Volume 485, Number 1, July I 2008
|Page(s)||177 - 181|
|Section||Stellar structure and evolution|
|Published online||22 April 2008|
XMM-Newton observations of the Small Magellanic Cloud: XMMU J004814.1-731003, a 25.55 s Be/X-ray binary pulsar*
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany e-mail: email@example.com
2 University of Maryland, Baltimore County; X-ray Astrophysics Laboratory, Mail Code 662, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
Accepted: 6 March 2008
Aims. To investigate candidates for Be/X-ray binaries in the Small Magellanic Cloud (SMC), we observed a region around the emission nebula N19 with XMM-Newton in October 2006.
Methods. We analysed the EPIC data of the detected point sources to derive their spectral and temporal characteristics.
Results. We detected X-ray pulsations with a period of 25.550(2) s from the second-brightest source in the field, which we designate XMMU J004814.1-731003. The X-ray spectrum is well modelled by a highly absorbed (NH = 5 cm-2) power-law with photon index . The precise X-ray position allows us to identify a Be star as the optical counterpart. XMMU J004814.1-731003 is located within the error circle of the transient ASCA source AX J0048.2-7309, but its position is inconsistent with that of the proposed optical counterpart of AX J0048.2-7309 (the emission line star [MA93] 215). It remains unclear if XMMU J004814.1-731003 is associated with AX J0048.2-7309. XMMU J004814.1-731003 might be identical to an RXTE pulsar that was discovered with a period of 25.5 s, but which is listed as a 51 s pulsar in the recent literature.
Key words: galaxies: individual: small Magellanic Cloud / galaxy: stellar content / stars: emission-line, Be / stars: neutron / X-rays: binaries
© ESO, 2008
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