Cosmological constraints from the local X-ray luminosity function of the most X-ray-luminous galaxy clusters

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

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We present precise constraints on the normalization of the power spectrum of mass fluctuations in the nearby Universe, σ 8, as a function of the mean local matter density, � m. Using the observed local X-ray luminosity function of galaxy clusters from the extended BCS and REFLEX studies, a mass‐luminosity relation determined from Chandra and ROSAT X-ray data and weak gravitational lensing observations, and the mass function predicted by the Hubble Volume simulations of Evrard et al., we obtain σ 8 = (0.508 ± 0.019) � −(0.253±0.024) ,

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1d6f78e9f0a79d7120b2e32bc1d7fc34b2c1c044

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Citations in the corpus

Observational probes of cosmic acceleration (2012, background): “…cluster cosmology constraints have come primarily from X-ray data (see, e.g., Henry, 2000; Reiprich and Böhringer, 2002; Schuecker et al., 2003; Allen et al., 2003; Pierpaoli et al., 2003), reflecting the fact that X-ray observables can be related to mass via simulations and/or analytic…”
The observed concentration–mass relation for galaxy clusters (2007, unknown): “Voigt & Fabian (2006) X-ray 5.12 ± 0.40 10.0 ± 1.2 6.62 ± 0.50 11.9 ± 1.5 Pointecouteau et al. (2005) X-ray 3.83+0.52−0.27 18.6 +3.5 −4.0 5.00 +0.66 −0.34 22.7 +4.5 −5.1 Allen et al. (2003) RXJ1416.”
Generalized Chaplygin gas as a unified scenario of dark matter/energy: Observational constraints (2004, methodology): “…as f modgas (zi; As, α) = bΩb ( 1+ 0.19h1/2 ) Ωeffm h 0.5 DASCDM(zi) DAgCg(zi; As, α) 3/2 (5) where the bias factorb = 0.93 ± 0.05 (Bialek et al. 2001; Allen et al. 2003) is a parameter motivated by gas dynamical simulations, which suggest that the baryon fraction in clusters is…”
The Observed Growth of Massive Galaxy Clusters I: Statistical Methods and Cosmological Constraints (2009, background): “…relation (e.g. Borgani et al. 2001) or simultaneously fitting an external luminosity–mass data set without accounting for selection effects (e.g. Allen et al. 2003).8 In M08, we took this approach to its logical limit by deriving the likelihood for bins of infinitesimal volume; however, that…”
The Observed Growth of Massive Galaxy Clusters II: X-ray Scaling Relations (2009, result): “…band luminosities or 1.7–2.3 for bolometric luminosities (e.g. Reiprich & Böhringer 2002; Zhang et al. 2007; M08; Rykoff et al. 2008; Zhang et al. 2008; Pratt et al. 2009; Vikhlinin et al. 2009a), though we note good agreement with a previous study of very luminous clusters (Allen et al. 2003).”
Search for New Physics with Atoms and Molecules (2017, background): “It was pointed out by Olive et al. (2011) that the generalization of the Copernican principle that assumes a homogeneous Universe at large scales is not fully satisfied in such a model and its theoretical foundation is unclear.”
Cosmological Parameters from Observations of Galaxy Clusters (2011, result): “X-ray studies in particular showed that the amplitude was lower than had been accepted previously (e.g. Borgani et al. 2001; Reiprich & Böhringer 2002; Seljak 2002; Pierpaoli et al. 2003; Allen et al. 2003; Schuecker et al. 2003), a result later confirmed by CMB and cosmic shear measurements.”
New constraints on dark energy from the observed growth of the most X-ray luminous galaxy clusters (2007, methodology): “…density of the universe and the amplitude of perturbations in the density field (e.g. Reiprich & Böhringer 2002; Seljak 2002; Viana et al. 2002; Allen et al. 2003; Pierpaoli et al. 2003; ⋆ E-mail: amantz@stanford.edu Schuecker et al. 2003; Voevodkin & Vikhlinin 2004; Dahle 2006; Rozo et al.…”
Constraints on dark energy from Chandra observations of the largest relaxed galaxy clusters (2004, background): “…1991, W hite et al. 1993, D avid, Jones & Form an 1995;W hite& Fabian 1995;Evrard 1997;M ohr,M athiesen & Evrard 1999; Ettori& Fabian 1999; Roussel, Sadat & Blanchard 2000;Allen,Schm idt & Fabian 2002a;Allen et al.2003;Ettori,Tozzi& Rosati2003;Sanderson & Ponm an 2003;Lin,M ohr& Stanford 2003).”
The structural and scaling properties of nearby galaxy clusters. I. The universal mass profile (2005, background): “…that CDM numerical simulations predict the correct shape of the Dark Matter distribution, not only in massive cluster (e.g. David et al. 2001; Allen et al. 2001; Arabadjis et al. 200 ; Buote & Lewis 2004; Buote 2004; Allen et al. 2003), but also in low mass clusters (Pratt & Arnaud 2003).”
A kinematical approach to dark energy studies (2006, background): “…2004; Ettori et al. 2003), measurements of the mean matter density and amplitude of matter fluctuations from X-ray clusters (Borgani et al. 2001; Allen et al. 2003; Reiprich & Böhringer 2002; Schuecker et al. 2003; Voevodkin & Vikhlinin 2004), measurements of the matter power spectrum from…”
Cosmic distance-duality as a probe of exotic physics and acceleration (2003, methodology): “ and the RG data sets is therefore rather stable. We do so far only use radio galaxy data to estimate the angular diameter distance. Other promising data sets include e.g. the X-ray gas mass fraction [12] and SZ data [13]. We have indeed included the gas mass fraction data of Allen et al, and margin”
What Shapes the Luminosity Function of Galaxies? (2003, unknown): “…(CMB)]; Sievers et al. 2003 [SunyaevZeldovich effect]), other recent analyses have suggested lower values, 8 0:7 (e.g., Peacock 2003 [large-scale structure]; Melchiori et al. 2002 [CMB]; Jarvis et al. 2003 [gravitational lensing]; Allen et al. 2003, Smith et al. 2003 [cluster abundance]).”
BUDHIES II: a phase-space view of H i gas stripping and star formation quenching in cluster galaxies (2015, unknown): “The cluster’s total X-ray luminosity is LX ⋍ 3.4 ± 1 × 10 44ergs−1h−2 (Allen et al. 2003).”
COSMOLOGICAL CONSTRAINTS FROM THE SLOAN DIGITAL SKY SURVEY MaxBCG CLUSTER CATALOG (2009, background): “…(Viana & Liddle 1996, 1999; Henry & Arnaud 1991; Henry 2000; Pierpaoli et al. 2001; Borgani et al. 2001; Seljak 2002; Viana et al. 2002; Schuecker et al. 2003; Allen et al. 2003; Bahcall et al. 2003; Bahcall & Bode 2003; Henry 2004; Voevodkin & Vikhlinin 2004; Rozo et al. 2007b; Gladders et al.…”
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION (2009, methodology): “Previous measurements of the LX −M relation based on X-ray data (Reiprich & Böhringer 2002; Allen et al. 2003; Popesso et al. 2005; Chen et al. 2007; Pratt et al. 2008; Zhang et al. 2008; Vikhlinin et al. 2009) as well as the the M − LX relation derived with lensing (Hoekstra 2007a; Bardeau et al.…”