A Hubble Space Telescope lensing survey of X-ray luminous galaxy clusters – IV. Mass, structure and thermodynamics of cluster cores at z = 0.2

By Graham P. Smith, Jean-Paul Kneib, I. Smail, P. Mazzotta, H. Ebeling, O. Czoske. 2005

224 citations recorded by the source corpus.

We present a comprehensive space-based study of ten X-ray luminous galaxy clusters (L_X>=8e44erg/s[0.1-2.4keV]) at z=0.2. Hubble Space Telescope observations reveal numerous gravitationally-lensed arcs for which we present four new spectroscopic redshifts, bringing the total to thirteen confirmed arcs in this cluster sample. We combine the multiple-image systems with the weakly-sheared background galaxies to model the total mass distribution in the cluster cores (R<=500kpc). These models are complemented by high-resolution X-ray data from Chandra and used to develop quantitative criteria to classify the clusters as relaxed or unrelaxed. Formally, (30+/-20)% of the clusters form a homogeneous sub-sample of relaxed clusters; the remaining (70+/-20)% are unrelaxed and are a much more diverse population. Most of the clusters therefore appear to be experiencing a cluster-cluster merger, or relaxing after such an event. We also study the normalization and scatter of scaling relations between cluster mass, luminosity and temperature. The scatter in these relations is dominated by the unrelaxed clusters and is typically sigma~0.4. Most notably, we detect 2-3 times more scatter in the mass-temperature relation than theoretical simulations and models predict. The observed scatter is also asymmetric - the unrelaxed systems are systematically 40% hotter than the relaxed clusters at 2.5 sigma significance. This structural segregation should be a major concern for experiments designed to constrain cosmological parameters using galaxy clusters. Overall our results are consistent with a scenario of cluster-cluster merger induced boosts to cluster X-ray luminosities and temperatures. [Abridged]

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b4e1618eb8f8cb75fd16fe9c68479575b620cbea

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Citations in the corpus

LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters (2009, methodology): “…function that is blind to such factors would support an increased understanding of possible biases in cluster mass estimates as a function of the dynamical state and shape of clusters (Dahle et al. 2002; Smith et al. 2005; Clowe et al. 2006; Bardeau et al. 2007; Hoekstra 2007; Okabe & Umetsu 2008).”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, background): “In many clusters, the BCG is indeed located near the bottom of the gravitational well of the cluster (e.g. Allen 1998; Smith et al. 2005; von der Linden et al. 2007; Best et al. 2007), but this is not always the case (Lin & Mohr 2004; Skibba et al. 2011).”
Resolved spectroscopy of gravitationally lensed galaxies: recovering coherent velocity fields in subluminous z ~ 2-3 galaxies (2009, methodology): “…projects such as the MAssive Cluster Survey (MACS, Ebeling et al. 2001) and Local Cluster Substructure Survey c© 0000 RAS, MNRAS 000, 000–000 (LoCuSS, Smith et al. 2005), we have studied a large sample of lensing clusters and undertaken a search within these HST images for promising magnified…”
Combining Strong and Weak Gravitational Lensing in Abell 1689 (2006, methodology): “It is interesting to compare to the offset found in Smith et al. (2005) for a sample of X-rayYluminous clusters whose properties are comparable to Abell 1689 (i.e., they have a high X-ray luminosity and are located at z 0:2).”
BUDHIES II: a phase-space view of H i gas stripping and star formation quenching in cluster galaxies (2015, background): “6 of Smith et al. 2005), suggesting A963 1 is a relaxed cluster.”
X-ray–optical classification of cluster mergers and the evolution of the cluster merger fraction (2011, background): “…and hydrostatic equilibrium, a pronounced spatial segregation of gas and galaxies constitutes powerful evidence of a recent or ongoing merger (e.g. Smith et al. 2005; Shan et al. 2010); conversely, excellent alignment of the BCG with the intracluster gas distribution is typical of relaxed systems…”
RESIDUAL GAS MOTIONS IN THE INTRACLUSTER MEDIUM AND BIAS IN HYDROSTATIC MEASUREMENTS OF MASS PROFILES OF CLUSTERS (2009, background): “More recently, mass estimates via strong lensing (Smith et al. 2005), weak lensing (e.g., Dahle 2006; Mahdavi et al. 2008; Zhang et al. 2008), combined strong and weak lensing (Bradač et al. 2006; Limousin et al. 2007; Oguri et al. 2009), and Sunyaev-Zel’dovich effect (e.g., Carlstrom et al. 2002,…”
A comparison of weak-lensing masses and X-ray properties of galaxy clusters (2007, background): “(See Bardeau et al. (2005) and Smith et al. (2005) for a discussion of the z = 0.2 cluster sample, which is selected from the X-ray Brightest Abell Clusters Survey (XBACS; Ebeling et al. 1996).)”
LoCuSS: the connection between brightest cluster galaxy activity, gas cooling and dynamical disturbance of X‐ray cluster cores (2009, background): “…the X-ray peak and the BCG is sensitive to the cluster dynamical state (Katayama et al. 2003), which is ⋆ E-mail: ajrs@star.sr.bham.ac.uk analagous to the offset between the peaks of the gravitational le sing mass map and the X-ray emission as an indicator of disturbance (Smith et al. 2005).”
Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies (2014, background): “…the early 1990s (e.g. Kneib et al. 1996) to constrain the detailed mass distribution in cluster cores as well as to probe the mass distributions of samples of X-ray-selected clusters out to the virial radius (e.g. Smith et al. 2005; Ebeling et al. 2009; Richard et al. 2010b; Zitrin et al. 2012).”
LoCuSS: first results from strong-lensing analysis of 20 massive galaxy clusters at z= 0.2 (2009, background): “…luminosity (Lin et al. 2006), Xray luminosity and temperature (e.g. Vikhlinin et al. 2006), Sunayev-Zeldovich effect (e.g. Nagai 2006; Bonamente et al. 2008), cluster kinematics (e.g. Blindert et al. 2004), and gravitational lensing (e.g. Bardeau et al. 2007; Smith et al. 2005; Okabe et al. 2009).”
The Mass Distribution of SDSS J1004$+$4112 Revisited (2010, methodology): “This technique has been adopted by several authors (e.g., Kayser 1990; Kochanek 1991; Koopmans et al. 1998; Keeton 2001a; Smith et al. 2005; Bradač et al. 2005; Halkola et al. 2006; Jullo et al. 2007; Sand et al. 2008), although the implementations were quite different for different papers.”
Weighing simulated galaxy clusters using lensing and X-ray (2009, background): “…discrepancy has been revealed in the sense that masses derived from strong lensing are typically higher by a factor 2−3 than masses derived from weak lensing and from the X-ray emitting intra-cluster-medium (ICM) (e.g. Wu & Mao 1996; Ota et al. 2004; Smith et al. 2005; Riemer-Sørensen et al. 2009).”
THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. I. THE TOTAL DENSITY OVER THREE DECADES IN RADIUS (2012, methodology): “A383 The model follows N11, which built upon Sand et al. (2004, 2008) and Smith et al. (2005).”
Combining Lens Distortion and Depletion to Map the Mass Distribution of A1689 (2007, background): “From space, deep multi-color images of massive clusters can be used to identify many sets of multiple images per cluster (Broadhurst et al. 2005b, hereafter B05b; Gavazzi et al. 2003; Kneib et al. 2004; Sand et al. 2004; Smith et al. 2005; Bradač et al. 2006).”
Discovery of a Ringlike Dark Matter Structure in the Core of the Galaxy Cluster Cl 0024+17 (2007, methodology): “…strong- and weak-lensing constraints to derive a cluster mass profile has been previously proposed and applied to observations (e.g., Abdelsalam et al. 1998; Bridle et al. 1998; Seitz et al. 1998; Kneib et al. 2003; Smith et al. 2005; Bradač et al. 2005; Halkola et al. 2006; Cacciato et al. 2006).”
THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, methodology): “Progress toward this goal has been made by LoCuSS, the Local Cluster Substructure Survey (Smith et al. 2005).”
A Keck Survey for Gravitationally Lensed Lyα Emitters in the Redshift Range 8.5 < z < 10.4: New Constraints on the Contribution of Low-Luminosity Sources to Cosmic Reionization (2007, methodology): “Further discussion of the code, LENSTOOL, used to create the mass models for systems for which rich detail is available Jullo et al, (in prep and Smith et al. (2005).”