ERRATUM: “CHANDRA SAMPLE OF NEARBY RELAXED GALAXY CLUSTERS: MASS, GAS FRACTION, AND MASS–TEMPERATURE RELATION” (2006, ApJ, 640, 691)

By A. Vikhlinin, Andrey V. Kravtsov, W. Forman, C. Jones, M. Markevitch, S. Murray, L. V. Speybroeck. 2005

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We present gas and total mass profiles for 13 low-redshift, relaxed clusters spanning a temperature range 0.7-9 keV, derived from all available Chandra data of sufficient quality. In all clusters, gas-temperature profiles are measured to large radii (Vikhlinin et al.) so that direct hydrostatic mass estimates are possible to nearly r500 or beyond. The gas density was accurately traced to larger radii; its profile is not described well by a beta model, showing continuous steepening with radius. The derived ρtot profiles and their scaling with mass generally follow the Navarro-Frenk-White model with concentration expected for dark matter halos in ΛCDM cosmology. However, in three cool clusters, we detect a central mass component in excess of the Navarro-Frenk-White profile, apparently associated with their cD galaxies. In the inner region (r < 0.1r500), the gas density and temperature profiles exhibit significant scatter and trends with mass, but they become nearly self-similar at larger radii. Correspondingly, we find that the slope of the mass-temperature relation for these relaxed clusters is in good agreement with the simple self-similar behavior, M500 Tα, where α = (1.5-1.6) ± 0.1, if the gas temperatures are measured excluding the central cool cores. The normalization of this M-T relation is significantly, by ≈30%, higher than most previous X-ray determinations. We derive accurate gas mass fraction profiles, which show an increase with both radius and cluster mass. The enclosed fgas profiles within r2500 0.4r500 have not yet reached any asymptotic value and are still far (by a factor of 1.5-2) from the universal baryon fraction according to the cosmic microwave background (CMB) observations. The fgas trends become weaker and its values closer to universal at larger radii, in particular, in spherical shells r2500 < r < r500.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

The XMM Cluster Survey: A Massive Galaxy Cluster at z = 1.45 (2006, background): “…would need to have a mass, within an overdensity of 500 with respect to the critical density, of around 2 × 1014 h−1 M⊙ (Pierpaoli et al. 2003; Viana et al. 2003), about 2/3 smaller than is implied by the most recent observational data (Arnaud, Pointecouteau & Pratt 2005; Vikhlinin et al. 2006).”
CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS (2008, methodology): “The Ponman et al. (2003) results rely on extrapolations based on assumed density (β-model) and temperature (polytropic-model) profiles, which may not be adequate and may bias the derived ICM properties (e.g., Borgani et al. 2004; Vikhlinin et al. 2006, V06 hereafter).”
The case for AGN feedback in galaxy groups (2009, background): “This gives a much larger lever arm for discriminating between thermal histories of the intragroup medium and it also allows one to compare groups to clusters at the characteristic radius where clusters show evi- dence for convergence in fgas (see, e.g., Vikhlinin et al. 2006; McCarthy et al. 2007).”
Systematics in the X-ray cluster mass estimators (2006, background): “We find that, while |A| 3 up to R500 for all the objects, B indicates that the spectroscopic temperature is within 20 per cent of T mw, with implications on the mass estimates (Mathiesen & Evrard 2001; Vikhlinin et al. 2006; see Section 5.1).”
Galaxy cluster X-ray luminosity scaling relations from a representative local sample (REXCESS) (2008, background): “…of the X-ray mass-temperature relation have shown percent-level agreement in normalisation and that the slope is not greatly different from the self-similar expectation (Arnaud et al. 2005; Vikhlinin et al. 2006), although it may be slightly steeper (Arnaud et al. 2005; Sun et al. 2008).”
THE LARGE-SCALE BIAS OF DARK MATTER HALOS: NUMERICAL CALIBRATION AND MODEL TESTS (2010, background): “This expectation is borne out for observables such as gas mass, core-excised luminosity, integrated SZ flux or its X-ray analog,YX (e.g., Mohr et al. 1999; Vikhlinin et al. 2006; Zhang et al. 2008; Vikhlinin et al. 2009; Arnaud et al. 2007, 2009; Sun et al. 2009).”
Hydrodynamical N-body simulations of coupled dark energy cosmologies (2008, background): “This could in fact alleviate tensions between the high baryon abundance estimated from CMB observations, and the somewhat lower values inferred from detailed X-ray observations of galaxy clusters (Vikhlinin et al. 2006; LaRoque et al. 2006; Afshordi et al. 2007; McCarthy, Bower & Balogh 2007).”
A Catalog of Galaxy Clusters Observed by XMM-Newton (2007, background): “The recent Chandra results of Vikhlinin et al. (2006) show a temperature profile in good agreement with the gradients seen by Markevitch et al. (1998) results and predicted by the standard theory.”
The EAGLE project: Simulating the evolution and assembly of galaxies and their environments (2014, methodology): “Mass profiles are obtained by fitting the functions proposed by Vikhlinin et al. (2006) to the density and temperature profiles and assuming hydrostatic equilibrium.”
SIMULATIONS OF THE MICROWAVE SKY (2009, methodology): “This model, which is described in more detail in Bode et al. (2009), adjusts four free parameters which are calibrated against X-ray gas fractions as a function of temperature from the sample of Sun et al. (2009) and Vikhlinin et al. (2006).”
Chaotic cold accretion on to black holes (2013, background): “Numerous XMM and Chandra observations of the hot gas in galaxies, groups and clusters (e.g. Vikhlinin et al. 2006; Diehl & Statler 2008; Rasmussen & Ponman 2009; Sun et al. 2009) have clearly demonstrated that the majority of systems have a cool core in roughly global thermal equilibrium.”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, positive): “Specifically, we use (see equation (3) and (8) of Vikhlinin et al. 2006)38 n2e(r) =n 2 0 (r/rc) −α (1 + r2/r2c ) 3β−α/2 1 (1 + rγ/rγs )ǫ/γ + n202 (1 + r2/r2c2) 3β2 , (72) Te(r) Tmg = 1.35 (x/0.045)1.9 + 0.45 (x/0.045)1.9 + 1 × 1 [1 + (x/0.6)2]0.45 , (73) where x ≡ r/r500.”
Cosmological Parameters from Observations of Galaxy Clusters (2011, methodology): “…for the puzzling deficit of baryons at r ∼ r500 inferred from some previous studies of massive clusters using lower quality X-ray data (at large radii) and stronger modeling priors (e.g. Vikhlinin et al. 2006; Gonzalez, Zaritsky & Zabludoff 2007; McCarthy, Bower & Balogh 2007; Ettori et al. 2009).”
Dark Matter Searches with Astroparticle Data (2011, background): “…gas show that not only is there more mass in the gas than in the galaxies themselves, typically by a factor of two, but for the gas to be in hydrostatic equilibrium there must be several times more mass in DM than in the gas or galaxies (e.g., Reiprich & Boehringer, 2002; Vikhlinin et al., 2006).”
The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation (2005, result): “A similar revision of the B01 parameters was previously proposed by Dolag et al. (2004; see also Kuhlen et al. 2005), who advocated lower K to accommodate their simulations of cluster-sized halos, and is in broad agreement with the profiles of observed clusters (Vikhlinin et al. 2006).”
CHANDRA CLUSTER COSMOLOGY PROJECT. II. SAMPLES AND X-RAY DATA REDUCTION (2008, methodology): “We choose Δ = 500, the radius within which the clusters are relatively relaxed (Evrard et al. 1996) and good measurements of gas mass and temperature can be obtained with our Chandra observations (Vikhlinin et al. 2006; Nagai et al. 2007b).”
Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters (2009, neutral): “We show in Figure 5 the comparison between simulation results and observational data on the mass fraction of hot gas as a function of temperature from Vikhlinin et al. (2006).”
Total mass biases in X-ray galaxy clusters (2008, methodology): “With respect to the isothermal β-model the modeling of the ICM has been significantly improved (e.g. Vikhlinin et al. 2006) through observational progress, which showed the existence of temperature profiles declining with radius (De Grandi & Molendi 2002; Vikhlinin et al. 2005; Piffaretti et al.…”