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2013ApJ...767..116M Joint Analysis of Cluster Observations. II. Chandra/XMM-Newton X-Ray and Weak Lensing Scaling Relations for a Sample of 50 Rich Clusters of Galaxies Mahdavi, Andisheh; Hoekstra, Henk; Babul, Arif; Bildfell, Chris; Jeltema, Tesla; Henry, J. Patrick Abstract. We present a study of multiwavelength X-ray and weak lensing scaling relations for a sample of 50 clusters of galaxies. Our analysis combines Chandra and XMM-Newton data using an energy-dependent cross-calibration. After considering a number of scaling relations, we find that gas mass is the most robust estimator of weak lensing mass, yielding 15% +/- 6% intrinsic scatter at r_{500}_^{WL} (the pseudo-pressure Y_X_ yields a consistent scatter of 22% +/- 5%). The scatter does not change when measured within a fixed physical radius of 1 Mpc. Clusters with small brightest cluster galaxy (BCG) to X-ray peak offsets constitute a very regular population whose members have the same gas mass fractions and whose even smaller (<10%) deviations from regularity can be ascribed to line of sight geometrical effects alone. Cool-core clusters, while a somewhat different population, also show the same (<10%) scatter in the gas mass-lensing mass relation. There is a good correlation and a hint of bimodality in the plane defined by BCG offset and central entropy (or central cooling time). The pseudo-pressure Y_X_ does not discriminate between the more relaxed and less relaxed populations, making it perhaps the more even-handed mass proxy for surveys. Overall, hydrostatic masses underestimate weak lensing masses by 10% on the average at r_{500}_^{WL}; but cool-core clusters are consistent with no bias, while non-cool-core clusters have a large and constant 15%-20% bias between r_{2500}_^{WL} and r_{500}_^{WL}, in agreement with N-body simulations incorporating unthermalized gas. For non-cool-core clusters, the bias correlates well with BCG ellipticity. We also examine centroid shift variance and power ratios to quantify substructure; these quantities do not correlate with residuals in the scaling relations. Individual clusters have for the most part forgotten the source of their departures from self-similarity. Key words: galaxies: clusters: general, galaxies: clusters: intracluster medium, gravitational lensing: weak, X-rays: galaxies: clusters =========================================================================== 2014ApJ...794..175M Erratum: "Joint Analysis of Cluster Observations. II. Chandra/XMM-Newton X-Ray and Weak Lensing Scaling Relations for a Sample of 50 Rich Clusters of Galaxies" (2013, ApJ, 767, 116) Mahdavi, Andisheh; Hoekstra, Henk; Babul, Arif; Bildfell, Chris; Jeltema, Tesla; Henry, J. Patrick Abstract. The published version of the article "Joint Analysis of Cluster Observations. II. Chandra/XMM-Newton X-ray and Weak Lensing Scaling Relations for a Sample of 50 Rich Clusters of Galaxies" contained an error in the bolometric correction factor in the reported X-ray luminosities. In addition, Table 1 contained thermodynamic quantities reported at r2500 instead of r500. No other aspects of the analysis were affected. We present a table with updated quantities and fit results.{see Table 1} In the published version of this article, we applied an incorrect bolometric bandpass correction factor to the X-ray flux of all clusters, resulting in bolometric X-ray luminosities that were too high throughout the entire analysis. Since this was a problem only with the bandpass correction factor, none of the other results of the paper were affected. In addition, Table 1 of the published article reported luminosities and temperatures at an aperture of r2500 instead of r500. Here we present updated luminosities and mass-luminosity scaling relations (Table 3) which take the correct bolometric correction factor into account. Note that the Chandra and XMM-Newton Observatory calibrations used are the same one as in the published article. These updated numbers are also present on the Web site of the paper, http://sfstar.sfsu.edu/jaco. Since the error was roughly a constant factor applied to LX, only the intercepts of the LX relations have changed substantially; the slopes and intrinsic scatters of these relations are still within the originally reported limits. {see Table 3} ===========================================================================
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