Journal
ASTROPHYSICAL JOURNAL
Volume 711, Issue 2, Pages 1033-1043Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/711/2/1033
Keywords
cosmology: observations; galaxies: clusters: general; galaxies: clusters: individual (Abell 1914); gravitational lensing: weak; surveys; X-rays: galaxies: clusters
Categories
Funding
- DFG [RE 1462/2]
- German BMBF through the Verbundforschung [50 OR 0601]
- Ministry of Education, Science, Sports and Culture of Japan
- Ministry of Education, Culture, Sports, Science, and Technology of Japan [18072001, 20740099]
- BMBF/DLR [50 OR 0207]
- MPG
- NASA [NNX08AX46G, HF-51259.01, NAS5-26555]
- Royal Society
- STFC
- Grants-in-Aid for Scientific Research [20740099] Funding Source: KAKEN
- Science and Technology Facilities Council [PP/E001203/1] Funding Source: researchfish
- STFC [PP/E003486/1, PP/E001203/1] Funding Source: UKRI
- NASA [NNX08AX46G, 92992] Funding Source: Federal RePORTER
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We compare X-ray hydrostatic and weak-lensing mass estimates for a sample of 12 clusters that have been observed with both XMM-Newton and Subaru. At an over-density of Delta = 500, we obtain 1 - M(X)/M(WL) = 0.01 +/- 0.07 for the whole sample. We also divided the sample into undisturbed and disturbed sub-samples based on quantitative X-ray morphologies using asymmetry and fluctuation parameters, obtaining 1 - M(X)/M(WL) = 0.09 +/- 0.06 and -0.06 +/- 0.12 for the undisturbed and disturbed clusters, respectively. In addition to non-thermal pressure support, there may be a competing effect associated with adiabatic compression and/or shock heating which leads to overestimate of X-ray hydrostatic masses for disturbed clusters, for example, in the famous merging cluster A1914. Despite the modest statistical significance of the mass discrepancy, on average, in the undisturbed clusters, we detect a clear trend of improving agreement between M(X) and M(WL) as a function of increasing overdensity, M(X)/M(WL) = (0.908 +/- 0.004) + (0.187 +/- 0.010) . log(10)(Delta/500). We also examine the gas mass fractions, f(gas) = M(gas)/M(WL), finding that they are an increasing function of cluster radius, with no dependence on dynamical state, in agreement with predictions from numerical simulations. Overall, our results demonstrate that XMM-Newton and Subaru are a powerful combination for calibrating systematic uncertainties in cluster mass measurements.
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