Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:0903.1731)
· On-line Data
· References in the article
· Citations to the Article (4) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (9)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The XMM Cluster Survey: Galaxy Morphologies and the Color-Magnitude Relation in XMMXCS J2215.9 - 1738 at z = 1.46
Authors:
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, Ed; 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; Suzuki, Nao
Affiliation:
AA(Astrophysics & Cosmology Research Unit, School of Mathematical Sciences, University of KwaZulu-Natal, Private Bag X54001, Durban 4000, South Africa ; South African Astronomical Observatory, P.O. Box 9, Observatory, 7935, Cape Town, South Africa ; Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK ; ), AB(University of California, Davis, CA 95616, USA ; Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, Livermore, CA 94551, USA ), AC(Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK ), AD(Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK ), AE(Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 2EG, UK ), AF(Institute of Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 9HJ, UK ), AG(Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UK ), AH(University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL, UK ), AI(Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UK ), AJ(Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UK ), AK(Institute of Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 9HJ, UK ), AL(Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UK ), AM(Cerro-Tololo Inter-American Observatory, National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA ), AN(Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 2EG, UK ), AO(Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UK ), AP(Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UK ), AQ(Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UK ), AR(Departmento de Matemática Aplicada da Faculdade de Ciências da Universidade do Porto, Rua do Campo Alegre 687, 4169-007, Portugal ; Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal ), AS(European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago 19, Chile ), AT(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA ; Department of Physics, University of California Berkeley, Berkeley, CA 94720-7300, USA ), AU(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), AV(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA ; Department of Physics, University of California Berkeley, Berkeley, CA 94720-7300, USA ), AW(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA ; Department of Physics, University of California Berkeley, Berkeley, CA 94720-7300, USA ), AX(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA ; Department of Physics, University of California Berkeley, Berkeley, CA 94720-7300, USA ), AY(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA )
Publication:
The Astrophysical Journal, Volume 697, Issue 1, pp. 436-451 (2009). (ApJ Homepage)
Publication Date:
05/2009
Origin:
IOP
ApJ Keywords:
galaxies: clusters: individual: XMMXCS J2215.9 – 1738, galaxies: elliptical and lenticular, cD, galaxies: evolution, X-rays: galaxies: clusters
DOI:
10.1088/0004-637X/697/1/436
Bibliographic Code:
2009ApJ...697..436H

Abstract

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 zf ≈ 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.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints