Date Presented:

2010/03/1

Abstract:

Using Chandra, XMM-Newton and optical data we study the young (?Myr) X-ray binary (XRB) populations of the Magellanic Clouds. We find that the Be-XRBs of the Small Magellanic Cloud (SMC) are observed in regions with star formation (SF) rate bursts ˜25-60 Myr ago. The similarity of this age with the age of maximum occurrence of the Be phenomenon (˜40 Myr) indicates that the presence of a circumstellar decretion disk plays a significant role in the number of observed XRBs in the 10-100 Myr age range. We also find that regions with strong but more recent SF (e.g. the Wing) are deficient in Be-XRBs. By correlating the number of observed Be-XRBs with the formation rate of their parent populations, we measure a Be-XRB production rate of ˜1 system per 10^{-6} M⊙/yr. Finally, we use the strong localization of the Be-XRB systems in order to set limits on the kicks imparted on the neutron star during the supernova explosion. Understanding of the populations of compact objects and their connection with star-formation (SF) will allow us to investigate channels of XRB formation in a variety of environments and therefore help in studies of the X-ray source populations of star-forming galaxies outside our Local Group, and even enable their use as a SF diagnostic. This work was supported from NASA LTSA grant NAG5-13056, and NASA grant GO2-3117X.

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