<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>47</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Antoniou, Vallia</style></author><author><style face="normal" font="default" size="100%">Zezas, Andreas</style></author><author><style face="normal" font="default" size="100%">Hatzidimitriou, D.</style></author><author><style face="normal" font="default" size="100%">Kalogera, V.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Star-Formation History and Young X-ray Binary Populations: The Case of the Small Magellanic Cloud</style></title><short-title><style face="normal" font="default" size="100%">Chandra's First Decade of Discovery</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">GALAXIES</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2009</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2009/09/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2009cfdd.confE..63A</style></url></web-urls></urls><pages><style face="normal" font="default" size="100%">63</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Using Chandra, XMM-Newton and optical photometric and spectroscopic catalogs we study the young (&amp;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.</style></abstract></record></records></xml>