Direct constraints on the dark matter self-interaction cross-section from the merging galaxy cluster 1E0657-56

Details Direct constraints on the dark matter self-interaction cross-section from the merging galaxy cluster 1E0657-56 Direct constraints on the dark matter self-interaction cross-section from the merging galaxy cluster 1E0657-56

2003-09-11

arxiv.org/abs/astro-ph/0309303v2

Astrophys.J.606:819-824,2004

Astronomy and Astrophysics

Astrophysics

Text clarified; some numbers changed slightly for consistency with final version of the accompanying lensing paper. 6 pages, u

Scientific paper

10.1086/383178

We 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.

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