Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...458..285k&link_type=abstract
Astronomy and Astrophysics, Volume 458, Issue 1, October IV 2006, pp.285-292
Astronomy and Astrophysics
Astrophysics
7
Magellanic Clouds, X-Rays: Stars, X-Rays: Binaries, Stars: Emission-Line, Be, Stars: General
Scientific paper
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 ⪆ 1034 erg s-1 for the X-ray source at LMC distance. Assuming that the bolometric luminosity does not exceed the Eddington luminosity of a ~ 1.0 M&sun; star we derive a blackbody temperature of (25-70) eV and an LMC absorbing column density of < 6× 1021 cm-2. 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 Hβ emission lines (with EWH_α˜ 34 Å) which indicate a B0-3e star. The radial velocities of the Hα and Hβ emission lines show a variation from ˜ 400-450 km s-1 to ˜ 5-20 km s-1 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 ˜ 0.9-1.0 M&sun;.
Filipović Miroslav D.
Haberl Franck
Kahabka Peter
Payne Jeff L.
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