Other
Scientific paper
Jan 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21940603b&link_type=abstract
American Astronomical Society, AAS Meeting #219, #406.03
Other
Scientific paper
We use HST/WFC3 imaging from the CANDELS multicycle treasury survey, in conjunction with the Sloan Digital Sky Survey, to explore the evolution of galactic structure for galaxies with stellar masses in excess of 3x10^10 solar masses from z=2.2 to z=0, a time span of 10Gyr. We explore the relationship between stellar mass, star formation activity and the structural parameters of galaxies as determined from parametric fits to the surface brightness profiles of galaxies. We confirm the dramatic evolution from z=2.2 to the present day in the number of non star-forming galaxies above 3x10^10 solar masses reported by other authors --- we find that the vast majority of these quiescent systems have concentrated light profiles, as parametrized in this work using galaxy Sersic index, and the population of concentrated galaxies grows similarly rapidly. We examine the joint distribution of star formation activity, Sersic index, stellar mass, M/R (a proxy for velocity dispersion) and stellar surface density. Quiescence correlates poorly with stellar mass at all z<2.2 given the <0.2 dex scatter between halo mass and stellar mass at z 0 inferred by More et al. 2011; MNRAS,410,210, this argues against halo mass being the only factor determining quiescence). Quiescence correlates most tightly with Sersic index, and correlates well with 'velocity dispersion' and stellar surface density. Yet, there is significant scatter in any of these correlations: a fraction of systems with high Sersic index form stars, and some quiescent galaxies have significant disks. Noting the rarity of quiescent galaxies without prominent bulges, we suggest that a prominent bulge (and, perhaps by association, a supermassive black hole) is a necessary but not sufficient condition for quenching star formation over the last 10Gyr; such a result is qualitatively consistent with the expectations of the AGN feedback paradigm. This work is supported by HST grant GO-12060.
Bell Eric F.
CANDELS Team
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