<?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%">Vasilopoulos, G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">New Be/X-ray binary pulsars in the in the Large Magellanic Cloud</style></title><short-title><style face="normal" font="default" size="100%">11th Hellenic Astronomical Conference</style></short-title></titles><dates><year><style  face="normal" font="default" size="100%">2013</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2013/09/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2013hell.conf...46V</style></url></web-urls></urls><pages><style face="normal" font="default" size="100%">46 - 46</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We observed a newly discovered X-ray source int X-rays and in the optical to confirm its nature as a high mass X-ray binary. We analysed XMM-Newton and Swift X-ray data, along with optical observations with the ESO Faint Object Spectrograph, to investigate the spectral and temporal characteristics of the source. The XMM-Newton data show coherent X-ray pulsations while the spectra can be modelled with a combination of a power law plus a black body component. We performed optical spectroscopy from which we classify the companion star as a B0-1.5Ve star. The X-ray pulsations, the long-term x-ray variability and the properties of the optical counterpart confirms the the x-ray source as a new Be/X-ray binary pulsar in the LMC.</style></abstract></record></records></xml>