The Ages of Passive Galaxies in a z = 1.62 Protocluster

We present a study of the relation between galaxy stellar age and mass for 14 members of the z = 1.62 protocluster IRC 0218, using multiband imaging and HST G102 and G141 grism spectroscopy. Using UVJ colors to separate galaxies into star-forming and quiescent populations, we find that, at stellar m...

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Bibliographic Details
Published in:The Astrophysical journal 2017-07, Vol.844 (1), p.43
Main Authors: Lee-Brown, Donald B., Rudnick, Gregory H., Momcheva, Ivelina G., Papovich, Casey, Lotz, Jennifer M., Tran, Kim-Vy H., Henke, Brittany, Willmer, Christopher N. A., Brammer, Gabriel B., Brodwin, Mark, Dunlop, James, Farrah, Duncan
Format: Article
Language:English
Subjects:
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COMPARATIVE EVALUATIONS
Galactic clusters
GALACTIC EVOLUTION
GALAXIES
galaxies: clusters: individual (CLG 0218.3-0510)
galaxies: evolution
galaxies: high-redshift
galaxies: star formation
GALAXY CLUSTERS
MASS
RED SHIFT
SPECTROSCOPY
Spectrum analysis
Star formation
STARS
Stars & galaxies
Stellar age
Stellar mass
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Summary:We present a study of the relation between galaxy stellar age and mass for 14 members of the z = 1.62 protocluster IRC 0218, using multiband imaging and HST G102 and G141 grism spectroscopy. Using UVJ colors to separate galaxies into star-forming and quiescent populations, we find that, at stellar masses , the quiescent fraction in the protocluster is , consistent with a ∼ 2× enhancement relative to the field value, . At masses , fQ in the cluster is , consistent with the field value of . Using galaxy values derived from the G102 spectroscopy, we find no relation between galaxy stellar age and mass. These results may reflect the impact of merger-driven mass redistribution-which is plausible, as this cluster is known to host many dry mergers. Alternately, they may imply that the trend in fQ in IRC 0218 was imprinted over a short timescale in the protocluster's assembly history. Comparing our results with those of other high-redshift studies and studies of clusters at , we determine that our observed relation between fQ and stellar mass only mildly evolves between and , and only at stellar masses . Both the and results are in agreement that the red sequence in dense environments was already populated at high redshift, , placing constraints on the mechanism(s) responsible for quenching in dense environments at .
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aa7948