The XMM Cluster Survey: A Massive Galaxy Cluster at z = 1.45

By S. Stanford, A. Romer, K. Sabirli, M. Davidson, M. Hilton, P. T. P. Viana, C. Collins, S. Kay, Andrew R. Liddle, R. Mann and 7 more. 2006

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We report the discovery of XMMXCS J2215.9-1738, a massive galaxy cluster at z = 1.45, which was found in the XMM Cluster Survey. The cluster candidate was initially identified as an extended X-ray source in archival XMM data. Optical spectroscopy shows that six galaxies within a ~60'' diameter region lie at z = 1.45 ± 0.01. Model fits to the X-ray spectra of the extended emission yield kT = 7.4 keV (90% confidence); if there is an undetected central X-ray point source, then kT = 6.5 keV. The bolometric X-ray luminosity is LX = 4.4 × 1044 ergs s-1 over a 2 Mpc radial region. The measured TX, which is the highest for any known cluster at z > 1, suggests that this cluster is relatively massive for such a high redshift. The redshift of XMMXCS J2215.9-1738 is the highest currently known for a spectroscopically confirmed cluster of galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fc00e8d46d9076903a7e36b446cbef51cfc65394

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Citations in the corpus

THE SUPERNOVA DELAY TIME DISTRIBUTION IN GALAXY CLUSTERS AND IMPLICATIONS FOR TYPE-Ia PROGENITORS AND METAL ENRICHMENT (2010, background): “Well-measured X-ray temperatures exist in the literature for five of the Barbary et al. sample clusters, and are all around 6-7 keV (Rosati et al. 2004; Stanford et al. 2002, 2006; Boehringer et al. 2008; Gilbank et al. 2008).”
The XMM-Newton Wide-Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies (2006, background): “Only recently distant clusters have started to be identified serendipitously from the Chandra (Boschin, 2002) and XMM archives, with a record-breaking object recently identified at z = 1.45 (Stanford et al. 2006).”
SPECTROSCOPIC CONFIRMATION OF TWO MASSIVE RED-SEQUENCE-SELECTED GALAXY CLUSTERS AT z ∼ 1.2 IN THE SpARCS-NORTH CLUSTER SURVEY (2008, background): “Indeed, X-ray detection of clusters at z > 1 is so challenging that currently the most promising surveys are those searching for clusters serendipitously in the entire XMM-Newton archive (e.g., Romer et al. 2001; Mullis et al. 2005; Stanford et al. 2006; Lamer et al. 2008).”
A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62 (2010, background): “1.5 (e.g., Rosati et al. 2004; Stanford et al. 2006), but X–ray selection typically require relaxed systems, which is unlikely to be the case at high redshifts where cluster progenitors will be less massive and more disordered, with less time for the intracluster medium (ICM) to thermalize (e.g.,…”
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION (2009, background): “Groups and clusters of galaxies, formed through the gravitational collapse of massive dark matter halos, are now readily identified up to redshift one and even beyond (e.g. Stanford et al. 2006; Eisenhardt et al. 2008).”
THE ATACAMA COSMOLOGY TELESCOPE: ACT-CL J0102−4915 “EL GORDO,” A MASSIVE MERGING CLUSTER AT REDSHIFT 0.87 (2011, unknown): “9−1738 (Stanford et al. 2006; Hilton et al. 2009) at z = 1.457.”
An Extreme Protocluster of Luminous Dusty Starbursts in the Early Universe (2017, background): “A ubiquitous feature of galaxy clusters up to ~z 2 is the presence of a strong red sequence produced by massive, passively evolving early-type galaxies, which dominate their cores (see, e.g., Bremer et al. 2006; Stanford et al. 2006; Hilton et al. 2009; Rosati et al. 2009).”
The XMM Cluster Survey:Optical analysis methodology and the first data release (2011, background): “9−1738 taken from Stanford et al. 2006; see Table 2).”
The WIRCam Deep Survey I. Counts, colours, and mass-functions derived from near-infrared imaging in the CFHTLS deep fields (2011, methodology): “This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey,a collaborative project of NRC and CNRS. Mullis et al. 2005; Stanford et al. 2005, 2006; Stott et al. 2010; Fassbender et al. 2011).”
A mature cluster with X-ray emission at z = 2.07 (2010, background): “Indeed,z & 1 X-ray and colourselected structures are spatially compact and dominated by massive early-type galaxies, as their local counterparts (Blakeslee et al. 2003, Mullis et al. 2005, Stanford et al. 2006, Papovich et al. 2010, Tanaka et al. 2010, Henry et al. 2010, Kurk et al. 2009).”
The first appearance of the red sequence of galaxies in proto-clusters at 2 <~ z <~ 3 (2007, background): “…Bower, Lucey, & Ellis 1992), and is well recognised even in distant clusters at least out to z ∼ 1 (e.g., Ellis et al. 1997; ⋆ E-mail: kodama@optik.mtk.nao.ac.jp Kodama et al. 1998; Stanford, Eisenhardt, & Dickinson 1998; van Dokkum et al. 1998; 2001; Blakeslee et al. 2003; Stanford et al. 2006).”
Searching for cool core clusters at high redshift (2008, background): “This massive object is the highest redshift cluster in our sample and the second most distant cluster (Mullis et al. 2005) confirmed to date (the most distant cluster known so far has redshift 1.45 (Stanford et al. 2006).”
THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, background): “These observations include the detection of perhaps unexpectedly massive galaxy clusters at z > 1 (Stanford et al. 2006; Eisenhardt et al. 2008; Jee et al. 2009; Huang et al. 2009; Rosati et al. 2009; Papovich et al. 2010; Schwope et al. 2010; Gobat et al. 2011; Jee et al. 2011; Foley et al. 2011)…”
Clusters of Galaxies in the First Half of the Universe from the IRAC Shallow Survey (2008, unknown): “With the arrival of XMMNewton, X-ray surveys offer renewed promise, leading recently to the identification of galaxy clusters at z ¼ 1:39 (Mullis et al. 2005) and 1.45 (Stanford et al. 2006).”
The realm of the galaxy protoclusters (2016, background): “Focusing instead on their gaseous components as a means of discovering high redshift clusters, existing wide-field X-ray surveys are at the limits of their sensitivity for clusters at about z ∼ 1.5 (Rosati et al., 2002; Mullis et al., 2005; Stanford et al., 2006).”
EVOLUTION OF THE COLOR–MAGNITUDE RELATION IN GALAXY CLUSTERS AT z ∼ 1 FROM THE ACS INTERMEDIATE REDSHIFT CLUSTER SURVEY (2008, background): “…Lucia et al. 2004, 2007; Holden et al. 2004; Lidman et al. 2004; Tanaka et al. 2005; Blakeslee et al. 2006; Cucciati et al. 2006; Franzetti et al. 2007; Homeier et al. 2006; Mei et al. 2006a,b; Stanford et al. 2006; Willmer et al. 2006; Cooper et al. 2007; Tanaka et al. 2007; Arnouts et al. 2008).”