The Observed Growth of Massive Galaxy Clusters II: X-ray Scaling Relations

By A. Mantz, S. Allen, H. Ebeling, David Rapetti, Alex Drlica-Wagner. 2009

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This is the second in a series of papers in which we derive simultaneous constraints on cosmology and X-ray scaling relations using observations of massive, X-ray flux-selected galaxy clusters. The data set consists of 238 clusters with 0.1-2.4keV luminosities >2.5 x 10 44 h -2 70 erg s -1 , and incorporates follow-up observations of 94 of those clusters using the Chandra X-ray Observatory or ROSAT (11 were observed with both). The clusters are drawn from three samples based on the ROSAT All-Sky Survey: the ROSAT Brightest Cluster Sample (78/37 clusters detected/followed-up), the ROSAT-ESO Flux-Limited X-ray sample (126/25) and the bright sub-sample of the Massive Cluster Survey (34/32). Our analysis accounts self-consistently for all selection effects, covariances and systematic uncertainties. Here we describe the reduction of the follow-up X-ray observations, present results on the cluster scaling relations, and discuss their implications. Our constraints on the luminosity-mass and temperature-mass relations, measured within r 500 , lead to three important results. First, the data support the conclusion that excess heating of the intracluster medium (or a combination of heating and condensation of the coldest gas) has altered its thermodynamic state from that expected in a simple, gravitationally dominated system; however, this excess heat is primarily limited to the central regions of clusters (r < 0.15r 500 ). Secondly, the intrinsic scatter in the centre-excised luminosity-mass relation is remarkably small, being bounded at the < 10 per cent level in current data; for the hot, massive clusters under investigation, this scatter is smaller than in either the temperature-mass or Y x -mass relations (10-15 per cent). Thirdly, the evolution with redshift of the scaling relations is consistent with the predictions of simple, self-similar models of gravitational collapse, indicating that the mechanism responsible for heating the central regions of clusters was in operation before redshift 0.5 (the limit of our data) and that its effects on global cluster properties have not evolved strongly since then. Our results provide a new benchmark for comparison with numerical simulations of cluster formation and evolution.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4307434579bc6408df315487184c147727cddae9

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Citations in the corpus

Scaling Properties of a Complete X-ray Selected Galaxy Group Sample (2014, unknown): “While for the M-YX relation the observed scatter (∼20%, e.g., Okabe et al. 2010) is larger than the scatter expected from simulations (<10%), the M-T relation indeed shows a small scatter (e.g., 13%, Mantz et al. 2010).”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, methodology): “…of the evolution of the cluster number density have provided some of the most precise and robust constraints on dark energy (Vikhlinin et al. 2009b; Mantz et al. 2010a), as well as departures from General Relativity on cosmological scales (Rapetti et al. 2010, 2013; Schmidt et al. 2009), and the…”
A SUNYAEV–ZEL'DOVICH-SELECTED SAMPLE OF THE MOST MASSIVE GALAXY CLUSTERS IN THE 2500 deg2 SOUTH POLE TELESCOPE SURVEY (2011, background): “…42 http://cxc.harvard.edu/toolkit/pimms.jsp 43 http://heasarc.nasa.gov/xanadu/xspec/xspec11/index.html 12 Williamson et al. tions from Pratt et al. (2009), Vikhlinin et al. (2009a), and Mantz et al. (2010), to compare our results with other X-ray cluster studies.”
Spherical collapse in quintessence models with zero speed of sound (2009, methodology): “Indeed, assuming hydrostatic equilibrium one can use the X-ray image of a cluster to reconstruct from its temperature and luminosity distribution the baryonic and dark matter radial profiles, as explained for instance in [52, 53].”
Weighing the giants – IV. Cosmology and neutrino mass (2014, methodology): “The project involves 51 massive clusters that have previously been used in cosmological studies (Allen et al. 2008; Mantz et al. 2010a,b, hereafter M10a,b).”
Evidence for Significant Growth in the Stellar Mass of Brightest Cluster Galaxies over the Past 10 Billion Years (2012, methodology): “21 of the clusters in Ebeling et al. (2007, 2010) and Mantz et al. (2010) are also in Ebeling et al. (1996, 1998, 2000), which enables us to compare the mass derived from the X-ray luminosity with the mass derived from X-ray temperature.”
Formation of Galaxy Clusters (2012, methodology): “Currently, cluster counts measured at high redshifts provide interesting constraints on cosmological parameters complementary to other methods (e.g., Mantz et al. 2010b, Rozo et al. 2010, Vikhlinin et al. 2009c) and a crucial test of the entire class ofΛCDM and quintessence models (e.g., Benson et…”
X-RAY PROPERTIES OF THE FIRST SUNYAEV–ZEL'DOVICH EFFECT SELECTED GALAXY CLUSTER SAMPLE FROM THE SOUTH POLE TELESCOPE (2010, background): “X-ray observations of these clusters could allow additional constraints on the redshift evolution of X-ray scaling relations, which typically have been studied from X-ray selected samples concentrated at z < 0.6 (e.g., Maughan 2007; Vikhlinin et al. 2009a; Mantz et al. 2009).”
Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts (2013, background): “Other biases in the determination of mass-observable scaling relations come from the object selection process itself (e.g., Mantz et al. 2010; Allen et al. 2011b; Angulo et al. 2012).”
Cosmology and astrophysics from relaxed galaxy clusters - II. Cosmological constraints (2014, methodology): “…which has been corroborated by a variety of independent cosmological data (e.g. Percival et al. 2007, 2010; Spergel et al. 2007; Kowalski et al. 2008; Mantz et al. 2008, 2010b; Dunkley et al. 2009; Vikhlinin et al. 2009; Rozo et al. 2010; Blake et al. 2011; Komatsu et al. 2011; Hinshaw et al.…”
Cluster Cosmology Constraints from the 2500 deg2 SPT-SZ Survey: Inclusion of Weak Gravitational Lensing Data from Magellan and the Hubble Space Telescope (2018, background): “8, comparisons with cluster samples selected through optical and X-ray methods have shown that the cluster populations can be described by powerlaw observable–mass scaling relations with lognormal intrinsic scatter (Vikhlinin et al. 2009a; Mantz et al. 2010a, 2016; Saro et al. 2015, 2017).”
Baryon impact on the halo mass function: Fitting formulae and implications for cluster cosmology (2015, background): “Catalogues from different cluster surveys have proven to be useful cosmological probes (e.g. Vikhlinin et al. 2009; Mantz et al. 2010; Rozo et al. 2010; Benson et al. 2013; Hasselfield et al. 2013; Planck Collaboration et al. 2015b; Bocquet et al. 2015; Mantz et al. 2015).”
RELICS: Reionization Lensing Cluster Survey (2019, background): “We also considered other factors in this selection, including X-ray mass estimates (Mantz et al. 2010; MCXC Piffaretti et al. 2011); weak lensing mass estimates (Sereno 2015 compilation including Weighing the Giants Applegate et al. 2014, von der Linden et al. 2014b; Umetsu et al. 2014; Hoekstra et…”
Observational probes of cosmic acceleration (2012, methodology): “5% (Burenin et al., 2007; Mantz et al., 2010).”
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).”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL’DOVICH EFFECT IN THE FIRST 720 SQUARE DEGREES OF THE SOUTH POLE TELESCOPE SURVEY (2012, background): “For example, adopting the temperature–luminosity relation of Mantz et al. (2010) results in luminosities that differ by ∼ 2± 2%, far less than the typical statistical uncertainty in the ROSAT count rates.”
ROBUST OPTICAL RICHNESS ESTIMATION WITH REDUCED SCATTER (2011, methodology): “The same calculation using the results of Mantz et al. (2010) gives σln M|LX = 0.32. also be reduced by increasing the correlation coefficient r, to make a significant reduction would require an unphysically large coefficient, in which overluminous clusters (where the scatter in LX is dominated by…”