Images, Structural Properties, and Metal Abundances of Galaxy Clusters Observed with Chandra ACIS-I at 0.1 < z < 1.3

By B. Maughan, C. Jones, W. Forman, L. V. Speybroeck. 2007

228 citations recorded by the source corpus.

We have assembled a sample of 115 galaxy clusters at 0.1 < z < 1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z > 0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple β-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z > 0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z = 0.1 and z ≈ 1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z≳ 0.5.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4b9f220a36933ff9b2f88ff45794f542df4b309d

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

The XMM Cluster Survey:Optical analysis methodology and the first data release (2011, result): “16, 17, and 18 we compare the XCS-DR1 redshifts and temperatures (values and errors) to previous data releases that have included X-ray cluster temperatures (Reiprich & Böhringer 2002; Pacaud et al. 2007; Maughan et al. 2008; Vikhlinin et al. 2009; Mantz et al. 2010).”
The EAGLE simulations of galaxy formation: the importance of the hydrodynamics scheme (2015, methodology): “For comparison, we show data from Vikhlinin et al. (2006), Maughan et al. (2008), Sun et al. (2009), Pratt et al. (2009) and Lin et al. (2012).”
Lensing and x-ray mass estimates of clusters (simulations) (2012, unknown): “Following Poole et al. (2006) and Maughan et al. (2008), we define the centroid-shift as w = 1 Rmax × √∑ i(∆i − 〈∆〉)2 (N − 1) , (10) where Rmax is the radius of the largest aperture, and ∆i = ~Rc,i − ~Rc,max is the shift of the centroid in the i−th aperture with respect to the centroid in the…”
THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, background): “The X-ray selected cluster sub-sample also exhibits a lower average ellipticity than our high-magnification (Einstein-radii selected) sample but is consistent with the mean ellipticity of the larger Maughan et al. (2008) sample.”
X-ray–optical classification of cluster mergers and the evolution of the cluster merger fraction (2011, background): “6 shown later; see also Maughan et al. 2008).”
THE SUPERNOVA DELAY TIME DISTRIBUTION IN GALAXY CLUSTERS AND IMPLICATIONS FOR TYPE-Ia PROGENITORS AND METAL ENRICHMENT (2010, background): “However, Maughan et al. (2008) have shown that measuring iron abundances within an annulus that excludes the central 15% in radius reduces the results only mildly, to values still consistent with the canonical ZFe,gas = 0.3.”
HUBBLE SPACE TELESCOPE COMBINED STRONG AND WEAK LENSING ANALYSIS OF THE CLASH SAMPLE: MASS AND MAGNIFICATION MODELS AND SYSTEMATIC UNCERTAINTIES (2014, background): “Although M0429 (z = 0.399) has been subject to various X-ray studies (Schmidt & Allen 2007; Comerford & Natarajan 2007; Maughan et al. 2008; Allen et al. 2008; Mann & Ebeling 2012), we did not find any previous SL, nor WL, analyses for this cluster outside the CLASH framework.”
DO HOT HALOS AROUND GALAXIES CONTAIN THE MISSING BARYONS? (2010, background): “…gas to have Z ∼ 0.2 Z (using Anders & Grevesse 1989 abundances) following Cen & Ostriker (2006) and Rasmussen et al. (2009), and since similar metallicity is found in the hot intracluster medium even toward the virial radius of distant galaxy clusters (Maughan et al. 2008; Anderson et al. 2009).”
X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories (2009, background): “Maughan et al. (2008) looked at a larger sample of 116 clusters at 0.1 < z < 1.3 in theChandra archive and essentially confirmed the results of Balestra et al. (2007).”
Bimodal gas accretion in the Horizon–MareNostrum galaxy formation simulation (2008, methodology): “Finally, the enrichment rates found for X-ray clusters by Balestra et al. (2007) and Maughan et al. (2008) (s ≈ 0.3 from z = 0 to z = 1.3 are well matched by the enrichment rate measured in the simulation between z = 2 − 3.”
ON THE CONNECTION BETWEEN GIANT RADIO HALOS AND CLUSTER MERGERS (2010, methodology): “…al. 2005; Ventimiglia et al. 2008; Böhringer et al. 2010); the emission centroid shift (e.g., Mohr et al. 1993; Poole et al. 2006, O’Hara et al. 2006; Ventimiglia et al. 2008, Maughan et al. 2008, Böhringer et al. 2010) and the surface brightness concentration parameter (e.g., Santos et al 2008).”
The COS-Halos Survey: Metallicities in the Low-redshift Circumgalactic Medium (2017, background): “The median CGM metallicity is also consistent with the enrichment of the hot (T > 106K) ‘halo’ gas comprising the intracluster medium (ICM; see Figure 12; Maughan et al. 2008).”
LoCuSS: the connection between brightest cluster galaxy activity, gas cooling and dynamical disturbance of X‐ray cluster cores (2009, methodology): “We determined this position in a similar fashion to Maughan et al.(2008), iteratively refining the cluster X-ray surface brightness centroid within an aperture of 2–3 arcmin initially, then repeating the centroiding within an aperture of∼1 arcmin.”
The MCXC: a meta-catalogue of x-ray detected clusters of galaxies (2010, methodology): “We construct a unique MACS catalogue by merging the three sub-catalogues and keeping only measurements given by Maughan et al. (2008) for the eighteen duplicate clusters (see Table 1).”
MEASURING THE ULTIMATE HALO MASS OF GALAXY CLUSTERS: REDSHIFTS AND MASS PROFILES FROM THE HECTOSPEC CLUSTER SURVEY (HeCS) (2012, background): “The X-ray luminosity of MS0906 is much larger than that of A750 (Maughan et al. 2008).”
CHANDRA CLUSTER COSMOLOGY PROJECT. II. SAMPLES AND X-RAY DATA REDUCTION (2008, unknown): “Such a trend (which is probably outside the range allowed by the data, see Tozzi et al. 2003; Maughan et al. 2008), will be equivalent to changing the mass scale for our high-z sample by +3%, +1%, and +6% if masses are estimated through the Mtot–YX, Mtot–Mgas, and Mtot–TX relations, respectively.”