@conference {23904,
	title = {Star-Formation History and Young X-ray Binary Populations: The Case of the Small Magellanic Cloud},
	year = {2009},
	month = {2009/09/1},
	pages = {63},
	abstract = {Using Chandra, XMM-Newton and optical photometric and spectroscopic catalogs we study the young (\&lt;100 Myr) X-ray binary populations of the Small Magellanic Cloud, which at \~{}60 kpc is our second nearest star-forming galaxy. In particular, we investigate the importance of Be/X-ray binaries as a dominant component of young X-ray binary populations, based on a study of the connection between X-ray source populations and their parent stellar populations. We find that a significant number of Be/X-ray binaries and/or pulsars are connected with a burst of star formation \~{}25-60 Myr ago, while regions with weak star-formation rate at \~{}42 Myr, such as the SMC Wing, are deficient in Be/X-ray binaries. We argue that the very strong similarity between the age of maximum occurence of Be stars and the age of the parent populations of X-ray binaries in the Small Magellanic Cloud indicates that the Be phenomenon plays a significant role in the number of X-ray binary populations in this age range. Finally, based on the spatial correlation between the star-formation activity and the X-ray binaries, we set a limit on their kick velocity of \~{}15-20 km/s, while there is strong indication for velocities of even a factor of two lower, and we estimate a Be/X-ray binary production rate of \~{}1 system per 10^{-6} M_{⊙}/yr.},
	keywords = {GALAXIES},
	url = {https://ui.adsabs.harvard.edu/abs/2009cfdd.confE..63A},
	author = {Antoniou, Vallia and Zezas, Andreas and Hatzidimitriou, D. and Kalogera, V.}
}
