Evidence for a change in the dominant satellite galaxy quenching mechanism at z=1

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Balogh , M L , Mcgee , S L , Mok , A , Muzzin , A , van der Burg , R F J , Bower , R G , Finoguenov , A , Hoekstra , H , Lidman , C , Mulchaey , J S , Noble , A , Parker , L C , Tanaka , M , Wilman , D J , Webb , T , Wilson , G & Yee , H K C 2016 , ' Evidence for a change in the dominant satellite galaxy quenching mechanism at z=1 ' , Monthly Notices of the Royal Astronomical Society , vol. 456 , no. 4 , pp. 4364-4376 . https://doi.org/10.1093/mnras/stv2949

Title: Evidence for a change in the dominant satellite galaxy quenching mechanism at z=1
Author: Balogh, Michael L.; Mcgee, Sean L.; Mok, Angus; Muzzin, Adam; van der Burg, Remco F. J.; Bower, Richard G.; Finoguenov, Alexis; Hoekstra, Henk; Lidman, Chris; Mulchaey, John S.; Noble, Allison; Parker, Laura C.; Tanaka, Masayuki; Wilman, David J.; Webb, Tracy; Wilson, Gillian; Yee, Howard K. C.
Contributor: University of Helsinki, Department of Physics
Date: 2016-03-11
Language: eng
Number of pages: 13
Belongs to series: Monthly Notices of the Royal Astronomical Society
ISSN: 0035-8711
URI: http://hdl.handle.net/10138/190712
Abstract: We present an analysis of galaxies in groups and clusters at 0.8 <z <1.2, from the GCLASS and GEEC2 spectroscopic surveys. We compute a 'conversion fraction' f(convert) that represents the fraction of galaxies that were prematurely quenched by their environment. For massive galaxies, M-star > 10(10.3) M-circle dot, we find f(convert) similar to 0.4 in the groups and similar to 0.6 in the clusters, similar to comparable measurements at z = 0. This means the time between first accretion into a more massive halo and final star formation quenching is t(p) similar to 2 Gyr. This is substantially longer than the estimated time required for a galaxy's star formation rate to become zero once it starts to decline, suggesting there is a long delay time during which little differential evolution occurs. In contrast with local observations we find evidence that this delay time-scale may depend on stellarmass, with t(p) approaching t(Hubble) for M-star similar to 10(9.5) M-circle dot. The result suggests that the delay time must not only be much shorter than it is today, but may also depend on stellar mass in a way that is not consistent with a simple evolution in proportion to the dynamical time. Instead, we find the data are well-matched by a model in which the decline in star formation is due to 'overconsumption', the exhaustion of a gas reservoir through star formation and expulsion via modest outflows in the absence of cosmological accretion. Dynamical gas removal processes, which are likely dominant in quenching newly accreted satellites today, may play only a secondary role at z = 1.
Subject: galaxies: clusters: general
galaxies: evolution
SIMILAR-TO 1
STAR-FORMATION RATES
STELLAR MASS FUNCTION
DARK-MATTER HALOS
BRIGHTEST CLUSTER GALAXIES
GEEC2 SPECTROSCOPIC SURVEY
DIGITAL SKY SURVEY
RED-SEQUENCE
REDSHIFT SURVEY
FORMATION HISTORIES
115 Astronomy, Space science
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