期刊
ASTROPHYSICAL JOURNAL
卷 750, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/750/2/93
关键词
galaxies: clusters: general; galaxies: clusters: individual (XMM-LSS02182-05102); galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: high-redshift; galaxies: structure
资金
- NASA [NAS5-26555]
- HST [GO-12060]
- NASA through from the Space Telescope Science Institute [GO-12060]
- European Research Council
- Royal Society
- Texas AM University
- George P. and Cynthia Woods Institute for Fundamental Physics and Astronomy
- Science and Technology Facilities Council [ST/G001979/1] Funding Source: researchfish
- STFC [ST/G001979/1] Funding Source: UKRI
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 (less than or similar to 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 similar or equal to 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.
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