<?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%">Misanovic, Z.</style></author><author><style face="normal" font="default" size="100%">Pietsch, W.</style></author><author><style face="normal" font="default" size="100%">Haberl, F.</style></author><author><style face="normal" font="default" size="100%">Trinchieri, G.</style></author><author><style face="normal" font="default" size="100%">Ehle, M.</style></author><author><style face="normal" font="default" size="100%">Hatzidimitriou, D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">XMM-Newton survey of the Local Group galaxy M33 bright individual sources</style></title><short-title><style face="normal" font="default" size="100%">Populations of High Energy Sources in Galaxies</style></short-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2006/01/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2006IAUS..230..162M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">230</style></volume><pages><style face="normal" font="default" size="100%">162 - 163</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%">As shown in our first poster, in a recent survey of M33 with XMM-Newton we detected the X-ray source population of this nearby spiral galaxy down to the (0.2-4.5) keV luminosity of 10&lt;SUP&gt;35&lt;/SUP&gt; erg s&lt;SUP&gt;-1&lt;/SUP&gt;, a factor of 10 deeper than in previous observations. The majority of the detected sources was classified using, in many cases, only their X-ray properties. In particular, 8 new X-ray binary (XRB) candidates were selected, based on their long-term X-ray light curves. We also classified supernova remnants (SNRs), super-soft sources (SSS), AGN, foreground stars and a population of ‘hard’ sources using the hardness ratio (HR) method. A detailed spectral and timing analysis of the brightest sources is in progress. We present a few examples of spectra for particular source classes. We find that bright ‘hard’ sources can be divided into two broad families: one best modelled by a powerlaw with photon index in the range of 1.0-2.0, and the other displaying disk blackbody spectra with kT of 0.8 to 1.5 keV.</style></abstract></record></records></xml>