Cosmological constraints from the X-ray gas mass fraction in relaxed lensing clusters observed with Chandra

By S. Allen, R. Schmidt, A. C. Fabian. 2002

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We present precise measurements of the X-ray gas mass fraction for a sample of luminous, relatively relaxed clusters of galaxies observed with the Chandra Observatory, for which independent confirmation of the mass results is available from gravitational lensing studies. Parameterizing the total (luminous plus dark matter) mass profiles using the model of Navarro, Frenk & White (1997), we show that the X-ray gas mass fractions in the clusters asymptote towards an approximately constant value at a radius r_2500, where the mean interior density is 2500 times the critical density of the Universe at the redshifts of the clusters. Combining the Chandra results on the X-ray gas mass fraction and its apparent redshift dependence with recent measurements of the mean baryonic matter density in the Universe and the Hubble Constant determined from the Hubble Key Project, we obtain a tight constraint on the mean total matter density of the Universe, Omega_m = 0.30^{+0.04}_{-0.03}, and measure a positive cosmological constant, Omega_Lambda = 0.95^{+0.48}_{-0.72}. Our results are in good agreement with recent, independent findings based on analyses of anisotropies in the cosmic microwave background radiation, the properties of distant supernovae, and the large-scale distribution of galaxies.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/43f837117f856f0e176f9c6ae3be628ebc405d72

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Citations in the corpus

ERRATUM: “CHANDRA SAMPLE OF NEARBY RELAXED GALAXY CLUSTERS: MASS, GAS FRACTION, AND MASS–TEMPERATURE RELATION” (2006, ApJ, 640, 691) (2005, background): “We also do not observe flattening of fgas(r) at radii within r2500 as reported, e.g., in Allen et al. (2002).”
Holographic dark energy (2016, methodology): “In addition, one can also obtain the constraints on DE by using the X-ray cluster gas mass fraction [132, 133].”
Cosmological constraints from the local X-ray luminosity function of the most X-ray-luminous galaxy clusters (2002, methodology): “…between σ8 and Ωm using the observed X-ray gas mass fractions, fgas, in the clusters and their apparent redshift dependence (e.g. White & Frenk 1991; White et al. 1993; Sasaki 1996; Pen 1997; Ettori & Fabian 1999; Allen et al. 2002a; Erdogdu, Ettori & Lahav 2002; Ettori, Tozzi & Rosati 2003).”
Near-Infrared Properties of Galaxy Clusters: Luminosity as a Binding Mass Predictor and the State of Cluster Baryons (2003, methodology): “Finally, with Chandra observations of 7 intermediate redshift clusters, Allen et al. (2002) deduced that ΩM = 0.30 +0.04 −0.03.”
X-Ray and Sunyaev-Zel’dovich Effect Measurements of the Gas Mass Fraction in Galaxy Clusters (2006, background): “We first compare our X-ray results with Chandra results obtained using a different analysis technique (Allen et al. 2002, 2004)8, in which the cluster mass is modeled assuming that the cluster gas is in hydrostatic equilibrium with a NFW potential and using a deprojected 3D gas temperature profile.”
Generalized Chaplygin gas as a unified scenario of dark matter/energy: Observational constraints (2004, methodology): “Recently, Allen et al. (2002; 2003) reported precise measurements of thefgasprofiles for 10 relaxed clusters determined from theChandra observational data.”
Predictions for high-frequency radio surveys of extragalactic sources (2004, background): “Recent X-ray Chandra observations show that for massive clusters the gas fraction is remarkably constant, fg = 0.113± 0.005, independently of the cluster redshift (Allen et al. 2002).”
Weak-Lensing Mass Reconstruction of the Interacting Cluster 1E 0657–558: Direct Evidence for the Existence of Dark Matter (2003, background): “Recent observations of clusters suggest that the mass is made of ∼ 1% of baryons observable in optical and infrared data, ∼ 11% of baryons observable in X-ray data (e.g. Allen et al. 2002), and the remaining ∼ 88% in the dark matter component.”
The cluster gas mass fraction as a cosmological probe: a revised study (2009, background): “…many studies have followed this approach to constrain the cosmological parameters (White & Fabian 1995; David et al. 1995; Ettori & Fabian 1998; Rines et al. 1999; Roussel et al. 2000; Allen et al. 2002; Ettori et al. 2003; Castillo-Morales & Schindler 2003; Sadat et al. 2005; Allen et al. 2008).”
Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters (2007, methodology): “Measurements of the apparent evolution of the cluster X-ray gas mass fraction, hereafter fgas, can also be used to probe the acceleration of the Universe (Allen et al. 2004; see also Sasaki 1996, Pen 1997, Allen et al. 2002a, 2003, Ettori et al. 2003, LaRoque et al. 2006).”
Weighing the giants – IV. Cosmology and neutrino mass (2014, background): “…deserves some additional consideration, since the value and evolution of its normalization, β0,mgas = ln fgas(r500), carry additional cosmological information (Sasaki 1996; Pen 1997; Allen et al. 2002, 2004, 2008, 2011; Ettori et al. 2003, 2009; Battaglia et al. 2013; Planelles et al. 2013; M14).”
A kinematical approach to dark energy studies (2006, background): “…al. 1998; Perlmutter et al. 1999; Knop et al. 2003; Riess et al. 2004; Astier et al. 2005), the distance-redshift relation to X-ray galaxy clusters (Allen et al. 2002, 2004; Ettori et al. 2003), measurements of the mean matter density and amplitude of matter fluctuations from X-ray clusters…”
The Search for the Missing Baryons at Low Redshift (2007, background): “The X-ray emission from this hot gas has been used to determine its mass, and the baryon content of these rich clusters is consistent with the cosmological value (Allen et al., 2002).”
A Direct Empirical Proof of the Existence of Dark Matter (2006, background): “They are skewed toward the plasma clouds, which is expected because the plasma contributes about 1/10th of the total cluster mass (Allen et al. 2002; Vikhlinin et al. 2006) (and a higher fraction in non-standard gravity models without dark matter).”