New constraints on dark energy from the observed growth of the most X-ray luminous galaxy clusters

By A. Mantz, S. Allen, H. Ebeling, D. R. Kipac, Stanford, Ifa, Hawaii. 2007

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We present constraints on the mean matter density, {Omega}{sub m}, normalization of the density fluctuation power spectrum, {sigma}{sub 8}, and dark energy equation of state parameter, w, obtained from the X-ray luminosity function of the Massive Cluster Survey (MACS) in combination with the local BCS and REFLEX galaxy cluster samples. Our analysis incorporates the mass function predictions of Jenkins et al. (2001), a mass-luminosity relation calibrated using the data of Reiprich and Bohringer (2002), and standard priors on the Hubble constant, H{sub 0}, and mean baryon density, {Omega}{sub b} h{sup 2}. We find {Omega}{sub m}=0.27 {sup +0.06} {sub -0.05} and {sigma}{sub 8}=0.77 {sup +0.07} {sub -0.06} for a spatially flat, cosmological constant model, and {Omega}{sub m}=0.28 {sup +0.08} {sub -0.06}, {sigma}{sub 8}=0.75 {+-} 0.08 and w=-0.97 {sup +0.20} {sub -0.19} for a flat, constant-w model. Our findings constitute the first precise determination of the dark energy equation of state from measurements of the growth of cosmic structure in galaxy clusters. The consistency of our result with w=-1 lends strong additional support to the cosmological constant model. The constraints are insensitive to uncertainties at the 10-20 percent level in the mass function and in the redshift evolution o the mass-luminosity relation; the constraint on dark energy is additionally robust against our choice of priors and known X-ray observational biases affecting the mass-luminosity relation. Our results compare favorably with those from recent analyses of type Ia supernovae, cosmic microwave background anisotropies, the X-ray gas mass fraction of relaxed galaxy clusters and cosmic shear. A simplified combination of the luminosity function data with supernova, cosmic microwave background and cluster gas fraction data using importance sampling yields the improved constraints {Omega}{sub m}=0.263 {+-} 0.014, {sigma}{sub 8}=0.79 {+-} 0.02 and w=-1.00 +- 0.05.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e004bedcd2accd7510d14bd23862e3aa4f6033ab

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Citations in the corpus

X-ray–optical classification of cluster mergers and the evolution of the cluster merger fraction (2011, methodology): “The resulting negative evolution with look-back time of, for example, the cluster mass function has long been rec- E-mail: amann@ifa.hawaii.edu ognized as a powerful tool to constrain cosmological parameters (e.g. Eke et al. 1998; Borgani et al. 2001; Vikhlinin et al. 2003; Mantz et al. 2008, 2010).”
Cosmology and astrophysics from relaxed galaxy clusters - II. Cosmological constraints (2014, background): “…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.…”
Cosmological Parameters from Observations of Galaxy Clusters (2011, methodology): “…the results from cluster growth so far have made use of mass functions from ΛCDM simulations, accounting for the value of w only in the expansion history (Vikhlinin et al. 2009b) or, at most, including the effect of density variations on the linear matter power spectrum (Mantz et al. 2008, 2010b).”
Simulating the Universe with MICE: The abundance of massive clusters (2009, background): “…matter density), the normalization of the matter power spectrum and the expansion history of the universe, characterized by the dark energy density and its equation of state (e.g. see Mantz et al. 2008; Cunha 2009; Henry et al. 2009; Rozo et al. 2009; Vikhlinin et al. 2009, and references therein).”
Weighing the giants – IV. Cosmology and neutrino mass (2014, methodology): “The first three points shown in the figure are those of Mantz et al. (2008), M10a and this work, discussed above.”
COSMOLOGICAL CONSTRAINTS FROM THE SLOAN DIGITAL SKY SURVEY MaxBCG CLUSTER CATALOG (2009, methodology): “Rather than duplicating their work, in this section we opt for performing a simple analysis that captures the essential physics behind the Mantz et al. (2008) and Vikhlinin et al. (2008b) results, which helps illustrate exactly why and how clusters complement CMB, supernova, and BAO studies.”
MEASURING THE ULTIMATE HALO MASS OF GALAXY CLUSTERS: REDSHIFTS AND MASS PROFILES FROM THE HECTOSPEC CLUSTER SURVEY (HeCS) (2012, background): “…and other mass probes (richness, YX , YSZ ,Mlens, see Rines et al. 2010), a determination of the mass function of clusters (e.g., Rines et al. 2008; Vikhlinin et al. 2009; Mantz et al. 2008; Henry et al. 2009) and a detailed study of the photometric and spectroscopic properties of cluster galaxies.”
The Observed Growth of Massive Galaxy Clusters II: X-ray Scaling Relations (2009, methodology): “E-mail: amantz@slac.stanford.edu The construction of X-ray flux-selected cluster samples out to redshift z = 0.5 and beyond has now enabled investigations of dark energy using these data (Mantz et al. 2008, hereafter M08; Vikhlinin et al. 2009b).”
The X-ray brightest clusters of galaxies from the Massive Cluster Survey (2010, background): “…the sample presented here allows cosmological and astrophysical studies of the properties and evolution of the most massive galaxy clusters over a contiguous redshift range from z ∼ 0 to z = 0.7 (Allen et al. 2003, 2004, 2008; Ebeling et al. 2009; Mantz et al. 2008, 2010a,b, Rapetti et al. 2009).”
The Observed Growth of Massive Galaxy Clusters I: Statistical Methods and Cosmological Constraints (2009, background): “…to jointly constrain the average density of matter, m, and the amplitude of density perturbations, σ8 (recently by Henry et al. 2009; Rozo et al. 2010, but see also Reiprich & Böhringer 2002; Allen et al. 2003; Schuecker et al. 2003 and additional references in Mantz et al. 2008, hereafter M08).”
Weighing the Giants – III. Methods and measurements of accurate galaxy cluster weak-lensing masses (2012, methodology): “Weak lensing follow-up of clusters can be used,an to some extent has already been used, to set the absolute calibrations for the mass-observable relations employed in current X-ray and optical cluster count surveys (e.g. Mantz et al. 2008, 2010a; Vikhlinin et al. 2009b; Rozo et al. 2010).”
COSMOLOGICAL CONSTRAINTS FROM GALAXY CLUSTERS IN THE 2500 SQUARE-DEGREE SPT-SZ SURVEY (2016, background): “(5) We choose to take the limit of small bins where y becomes arbitrarily small at all xi, and n is zero except at the locations of xi where clusters have been observed (Mantz et al. 2008, 2010, V09).”
Evidence of the accelerated expansion of the Universe from weak lensing tomography with COSMOS (2009, background): “…et al. 2009), cosmic microwave background (de Bernardis et al. 2000; Spergel et al. 2003; Komatsu et al. 2009), galaxy clusters (Allen et al. 2008; Mantz et al. 2008, 2009; Vikhlinin et al. 2009), baryon acoustic oscillations (Eisenstein et al. 2005; Percival et al. 2007, 2009), integrated…”