, with an e-folding time of < 0.8 Gyr. These quenc
 hing timescales are shorter for more massive satellites but do not dep
 end on host halo mass\: the observed increase in satellite quiescent f
 raction with halo mass arises simply because of group preprocessing. B
 ecause of the long time delay before quenching starts\, satellites exp
 erience significant stellar mass growth after infall\, nearly identica
 l to central galaxies. Finally\, I discuss the the connection of these
  results to satellite gas accretion\, consumption\, and stripping\, as
  well as implications for the subhalo abundance matching technique.
LOCATION:355 Varian
PRIORITY:3
TRANSP:0
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