The X-ray brightest clusters of galaxies from the Massive Cluster Survey

By H. Ebeling, A. Edge, A. Mantz, E. Barrett, J. Henry, C. J. Ma, L. Speybroeck. 2010

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We present a statistically complete sample of very X-ray luminous galaxy clusters detected in the MAssive Cluster Survey (MACS). This second MACS release comprises all 34 MACS clusters with nominal X-ray fluxes in excess of 2 x 10 -12 erg s -1 cm -2 (0.1-2.4 keV) in the ROSAT Bright Source Catalogue; two-thirds of them are new discoveries. Extending over the redshift range from 0.3 to 0.5, this subset complements the complete sample of the 12 most distant MACS clusters (z > 0.5) published in 2007 and further exemplifies the efficacy of X-ray selection for the compilation of samples of intrinsically massive galaxy clusters. Extensive follow-up observations with Chandra/ACIS led to three additional MACS cluster candidates being eliminated as (predominantly) X-ray point sources. For another four clusters - which, however, remain in our sample of 34 - the point-source contamination was found to be about 50 per cent. The median X-ray luminosity of 1.3 x 10 45 erg s -1 (0.1-2.4 keV, Chandra, within r 500 ) of the clusters in this subsample demonstrates the power of the MACS strategy to find the most extreme and rarest clusters out to significant redshift. A comparison of the optical and X-ray data for all clusters in this release finds a wide range of morphologies with no obvious bias in favour of either relaxed or merging systems.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/33249cfdb256f6a47df9a4cf338fa15ddc428415

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CLASH: THE ENHANCED LENSING EFFICIENCY OF THE HIGHLY ELONGATED MERGING CLUSTER MACS J0416.1−2403 (2012, background): “M0416 was listed as a MACS cluster (MAssive Cluster Survey, see Ebeling et al. 2010) due to its X-ray brightness.”
Evidence for Significant Growth in the Stellar Mass of Brightest Cluster Galaxies over the Past 10 Billion Years (2012, methodology): “To increase the number of clusters in Stott et al. (2008) with mass measurements, we use the X-ray temperatures (Ebeling et al. 2007, 2010) and the X-ray luminosities (Ebeling et al. 1996, 1998, 2000) of these clusters (the luminosities were corrected for the cosmology used in this paper) and the…”
The MCXC: a meta-catalogue of x-ray detected clusters of galaxies (2010, background): “A further complete subsample of bright objects in the 0.3 < z < 0.5 redshift range (theMACS BRIGHT sub-catalogue, 34 clusters) are given in Ebeling et al. (2010).”
Weighing the Giants – III. Methods and measurements of accurate galaxy cluster weak-lensing masses (2012, background): “2004; Burenin et al. 2007; Ebeling et al. 2010), the uncertainty in the absolute mass calibration of the survey proxy, which is of the order≈ 15%, dominates the systematic uncertainty on the matter power spectrum normalizationσ8 (Mantz et al. 2010a; Vikhlinin et al. 2009b).”
HUBBLE SPACE TELESCOPE COMBINED STRONG AND WEAK LENSING ANALYSIS OF THE CLASH SAMPLE: MASS AND MAGNIFICATION MODELS AND SYSTEMATIC UNCERTAINTIES (2014, background): “We often also abbreviate Abell clusters (e.g., Abell et al. 1989) with “A,” and MACS clusters (MAssive Cluster Survey; e.g., Ebeling et al. 2001, 2010) with “M,” etc.”
ARE ULTRA-FAINT GALAXIES AT z = 6–8 RESPONSIBLE FOR COSMIC REIONIZATION? COMBINED CONSTRAINTS FROM THE HUBBLE FRONTIER FIELDS CLUSTERS AND PARALLELS (2015, methodology): “Most notably, using a set of ∼ 180 and ∼ 200 multiple images in A2744 and MACS0416, respectively, Jauzac et al. (2015, 2014) reconstructed the projected cluster mass down to a precision of ∼ 1%, which represents a significant improvement over pre-HFF mass models.”
CLASH: WEAK-LENSING SHEAR-AND-MAGNIFICATION ANALYSIS OF 20 GALAXY CLUSTERS (2014, methodology): “The CLASH sample is drawn largely from the Abell and MACS cluster catalogs (Abell 1958; Abell et al. 1989; Ebeling et al. 2001, 2007, 2010).”
The Observed Growth of Massive Galaxy Clusters II: X-ray Scaling Relations (2009, background): “Our data are drawn from three wide-area cluster samples derived from the ROSAT All-Sky Survey (RASS; Trümper 1993): 1 Throughout this paper, we refer to ‘selection effects’ or ‘selection biases’ relative to a mass-limited sample, since we are primarily interested in deriving scaling relations as a ”
The SPTpol Extended Cluster Survey (2019, background): “…al. 2018; Gonzalez et al. 2019), as sources of extended extragalactic emission at X-ray wavelengths (e.g., Gioia et al. 1990; Böhringer et al. 2004; Ebeling et al. 2010; Piffaretti et al. 2011; Mehrtens et al. 2012; Liu et al. 2015b; Adami et al. 2018; Klein et al. 2019), and via their…”
JOINT ANALYSIS OF CLUSTER OBSERVATIONS. II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES (2012, methodology): “Using the LX–TX relation, we find that our sample is consistent with being randomly drawn from the same parent population as samples with well-understood selection functions, such as HIFLUGCS (Reiprich & Böhringer 2002) and MACS (Ebeling et al. 2010).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “Using gravitational lensing data to estimate the dark matter column densities through these clusters, Markevitch et al. (2004) and Bradač et al. (2008a) use the observed dark matter and X-ray peak separations to derive limits on the velocity-independent dark matter self-interaction cross-section pe”
The Observed Growth of Massive Galaxy Clusters I: Statistical Methods and Cosmological Constraints (2009, methodology): “…ROSAT-ESO Flux-Limited X-ray sample (REFLEX; Böhringer et al. 2004) and the bright subsample of the Massive Cluster Survey (Bright MACS; Ebeling, Edge & Henry 2001; Ebeling et al. 2010) – we select a statistically complete sample of 238 X-ray luminous clusters covering the redshift range z < 0.5.”
X-ray–optical classification of cluster mergers and the evolution of the cluster merger fraction (2011, methodology): “We note that, contrary to the previous MACS releases (Ebeling et al. 2007, 2010), this set of 24 does not represent a statistically complete subsample.”
THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, methodology): “The CLASH sample is drawn heavily from the Abell and MACS cluster catalogs (Abell 1958; Abell et al. 1989; Ebeling et al. 2001, 2007, 2010).”
Active galactic nuclei: what’s in a name? (2017, background): “The hot-gas component can be up-to LX ≈ 1041–1042 erg s−1 from galaxies (e.g. Boroson et al. 2011; Mineo et al. 2012b) and can be as high as LX ≈ 1044–1045 erg s−1 in the cores of massive galaxy clusters (e.g. Stanek et al. 2006; Ebeling et al. 2010).”
Weighing the giants – IV. Cosmology and neutrino mass (2014, methodology): “As in M10a,b, the cluster samples used here are based on the BCS (Ebeling et al. 1998), REFLEX (Böhringer et al. 2004), and Bright MACS (Ebeling et al. 2010) catalogs, themselves compiled from the ROSAT All-Sky Survey (RASS; Trümper 1993).”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, methodology): “…of a dedicated program (Donovan 2007) to image clusters selected from two cluster samples constructed from the Rosat All Sky Survey (RASS, Truemper 1993), namely the MAssive Cluster Survey (MACS; Ebeling et al. 2001, 2007, 2010) and the Brightest Cluster Survey (BCS; Ebeling et al. 1998, 2000).”
RELICS: Reionization Lensing Cluster Survey (2019, background): “…et al. 1990); the ROSAT X-ray All-Sky Galaxy Cluster Survey (RXC; Ebeling et al. 1998, 2000a); the ROSAT MAssive Cluster Survey (MACS and SMACS; Ebeling et al. 2001, 2007, 2010, 2013; Mann & Ebeling 2012; Repp et al. 2016; Repp & Ebeling 2018); an extended radio source 2…”