Other
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21721305r&link_type=abstract
American Astronomical Society, AAS Meeting #217, #213.05; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
One of galaxy evolution's most long-standing problems is determining how clusters affect the properties of infalling galaxies. One useful metric for this is how quickly the passive galaxy population in clusters assembles over time. Standard practice has been to assume that all red sequence galaxies are passive and to measure the evolution in the red fraction and red sequence luminosity function over time. This approach, however, neglects the possible contribution of dusty galaxies to the red sequence, which can be significant at intermediate environment and low to intermediate stellar masses. We move beyond a simple red sequence cut by using a new multi-color technique to distinguish red passive galaxies from red dusty star-forming galaxies. Isolating passive galaxies is inherently more physical than studying galaxies selected on one color alone. We track the buildup of passive galaxies in the field and in clusters using the COSMOS data for the former and a large imaging and spectroscopy survey of intermediate redshift clusters for the latter. The fraction of passive galaxies in clusters increases with increasing galaxy mass, increasing cluster velocity dispersion, and with time at a fixed mass and velocity dispersion. We relate the passive fraction in clusters to that for field galaxies of similar masses and use this to constrain the processes that shut off star formation in infalling cluster galaxies. The fraction of dust-obscured star forming galaxies changes with stellar mass and environment and this affects the interpretation of the rapid evolution in the faint red sequence galaxy population and its environmental dependence, as seen in other works.
Jablonka Pascale
Moustakas John
Rudnick Gregory
van der Wel Arjen
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