Volume 458, Number 1, October IV 2006
|Page(s)||285 - 292|
|Section||Stellar structure and evolution|
|Published online||16 October 2006|
The super-soft source XMMU J052016.0-692505 in the LMC
A likely white dwarf Be/X-ray binary
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, 85741 Garching, Germany e-mail: [pkahabka;fwh]@mpe.mpg.de
2 Centre for Astronomy, James Cook University, Townsville, Queensland 4811, Australia
3 University of Western Sydney, Locked Bag 1797, Penrith South DC, NSW 1797, Australia
Accepted: 28 July 2006
Aims.We report the discovery of the super-soft X-ray source XMMU J052016.0-692505 in the LMC with XMM-Newton.
Methods.We analyse the EPIC spectra of XMMU J052016.0-692505 and study the likely optical counterpart LMCV2135.
Results.Using an absorbed blackbody spectrum we derive a bolometric luminosity of for the X-ray source at LMC distance. Assuming that the bolometric luminosity does not exceed the Eddington luminosity of a ~ star we derive a blackbody temperature of and an LMC absorbing column density of <. The likely optical counterpart of XMMU J052016.0-692505 is the LMC variable star LMCV2135 which is a MACHO and OGLE variable. The infrared and optical colors and magnitudes of this star are consistent with a hot star of likely spectral type B. The long-term MACHO light curve shows variability with a timescale of ∼500 and ∼1000 days. The optical spectra obtained at the 1.9-meter telescope of the South African Astronomical Observatory show strong Hα and H emission lines (with Å) which indicate a B0–3e star. The radial velocities of the Hα and H emission lines show a variation from ∼ to ∼ which is consistent with the systemic velocity of the LMC and an intrinsic variation most likely due to the rotation of the Be disk. We discuss LMCV2135/XMMU J052016.0-692505 as a Be/white dwarf binary system in the LMC. The super-soft X-ray spectrum of the source could be due to a stable nuclear burning white dwarf with a mass of ∼.
Key words: Magellanic Clouds / X-rays: stars / X-rays: binaries / stars: emission-line, Be / stars: general
© ESO, 2006
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