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What turns galaxies off? The different morphologies of star-forming and quiescent galaxies since z~2 from CANDELS | Eric F. Bell
; Arjen van der Wel
; Casey Papovich
; Dale Kocevski
; Jennifer Lotz
; Daniel H. McIntosh
; Jeyhan Kartaltepe
; S. M. Faber
; Harry Ferguson
; Anton Koekemoer
; Norman Grogin
; Stijn Wuyts
; Edmond Cheung
; Christopher J. Conselice
; James S. Dunlop
; Mauro Giavalisco
; Jessica Herrington
; David Koo
; Elizabeth J. McGrath
; Duilia de Mello
; Hans-Walter Rix
; Aday R. Robaina
; Christina C. Williams
; | Date: |
17 Oct 2011 | Abstract: | We use HST/WFC3 imaging from the CANDELS multicycle treasury survey, in
conjunction with the SDSS, to explore the evolution of galactic structure for
galaxies with stellar masses M*>3e10M_sun from z=2.2 to the present epoch, a
time span of 10 Gyr. We explore the rest-frame optical colors, stellar mass,
star formation (SF) activity and the structural parameters of galaxies. We
confirm the dramatic evolution from z=2.2 to the present day in the number
density of non-star-forming galaxies above 3e10M_sun reported by other authors.
The vast majority of these quiescent systems have concentrated light profiles,
as parameterized by the Sersic index, and the population of concentrated
galaxies grows similarly rapidly. We examine the joint distribution of SF
activity, Sersic index, stellar mass, mass divided by radius (a proxy for
velocity dispersion), and stellar surface density. Quiescence correlates poorly
with stellar mass at all z<2.2 (given the <0.2dex scatter between halo mass and
stellar mass at z~0 inferred by More et al. 2009; MNRAS, 392, 801, this argues
against halo mass being the only factor determining quiescence). Quiescence
correlates better with Sersic index, ’velocity dispersion’ and stellar surface
density, where Sersic index correlates the best (increasingly so at lower
redshift). Yet, there is significant scatter between quiescence and galaxy
structure: while the vast majority of quiescent galaxies have prominent bulges,
many of them have significant disks, and a number of bulge-dominated galaxies
have significant SF. Noting the rarity of quiescent galaxies without prominent
bulges, we argue that a prominent bulge (and, perhaps by association, a
supermassive black hole) is a necessary but not sufficient condition for
quenching SF on galactic scales over the last 10Gyr; such a result is
qualitatively consistent with the expectations of the AGN feedback paradigm. | Source: | arXiv, 1110.3786 | Services: | Forum | Review | PDF | Favorites |
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