For refcode 2006ApJ...652..232H: Retrieve 14 NED objects in this reference. Please click here for ADS abstract
NED Abstract
Copyright by American Astronomical Society.
Reproduced by permission
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
Xray observations of moderateredshift galaxy clusters from the
Canadian Network for Observational Cosmology (CNOC) subsample of the
EMSS. The combination of extensive optical and deep Xray observations
of these clusters make them ideal candidates for multiwavelength mass
comparison studies. Xray 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 Xray
and dynamical methods across the sample, with an average
M_dyn_/M_X_=0.97+/0.05. We also compare Xray masses to weaklensing
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 Xrayscaling
relationships and find powerlaw slopes that are slightly steeper than
the predictions of selfsimilar 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 redsequence optical richness (B_gc,red_) and global cluster
Xray properties (T_X_, L_X_, and M_2500_) are also examined and
fitted.
Key words: Cosmology: Observations, Galaxies: Clusters: General, XRays:
Galaxies: Clusters
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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 bestfit 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 Xray, dynamical, and weaklensing
cluster mass estimation methods.
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