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