X-ray and Optical Observations of the Merging Cluster Abell S1063.

Details X-ray and Optical Observations of the Merging Cluster Abell S1063. X-ray and Optical Observations of the Merging Cluster Abell S1063.

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009cfdd.confe.111g&link_type=abstract

Chandra's First Decade of Discovery, Proceedings of the conference held 22-25 September, 2009 in Boston, MA. Edited by Scott Wo

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Clusters Of Galaxies

Scientific paper

We present the first in depth analysis of the massive cluster Abell S1063. This is one of the hottest X-ray clusters discovered to date and is undergoing a major merging event. It provides an important comparison system for the well known ``bullet cluster'', as it has a similar redshift, X-ray temperature and luminosity. The average temperature of the hot intracluster medium has been measured for the first time, using Chandra ACIS-I, and found to be > 12 keV. Optical spectroscopy, from GMOS-S, has provided a mean cluster recessional velocity of 103800^{+300}_{-330} km s^{-1} and a velocity dispersion of 1840^{+230}_{-150} km s^{-1} (1 σ errors). Both the large velocity dispersion and high X-ray temperature suggest either a very massive cluster (M ( 4.0 × 10^{15} M_{sun}) or a merger system. The merger model is supported by a small offset between the galaxy density and the peak of the X-ray emission, by the presence of offset and twisted X-ray isophotes, and by a non-Gaussian galaxy velocity distribution. We also report that the velocity distribution is consistent with the velocity distributions found in N-body simulations of head-on cluster mergers (e.g. 1:4 mass ratio). Moreover, we find that the best fit model for the distribution of the cluster gas consists of two, offset, isothermal beta model components. Therefore, we propose that a recent merger event close to the plane of the sky is responsible for the observed properties of the cluster. In addition, optical imaging, from SuSI2 on the NTT and GMOS-S at Gemini, have also uncovered the presence of several gravitational arcs that can be used to further constrain the mass of the cluster.

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