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Table · dataset · 2014

Near-IR observations of XMM-LSS J02182-05102

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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).

Description

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 (<~1kpc), 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^.

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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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Stated by source
Infrared · Optical
Inferred from text
Astronomical sciences 73% · Imaging 75%
Provenance · 1 source records, 11 field assertions
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IVOA Registry (Virtual Observatory)ivo://cds.vizier/j/apj/750/9314 d agoJSON v1
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