Please note that eDoc will be permanently shut down in the first quarter of 2021!      Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          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
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
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.