<?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%">Sell, Paul H.</style></author><author><style face="normal" font="default" size="100%">Zezas, Andreas</style></author><author><style face="normal" font="default" size="100%">Williams, Stephen J.</style></author><author><style face="normal" font="default" size="100%">Andrews, Jeff J.</style></author><author><style face="normal" font="default" size="100%">Gazeas, Kosmas</style></author><author><style face="normal" font="default" size="100%">Gallagher, John S.</style></author><author><style face="normal" font="default" size="100%">Ptak, Andrew</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The X-ray binary populations of M81 and M82</style></title><short-title><style face="normal" font="default" size="100%">IAU Symposium</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Accretion</style></keyword><keyword><style  face="normal" font="default" size="100%">galaxies: individual (M81</style></keyword><keyword><style  face="normal" font="default" size="100%">galaxies: spiral</style></keyword><keyword><style  face="normal" font="default" size="100%">galaxies: star clusters</style></keyword><keyword><style  face="normal" font="default" size="100%">galaxies: starburst</style></keyword><keyword><style  face="normal" font="default" size="100%">M82)</style></keyword><keyword><style  face="normal" font="default" size="100%">stars: neutron</style></keyword><keyword><style  face="normal" font="default" size="100%">X-rays: binaries</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2019</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2019/12/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2019IAUS..346..344S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">346</style></volume><pages><style face="normal" font="default" size="100%">344 - 349</style></pages><isbn><style face="normal" font="default" size="100%">1743-9221</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We use deep Chandra and HST data to uniquely classify the X-ray binary (XRB) populations in M81 on the basis of their donor stars and local stellar populations (into early-type main sequence, yellow giant, supergiant, low-mass, and globular cluster). First, we find that more massive, redder, and denser globular clusters are more likely to be associated with XRBs. Second, we find that the high-mass XRBs (HMXBs) overall have a steeper X-ray luminosity function (XLF) than the canonical star-forming galaxy XLF, though there is some evidence of variations in the slopes of the sub-populations. On the other hand, the XLF of the prototypical starburst M82 is described by the canonical powerlaw (α&lt;SUB&gt;cum&lt;/SUB&gt; ∼ 0.6) down to L&lt;SUB&gt;X&lt;/SUB&gt; ∼ 10&lt;SUP&gt;36&lt;/SUP&gt; erg s&lt;SUP&gt;-1&lt;/SUP&gt;. We attribute variations in XLF slopes to different mass transfer modes (Roche-lobe overflow versus wind-fed systems).</style></abstract></record></records></xml>