X-ray Emission from the
Star Clusters Near the Galactic Center
F. Yusef-Zadeh(Northwestern U.) C. Law & A. Fruscione (CfA) M. Wardle (University of Sydney) Q.D. Wang & C.C. Lang (U. of Massachusetts) A. Cotera (University of Arizona)
Abstract
The detection of two thermal X-ray sources from an extraordinarily compact massive star cluster, the Arches cluster (G0.12-0.02), is reported. This cluster is embedded within a bath of diffuse X-ray emission extending beyond the edge of the cluster to at least 90 (3.6 pc 2.4 pc). The diffuse emission beyond the boundary of the cluster is discussed in the context of combined shocked stellar winds escaping from the cluster. The presence of such a high velocity wind flow has implications for other dense systems of mass-losing hot stars such as the IRS 16 at the Galactic center. IRS 16 consists of a number of hot mass-losing stars which could produce an X-ray emitting high cluster wind flow with a velocity of 1000 km s-1 as predicted by Canto et al. and detected in the Arches cluster. The interaction of such a hot cluster wind flow with Sgr A* may affect the mass accretion rate. We also present the distribution of the 6.4 keV emission from the Arches cluster as well as discuss the relationship between the X-ray filaments at the edge of the nonthermal radio filaments of the Arc.
CATEGORY: NORMAL STARS AND WHITE DWARFS