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Mass and Hot Baryons in Massive Galaxy Clusters from Subaru Weak Lensing and AMiBA SZE Observations | | K. Umetsu
; M. Birkinshaw
; G.-C. Liu
; J.-H.P. Wu
; E. Medezinski
; T. Broadhurst
; D. Lemze
; A. Zitrin
; P.T.P. Ho
; C.-W. L. Huang
; P. M. Koch
; Y.-W. Liao
; K.-Y. Lin
; S. M. Molnar
; H. Nishioka
; F.-C. Wang
; P. Altamirano
; C.-H. Chang
; S.-H. Chang
; S.-W. Chang
; M.-T. Chen
; C.-C. Han
; Y.-D. Huang
; Y.-J. Hwang
; H. Jiang
; M. Kesteven
; D. Y. Kubo
; C.-T. Li
; P. Martin-Cocher
; P. Oshiro
; P. Raffin
; T. Wei
; W. Wilson
; | | Date: |
6 Oct 2008 | | Abstract: | We present a multiwavelength analysis of a sample of four hot (T_X>8keV)
X-ray galaxy clusters (A1689, A2261, A2142, and A2390) using joint AMiBA
Sunyaev-Zel’dovich effect (SZE) and Subaru weak lensing observations, combined
with published X-ray temperatures, to examine the distribution of mass and the
intracluster medium (ICM) in massive cluster environments. Our observations
establish that A2261 is very similar to A1689 in terms of both weak and strong
lensing properties. Many tangential arcs are visible around A2261, with an
effective Einstein radius sim 40 arcsec (at z sim 1.5), which when combined
with our weak lensing measurements implies a mass profile well fitted by an NFW
model with a high concentration c_{vir} sim 10, similar to A1689 and to other
massive clusters. The cluster A2142 shows complex mass substructure, and
displays a shallower profile (c_{vir} sim 5), being well traced by the SZE in
the AMiBA map, and consistent with detailed X-ray observations which imply
recent interaction. For A2390 we obtain highly elliptical mass and ICM
distributions at all radii, consistent with other X-ray and strong lensing
work. Our cluster gas fraction measurements, free from the hydrostatic
equilibrium assumption, are overall in good agreement with published X-ray and
SZE observations, with the sample-averaged gas fraction of <f_{gas}(<r_{200})>
= 0.133 pm 0.027 for our sample with <M_{vir}>=(1.2pm 0.1) imes 10^{15}
M_{sun}/h. When compared to the cosmic baryon fraction f_b = Omega_b/Omega_m
constrained by the WMAP 5-year data, this indicates <f_{gas}(<r_{200})>/f_b =
0.78 pm 0.16, i.e., (22 pm 16)% of the baryons are missing from the hot phase
of clusters. | | Source: | arXiv, 0810.0969 | | Services: | Forum | Review | PDF | Favorites | |
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