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For refcode 2006ApJ...652..232H:
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2006ApJ...652..232H Multiwavelength Mass Comparisons of the z~0.3 CNOC Cluster Sample A. K. Hicks, E. Ellingson, H. Hoekstra, and H. K. C. Yee Abstract. Results are presented from a detailed analysis of optical and X-ray observations of moderate-redshift galaxy clusters from the Canadian Network for Observational Cosmology (CNOC) subsample of the EMSS. The combination of extensive optical and deep X-ray observations of these clusters make them ideal candidates for multiwavelength mass comparison studies. X-ray surface brightness profiles of 14 clusters with 0.17<z<0.55 are constructed from Chandra observations and fit to single- and double-{beta} models. Spatially resolved temperature analysis is performed, indicating that five of the clusters in this sample exhibit temperature gradients within their inner 60 -- 200 kpc. Integrated spectra extracted within R_2500_ provide temperature, abundance, and luminosity information. Under assumptions of hydrostatic equilibrium and spherical symmetry, we derive gas and total masses within R_2500_ and R_200_. We find an average gas mass fraction of f_gas_(R_200_)=0.092+/-0.004h^-3/2^_70_, resulting in {OMEGA}_m_=0.42+/-0.02 (formal error). We also derive dynamical masses for these clusters to R_200_. We find no systematic bias between X-ray and dynamical methods across the sample, with an average M_dyn_/M_X_=0.97+/-0.05. We also compare X-ray masses to weak-lensing mass estimates of a subset of our sample, resulting in a weighted average of M_lens_/M_X_ of 0.99+/-0.07. We investigate X-ray-scaling relationships and find power-law slopes that are slightly steeper than the predictions of self-similar models, with an E(z)^-1^L_X_-T_X_ slope of 2.4+/-0.2 and an E(z)M_2500_-T_X_ slope of 1.7+/-0.1. Relationships between red-sequence optical richness (B_gc,red_) and global cluster X-ray properties (T_X_, L_X_, and M_2500_) are also examined and fitted. Key words: Cosmology: Observations, Galaxies: Clusters: General, X-Rays: Galaxies: Clusters =========================================================================== 2008ApJ...672.1293H Erratum: "Multiwavelength Mass Comparisons of the z ~ 0.3 CNOC Cluster Sample" (ApJ, 652, 232 [2006]) Hicks, A. K.; Ellingson, E.; Hoekstra, H.; Yee, H. K. C. Abstract. In our original paper there was a miscalculation in the determination of central gas densities for that sample, which we correct here. We also report a processing error in the exposure map for MS 1512.4+3647 and supply a correction factor for its surface brightness normalization and background. The code which was used to determine cluster central densities contained an error such that it did not account for a (1+z)^3^ cosmological dimming factor, derived from a combination of cosmological distance and time dilation corrections. Subsequently, all central densities, gas masses, and gas mass fractions reported in the paper should be scaled up by a factor of (1+z)^3/2^. An error also occurred in the production of the exposure map for MS 1512.4+3647, which caused the best-fit surface brightness normalization and background for that cluster to be reduced by a factor of 8 (all other {beta}-model values remain unaffected). Therefore, the SB normalization and background of MS 1512.4+3647 should be multiplied by this factor, while its central gas density, gas mass, and gas mass fraction should be multiplied by sqrt(8) (in addition to the cosmological factor mentioned above). Table A1 contains updated values for central densities, gas masses, and gas mass fractions, along with 90% confidence intervals. Using these values, we obtain a weighted mean gas mass fraction for the sample, f_gas_(R_200_)=0.136+/-0.004h^-3/2^_70_, resulting in {OMEGA}_m_=0.28+/-0.01, a value consistent with WMAP 3 year results (D. N. Spergel et al., ApJ, 652, 232 [2006]). We emphasize that these corrections do not otherwise affect our results. In particular, our main conclusion remains valid, e.g., our finding that there is very good agreement between X-ray, dynamical, and weak-lensing cluster mass estimation methods. ===========================================================================
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