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29 March 2024
 
  » arxiv » astro-ph/0309303

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Direct constraints on the dark matter self-interaction cross-section from the merging galaxy cluster 1E0657-56
M. Markevitch ; A. H. Gonzalez ; D. Clowe ; A. Vikhlinin ; L. David ; W. Forman ; C. Jones ; S. Murray ; W. Tucker ;
Date 11 Sep 2003
Journal Astrophys.J. 606 (2004) 819-824
Subject astro-ph
Affiliation1,4), L. David , W. Forman , C. Jones , S. Murray , W. Tucker (1,5) ( CfA, Univ. of Florida, Univ. Bonn, IKI, UCSD
AbstractWe compare new maps of the hot gas, dark matter, and galaxies for 1E0657-56, a cluster with a rare, high-velocity merger occurring nearly in the plane of the sky. The X-ray observations reveal a bullet-like gas subcluster just exiting the collision site. A prominent bow shock gives an estimate of the subcluster velocity, 4500 km/s, which lies mostly in the plane of the sky. The optical image shows that the gas lags behind the subcluster galaxies. The weak-lensing mass map reveals a dark matter clump lying ahead of the collisional gas bullet, but coincident with the effectively collisionless galaxies. From these observations, one can directly estimate the cross-section of the dark matter self-interaction. That the dark matter is not fluid-like is seen directly in the X-ray -- lensing mass overlay; more quantitative limits can be derived from three simple independent arguments. The most sensitive constraint, sigma/m<1 cm^2/g, comes from the consistency of the subcluster mass-to-light ratio with the main cluster (and universal) value, which rules out a significant mass loss due to dark matter particle collisions. This limit excludes most of the 0.5-5 cm^2/g interval proposed to explain the flat mass profiles in galaxies. Our result is only an order-of-magnitude estimate which involves a number of simplifying, but always conservative, assumptions; stronger constraints may be derived using hydrodynamic simulations of this cluster.
Source arXiv, astro-ph/0309303
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