Hilton, Matt, Stanford, S Adam, Stott, John P, Collins, Chris A, Hoyle, Ben, Davidson, Michael, Hosmer, Mark, Kay, Scott T, Liddle, Andrew R, Lloyd-Davies, Edward, Mann, Robert G, Mehrtens, Nicola, Miller, Christopher J, Nichol, Robert C, Romer, A Kathy, Sabirli, Kivanc, Sahlén, Martin, Viana, Pedro T P, West, Michael J, Barbary, Kyle, Dawson, Kyle S, Meyers, Joshua, Perlmutter, Saul, 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. 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 similar to 1. Within the central 0.5 Mpc, approximately similar to 62% of the galaxies identified as likely cluster members are ellipticals or S0s; and similar to 38% are spirals or irregulars. Therefore, early-type galaxies were already entrenched as the dominant galaxy population in at least some clusters approximately similar to 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 similar to 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 approximate to 3 Gyr, corresponding to the major epoch of star formation coming to an end at z(f) approximate to 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.

Item Type: Article
Schools and Departments: School of Mathematical and Physical Sciences > Physics and Astronomy
Depositing User: Mark Hosmer
Date Deposited: 06 Feb 2012 19:29
Last Modified: 26 Jan 2018 12:24
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