The XMM cluster survey:Galaxy morphologies and the color-magnitude relation in XMMXCS J2215.9 - 1738 at z = 1.46

Hilton, Matt and Stanford, S. Adam and Stott, John P. and Collins, Chris A. and Hoyle, Ben and Davidson, Michael and Hosmer, Mark and Kay, Scott T. and Liddle, Andrew R. and Lloyd-Davies, Ed and Mann, Robert G. and Mehrtens, Nicola and Miller, Christopher J. and Nichol, Robert C. and Romer, A. Kathy and Sabirli, Kivanc and Sahlén, Martin and Viana, Pedro T P and West, Michael J. and Barbary, Kyle and Dawson, Kyle S. and Meyers, Joshua and Perlmutter, Saul and Rubin, David and Suzuki, Nao (2009) The XMM cluster survey:Galaxy morphologies and the color-magnitude relation in XMMXCS J2215.9 - 1738 at z = 1.46. The Astrophysical Journal, 697 (1). pp. 436-451. ISSN 0004-637X

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We present a study of the morphological fractions and color-magnitude relation (CMR) in the most distant X-ray selected galaxy cluster currently known, XMMXCS J2215.9 - 1738 at z = 1.46, using a combination of optical imaging data obtained with the Hubble Space Telescope Advanced Camera for Surveys, and infrared data from the Multi-Object Infrared Camera and Spectrograph, mounted on the 8.2 m Subaru telescope. We find that the morphological mix of the cluster galaxy population is similar to clusters at z 1. Within the central 0.5 Mpc, approximately 62% of the galaxies identified as likely cluster members are ellipticals or S0s; and 38% are spirals or irregulars. Therefore, early-type galaxies were already entrenched as the dominant galaxy population in at least some clusters approximately 4.5 Gyr after the big bang. We measure the CMRs for the early-type galaxies, finding that the slope in the z 850-J relation is consistent with that measured in the Coma cluster, some 9 Gyr earlier, although the uncertainty is large. In contrast, the measured intrinsic scatter about the CMR is more than three times the value measured in Coma, after conversion to rest-frame U - V. From comparison with stellar population synthesis models, the intrinsic scatter measurements imply mean luminosity-weighted ages for the early-type galaxies in J2215.9 - 1738 of 3 Gyr, corresponding to the major epoch of star formation coming to an end at z f 3-5. We find that the cluster exhibits evidence of the "downsizing" phenomenon: the fraction of faint cluster members on the red sequence expressed using the Dwarf-to-Giant Ratio (DGR) is 0.32 0.18 within a radius of 0.5R 200. This is consistent with extrapolation of the redshift evolution of the DGR seen in cluster samples at z <1. In contrast to observations of some other z > 1 clusters, we find a lack of very bright galaxies within the cluster.

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Journal Article
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The Astrophysical Journal
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17 Jan 2017 14:30
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22 Nov 2022 04:17