<?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%">Sturm, R.</style></author><author><style face="normal" font="default" size="100%">Haberl, F.</style></author><author><style face="normal" font="default" size="100%">Coe, M. J.</style></author><author><style face="normal" font="default" size="100%">Bartlett, E. S.</style></author><author><style face="normal" font="default" size="100%">Buckley, D. A. H.</style></author><author><style face="normal" font="default" size="100%">Corbet, R. H. D.</style></author><author><style face="normal" font="default" size="100%">Ehle, M.</style></author><author><style face="normal" font="default" size="100%">Filipović, M. D.</style></author><author><style face="normal" font="default" size="100%">Hatzidimitriou, D.</style></author><author><style face="normal" font="default" size="100%">Mereghetti, S.</style></author><author><style face="normal" font="default" size="100%">La Palombara, N.</style></author><author><style face="normal" font="default" size="100%">Pietsch, W.</style></author><author><style face="normal" font="default" size="100%">Tiengo, A.</style></author><author><style face="normal" font="default" size="100%">Townsend, L. J.</style></author><author><style face="normal" font="default" size="100%">Udalski, A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The XMM-Newton survey of the Small Magellanic Cloud: discovery of the 11.866 s Be/X-ray binary pulsar XMMU J004814.0-732204(SXP11.87)</style></title><short-title><style face="normal" font="default" size="100%">Astronomy and Astrophysics</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - High Energy Astrophysical Phenomena</style></keyword><keyword><style  face="normal" font="default" size="100%">Be</style></keyword><keyword><style  face="normal" font="default" size="100%">galaxies: individual: Small Magellanic Cloud</style></keyword><keyword><style  face="normal" font="default" size="100%">galaxies: stellar content</style></keyword><keyword><style  face="normal" font="default" size="100%">stars: emission-line</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%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2011/03/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2011A&amp;A...527A.131S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">527</style></volume><pages><style face="normal" font="default" size="100%">A131</style></pages><isbn><style face="normal" font="default" size="100%">0004-6361</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;BR /&gt; Aims: One of the goals of the XMM-Newton survey of the Small Magellanic Cloud is to study the Be/X-ray binary population. During one of our first survey observations, a bright new transient - XMMU J004814.0-732204 - was discovered. &lt;BR /&gt; Methods: We present the analysis of the EPIC X-ray data, together with optical observations, to investigate the spectral and temporal characteristics of XMMU J004814.0-732204. &lt;BR /&gt; Results: We found coherent X-ray pulsations in the EPIC data with a period of (11.86642 ± 0.00017) s. The X-ray spectrum can be modelled by an absorbed power law with an indication for a soft excess. Depending on the modelling of the soft X-ray spectrum, the photon index ranges between 0.53 and 0.66. We identify the optical counterpart as a B = 14.9 mag star that was monitored during the MACHO and OGLE-III projects. The optical light curves show regular outbursts by ~0.5 mag in B and R and up to 0.9 mag in I, which repeat on a time scale of about 1000 days. The OGLE-III optical colours of the star are consistent with an early B spectral type. An optical spectrum obtained at the 1.9 m telescope of the South African Astronomical Observatory in December 2009 shows Hα emission with an equivalent width of 3.5 ± 0.6 Å. &lt;BR /&gt; Conclusions: The X-ray spectrum and the detection of pulsations suggest that XMMU J004814.0-732204is a new high-mass X-ray binary pulsar in the SMC. The long term variability and the Hα emission line in the spectrum of the optical counterpart identify it as a Be/X-ray binary system.</style></abstract></record></records></xml>