<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Hatzidimitriou, D.</style></author><author><style face="normal" font="default" size="100%">Antoniou, V.</style></author><author><style face="normal" font="default" size="100%">Zezas, A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">High mass X-ray binaries in the Small Magellanic Cloud</style></title><short-title><style face="normal" font="default" size="100%">Ipparchos</style></short-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2008/05/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2008Ippa....2d..27H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">2</style></volume><pages><style face="normal" font="default" size="100%">27 - 32</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Using Chandra, XMM and optical data (both photometric and spectroscopic), we studied the X-ray binary population in the Small Magellanic Cloud (SMC), down to an X-ray luminosity of ~4×10^33 erg s-1, thus allowing the investigation of the faintest of the high-mass Xraybinary populations. The regions were selected so as to have varying star formation histories, in order to investigate, using homogeneous and well defined samples, the connection between the Be- XRB phenomenon and SF history. The characterization of the X-ray sources discovered in our Chandra and XMM surveys and the selection of our sample of Be-XRBs, was based on a combination of X-ray and optical properties. We found that the number of Be/X-ray binaries (Be-XRBs) peaks at the age of 40-70 Myr ago. Finally, we constructed their X-ray luminosity function (XLF). There are very few X-ray sources above ~10^35 ergs^-1, which is consistent with the transient nature of Be X-ray binaries. There is also indication for a flattening of the XLF at ~10^35 ergs^-1, which would be consistent with the onset of the propeller effect.</style></abstract></record></records></xml>