Discovery of an X-Ray-luminous Galaxy Cluster at z = 1.4

By C. Mullis, Piero Rosati, G. Lamer, H. Böhringer, A. Schwope, P. Schuecker, R. Fassbender. 2005

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We report the discovery of a massive, X-ray-luminous cluster of galaxies at z = 1.393, the most distant X-ray-selected cluster found to date. XMMU J2235.3-2557 was serendipitously detected as an extended X-ray source in an archival XMM-Newton observation of NGC 7314. VLT FORS2 R- and z-band snapshot imaging reveals an overdensity of red galaxies in both angular and color spaces. The galaxy enhancement is coincident in the sky with the X-ray emission; the cluster red sequence at R-z ≃ 2.1 identifies it as a high-redshift candidate. Subsequent FORS2 multiobject spectroscopy unambiguously confirms the presence of a massive cluster based on 12 concordant redshifts in the interval 1.38 < z < 1.40. The preliminary cluster velocity dispersion is 762 ± 265 km s-1. VLT ISAAC Ks- and J-band images underscore the rich distribution of red galaxies associated with the cluster. Based on a 45 ks XMM-Newton observation, we find that the cluster has an aperture-corrected unabsorbed X-ray flux of fX = (3.6 ± 0.3) × 10-14 ergs cm-2 s-1, a rest-frame X-ray luminosity of LX = (3.0 ± 0.2) × 1044 h ergs s-1 (0.5-2.0 keV), and a temperature of kT = 6.0 keV. Though XMMU J2235.3-2557 is likely the first confirmed z > 1 cluster found with XMM-Newton, the relative ease and efficiency of discovery demonstrates that it should be possible to build large samples of z > 1 clusters through the joint use of X-ray and large ground-based telescopes.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a75e1fcf65757425d14b970b5f25e9fca10fe6bc

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Citations in the corpus

The XMM Cluster Survey:Optical analysis methodology and the first data release (2011, unknown): “4−255742.1 at z = 1.39 (Mullis et al. 2005; Rosati et al. 2009; Jee et al. 2009).”
The XMM Cluster Survey: A Massive Galaxy Cluster at z = 1.45 (2006, methodology): “The number of known clusters at z > 1 is currently small (≃ 10 with X-ray confirmation: e.g. Stanford et al. 2001, 2002; Rosati et al. 2004; Mullis et al. 2005), but growing rapidly thanks to new surveys being carried out in the X-ray (e.g. Romer et al. 2001; Mullis et al. 2005; 1 University of…”
THE ERA OF STAR FORMATION IN GALAXY CLUSTERS (2013, background): “3-2557 at z = 1.39 (Mullis et al. 2005; Rosati et al. 2009) and SPT-CL J2040-4451 at z = 1.48 (Bayliss et al. 2013), with masses of ∼ 9 × 1014 M⊙, ∼ 6 × 10 14 M⊙ and ∼ 6 × 10 14 M⊙, respectively, should no longer be experiencing efficient merging due to their high in situ velocity dispersions.”
The X-Ray Luminosity-Mass Relation for Local Clusters of Galaxies (2006, background): “…are currently known, the number will grow considerably in the next five years, as a result of improved search techniques using multi-band optical (Gladders & Yee 2005) combined with infrared (Stanford et al. 2005) or X-ray (Rosati et al. 1998; Romer et al. 2000; Mullis et al. 2005) imaging.”
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).”
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).”
A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62 (2010, background): “Few clusters have confirmed redshifts beyondz∼ 1.3 (e.g., Mullis et al. 2005; Stanford et al. 2005; Brodwin et al. 2006; Stanford et al. 2006; Eisenhardt et al. 2008; Kurk et al. 2009; Wilson et al. 2009).”
THE ATACAMA COSMOLOGY TELESCOPE: ACT-CL J0102−4915 “EL GORDO,” A MASSIVE MERGING CLUSTER AT REDSHIFT 0.87 (2011, unknown): “3−2557 (Mullis et al. 2005; Rosati et al. 2009) at z = 1.393 and XMMXCS J2215.”
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 GMBCG GALAXY CLUSTER CATALOG OF 55,424 RICH CLUSTERS FROM SDSS DR7 (2010, background): “It has been shown that red-sequence galaxies exist in clusters of varied richness and extend to redshift z ∼ 1.6 (Bower et al. 1992; Smail et al. 1998; Barrientos 1999; Mullis et al. 2005; Eisenhardt et al. 2005; Papovich et al. 2010).”
Searching for cool core clusters at high redshift (2008, methodology): “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).”
Scaling relations for galaxy clusters in the Millennium-XXL simulation (2012, background): “…repeatedly been suggested to be in tension with the standard ΛCDM model, possibly providing evidence for non-Gaussian initial density perturbations (Mullis et al. 2005; Hoyle et al. 2011; Foley et al. 2011; Brodwin et al. 2010; Baldi & Pettorino 2011; Menanteau et al. 2012; Hoyle et al. 2012, but…”
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).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, unknown): “3-2557 at z ∼ 1.4 (Mullis et al. 2005; Rosati et al. 2009) and SPT-CLJ05465345 at z ∼ 1.1.”
The XMM-Newton Wide-Field Survey in the COSMOS Field. I. Survey Description (2006, unknown): “The highest redshift is at z∼1.4 (Mullis et al. 2005).”
Hubble Space Telescope and Spitzer Imaging of Red and Blue Galaxies at z ~ 2.5: A Correlation between Size and Star Formation Activity from Compact Quiescent Galaxies to Extended Star-forming Galaxies (2007, background): “…with little ongoing star formation and dust, although the fraction of blue late-type galaxies in clusters increases with redshift (e.g., Blakeslee et al. 2003; Toft et al. 2004; Bell et al. 2004; McIntosh et al. 2005; Lidman et al. 2004;Mullis et al. 2005; Cooper et al. 2007; Cassata et al. 2007).”
Protoclusters associated with z > 2 radio galaxies - I. Characteristics of high redshift protoclusters (2006, background): “Several studies of massive clusters with redshifts up to z= 1.4 have found little evolution in the cluster properties (e.g., Tozzi et al., 2003; Hashimoto et al., 2004; Maughan et al., 2004; Rosati et al., 2004; Mullis et al., 2005).”
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).”
Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, background): “Presently, the highest redshift clusters known to be dominated by old, massive ETGs are at z ≃ 1.4 (Stanford et al. 2005, Mullis et al. 2005).”