Cibinel, A, Carollo, C M, Lilly, S J, Bonoli, S, Miniati, F, Pipino, A, Silverman, J D, van Gorkom, J, Cameron, Ewan, Finoguenov, A, Norberg, P, Peng, Y and Rudick, C S (2013) The Zurich Environmental Study (ZENS) of galaxies in groups along the cosmic web. III. Galaxy photometric measurements and the spatially-resolved color properties of early- and late-type satellites in diverse environments. The Astrophysical Journal, 777 (116). ISSN 1538-4357

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Abstract

We present photometric measurements for the galaxies—and when possible their bulges and disks—in the 0.05 < z < 0.0585 groups of the Zurich Environmental Study (ZENS); these measurements include (B – I) colors, color gradients and maps, color dispersions, as well as stellar masses and star formation rates. The ZENS galaxies are classified into quenched, moderately star-forming, and strongly star-forming using a combination of spectral features and far-UV-to-optical colors; this approach optimally distinguishes quenched systems from dust-reddened star-forming galaxies. The latter contribute up to 50% to the (B – I) "red sequence" at ~1010 M ☉. At fixed morphological or spectral type, we find that galaxy stellar masses are largely independent of environment, and especially of halo mass. As a first utilization of our photometric database, we study, at fixed stellar mass and Hubble type, how (B – I) colors, color gradients, and color dispersion of disk satellites depend on group mass M GROUP, group-centric distance R/R 200, and large-scale structure overdensity δLSS. The strongest environmental trend is found for disk-dominated satellites with M GROUP and R/R 200. At M lsim 1010 M ☉, disk-dominated satellites are redder in the inner regions of the groups than in the outer parts. At M gsim 1010 M ☉, these satellites have shallower color gradients in higher mass groups and in the cores of groups compared with lower mass groups and the outskirts of groups. Stellar population analyses and semi-analytic models suggest that disk-dominated satellites undergo quenching of star formation in their outer disks, on timescales τquench ~ 2 Gyr, as they progressively move inside the group potential.

Item Type:	Article
Schools and Departments:	School of Mathematical and Physical Sciences > Physics and Astronomy
Depositing User:	Anna Cibinel
Date Deposited:	17 Jul 2015 15:50
Last Modified:	02 Jul 2019 23:45
URI:	http://sro.sussex.ac.uk/id/eprint/55414

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