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dc.contributor.authorFaloon, A. J.
dc.contributor.authorWebb, T. M. A.
dc.contributor.authorEllingson, E.
dc.contributor.authorYan, R.
dc.contributor.authorGilbank, David G.
dc.contributor.authorGeach, J. E.
dc.contributor.authorNoble, A. G.
dc.contributor.authorBarrientos, L. F.
dc.contributor.authorYee, H. K. C.
dc.contributor.authorGladders, M.
dc.contributor.authorRichard, J.
dc.date.accessioned2013-06-11T13:30:51Z
dc.date.available2013-06-11T13:30:51Z
dc.date.issued2013-05-10
dc.identifier.citationFaloon , A J , Webb , T M A , Ellingson , E , Yan , R , Gilbank , D G , Geach , J E , Noble , A G , Barrientos , L F , Yee , H K C , Gladders , M & Richard , J 2013 , ' The structure of the merging RCS 231953+00 supercluster at z ~ 0.9 ' , The Astrophysical Journal , vol. 768 , no. 2 , 104 . https://doi.org/10.1088/0004-637X/768/2/104
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 1905430
dc.identifier.otherPURE UUID: 612dbaf4-7d85-43dd-bab0-e2500d643593
dc.identifier.otherWOS: 000318228400007
dc.identifier.otherScopus: 84877056773
dc.identifier.urihttp://hdl.handle.net/2299/10750
dc.description.abstractThe RCS2319+00 supercluster is a massive supercluster at z = 0.9 comprising three optically selected, spectroscopically confirmed clusters separated by <3Mpc on the plane of the sky. This supercluster is one of a few known examples of the progenitors of present-day massive clusters (1015 M ☉ by z ~ 0.5). We present an extensive spectroscopic campaign carried out on the supercluster field resulting, in conjunction with previously published data, in 1961 high-confidence galaxy redshifts. We find 302 structure members spanning three distinct redshift walls separated from one another by ~65Mpc (Δ z = 0.03). The component clusters have spectroscopic redshifts of 0.901, 0.905, and 0.905. The velocity dispersions are consistent with those predicted from X-ray data, giving estimated cluster masses of ~10 14.5-10 14.9 M ☉. The Dressler-Shectman test finds evidence of substructure in the supercluster field and a friends-of-friends analysis identified five groups in the supercluster, including a filamentary structure stretching between two cluster cores previously identified in the infrared by Coppin etal. The galaxy colors further show this filamentary structure to be a unique region of activity within the supercluster, comprised mainly of blue galaxies compared to the ~43%-77% red-sequence galaxies present in the other groups and cluster cores. Richness estimates from stacked luminosity function fits result in average group mass estimates consistent with ~1013 M ☉ halos. Currently, 22% of our confirmed members reside in 1013 M ☉ groups/clusters destined to merge onto the most massive cluster, in agreement with the massive halo galaxy fractions important in cluster galaxy pre-processing in N-body simulation merger tree studiesen
dc.format.extent21
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.subjectRICH CLUSTERS
dc.subjectSEQUENCE CLUSTER SURVEY
dc.subjectSDSS DR7 SUPERCLUSTERS
dc.subjectREDSHIFT SURVEY
dc.subjectCL-1604 SUPERCLUSTER
dc.subjectCOLOR-MAGNITUDE RELATION
dc.subjecttechniques: spectroscopic
dc.subjectGALAXY CLUSTERS
dc.subjectgalaxies: clusters: individual (RCS 231953+0038.0, RCS 232002+0033.4, RCS 231948+0030.1)
dc.subjectLUMINOSITY FUNCTION
dc.subjectgalaxies: high-redshift
dc.subjectDIGITAL SKY SURVEY
dc.subjectRED-SEQUENCE
dc.titleThe structure of the merging RCS 231953+00 supercluster at z ~ 0.9en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionSMUR
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-637X/768/2/104
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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