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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 660760.0, MPI für Astronomie / Publikationen_mpia
CANDELS observations of the structural properties of cluster galaxies at z = 1.62
Authors:Papovich, C.; Bassett, R.; Lotz, J. M.; van der Wel, A.; Tran, K. -. V.; Finkelstein, S. L.; Bell, E. F.; Conselice, C. J.; Dekel, A.; Dunlop, J. S.; Guo, Y.; Faber, S. M.; Farrah, D.; Ferguson, H. C.; Finkelstein, K. D.; Häussler, B.; Kocevski, D. D.; Koekemoer, A. M.; Koo, D. C.; McGrath, E. J.; McLure, R. J.; McIntosh, D. H.; Momcheva, I.; Newman, J. A.; Rudnick, G.; Weiner, B.; Willmer, C. N. A.; Wuyts, S.
Date of Publication (YYYY-MM-DD):2012
Journal Abbrev.:The Astrophysical Journal
Volume:750
Issue / Number:2
Start Page:id. 93
Audience:Not Specified
Abstract / Description:We discuss the structural and morphological properties of galaxies in a z = 1.62 proto-cluster using near-IR imaging data from Hubble Space Telescope Wide Field Camera 3 data of the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). The cluster galaxies exhibit a clear color-morphology relation: galaxies with colors of quiescent stellar populations generally have morphologies consistent with spheroids, and galaxies with colors consistent with ongoing star formation have disk-like and irregular morphologies. The size distribution of the quiescent cluster galaxies shows a deficit of compact (lsim 1 kpc), massive galaxies compared to CANDELS field galaxies at z = 1.6. As a result, the cluster quiescent galaxies have larger average effective sizes compared to field galaxies at fixed mass at greater than 90% significance. Combined with data from the literature, the size evolution of quiescent cluster galaxies is relatively slow from z ~= 1.6 to the present, growing as (1 + z)-0.6 ± 0.1. If this result is generalizable, then it implies that physical processes associated with the denser cluster region seem to have caused accelerated size growth in quiescent galaxies prior to z = 1.6 and slower subsequent growth at z < 1.6 compared to galaxies in the lower density field. The quiescent cluster galaxies at z = 1.6 have higher ellipticities compared to lower redshift samples at fixed mass, and their surface-brightness profiles suggest that they contain extended stellar disks. We argue that the cluster galaxies require dissipationless (i.e., gas-poor or "dry") mergers to reorganize the disk material and to match the relations for ellipticity, stellar mass, size, and color of early-type galaxies in z < 1 clusters.
Free Keywords:galaxies: clusters: general; galaxies: clusters: individual: XMM-LSS02182-05102; galaxies: elliptical and lenticular; cD; galaxies: evolution; galaxies: high-redshift; galaxies: structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://cdsads.u-strasbg.fr/abs/2012ApJ...750...93P
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