Subaru Weak Lensing Study of Seven Merging Clusters of Galaxies Keiichi Umetsu (ASIAA, Taiwan) & Nobuhiro Okabe (Tohoku Univ, Japan) Ref. Okabe & Umetsu 2007, submitted to PASJ (astro-ph/0702649) 1. Introduction We present and compare projected distributions of mass, galaxies, and the intracluster medium (ICM) for a sample of merging clusters of merging clusters of galaxies based on the joint weak-lensing, optical imaging, and X-ray analysis. Our sample comprises seven nearby Abel clusters (0.0542 < z < 0.279), for which we have conducted systematic, deep imaging observations with Suprime-Cam on Subaru telescope. Our seven target clusters, representing various merging stages and conditions, allow us to investigate in details the physical interplay between DM, ICM, and galaxies associated with cluster formation and evolution. A1750 and A1758 are binary systems consisting of two cluster-sized components. A520, A754, A1758, and A1914 are on-going cluster mergers, and A2034 and A2142 are cold-front clusters. 2. Observations and Data Cluster X-ray properties: (a) Binary, (b) On-going, (c) Cold front Target clusters and Subaru/X-ray observations Background Galaxy Sample for Mapmaking 3. Distributions of Mass/Galaxies/ICM in Clusters of Different Merging Stages (a) A1750: early phase (b) A1758N: on-going (c) A2142: cold front Subaru Rc-band image (25’x23.5’) Subaru Rc-band image (21’x18’) Subaru Rc-band image (27’x19’) Thermal SZE measurement by AMiBA (94GHz, 23’ FoV) 60cm x 7 elements Tsys = 100K (Trx=70K) 94GHz (11GHz BW) Dual poralizations Complex 4-lag correlator Sensitivity: 50mJy per 6’ beam in 1hr Mass contours (1s,2s,..) XMM X-ray contours Mass contours (1s,2s,..) Mass contours (1s,2s,..) XMM X-ray contours Chandra X-ray image (0.7-7.0keV) XMM X-ray image (0.5-7.0keV) Rc-band Cluster Luminosity density XMM X-ray image (0.5-7.0keV) Rc-band Cluster Luminosity density Rc-band Cluster Luminosity density SZ Flux@3mm = -300mJy (6s) per 6’ beam, 5x2 hrs 2-patch tracking by the AMiBA team Mass contours (1s,2s,..) Mass contours (1s,2s,..) Mass contours (1s,2s,..) Mass contours (1s,2s,..) Mass contours (1s,2s,..) Mass contours (1s,2s,..) 4. Cluster Global Properties: Lensing mass, Total optical luminosity, X-ray properties Color-selected red galaxy sample Cluster mass and luminosity estimates Best fitting NFW/SIS parameters from z-statistic Temperature ratio, Tx/Tsis, as a function of virial temperature Summary Projected mass, light, and X-ray maps are overall similar and regular in the binary clusters, which are presumably in an early merging phase. Mass distributions in the on-going systems are highly irregular but similar to galaxy distributions; their distributions are quite different from the ICM distribution in a various way, from cluster to cluster. The cold front clusters reveal irregular mass structures which are different from the ICM structure. All of 3 cold fronts are found to be associated with t a mass structure located ahead of the moving cold front, as found in the bullet cluster 1E0657-56. The ICM temperature of on-going/cold-front clusters is significantly higher than the cluster virial temperature by a factor of 2-3. This temperature excess in the ICM can be explained by the effects of merger boosts. Virial temperature (lensing-based SIS) vs. X-ray average temperature Merger boosts: Tx/Tsis>1 Tx=Tsis Tx=Tsis