Optical follow-up of new Small Magellanic Cloud wing Be/X-ray binaries

Type Journal Article
Names M. P. E. Schurch, M. J. Coe, K. E. McGowan, V. A. McBride, D. A. H. Buckley, J. L. Galache, R. H. D. Corbet, M. Still, P. Vaisanen, A. Kniazev, K. Nordsieck
Publication Monthly Notices of the Royal Astronomical Society
Volume 381
Issue 4
Pages 1561-1568
Date November 1, 2007
URL http://adsabs.harvard.edu/abs/2007MNRAS.381.1561S
Library Catalog NASA ADS
Abstract We investigate the optical counterparts of recently discovered Be/X-ray binaries in the Small Magellanic Cloud (SMC). In total four sources, SXP101, SXP700, SXP348 and SXP65.8 were detected during the Chandra survey of the wing of the SMC. SXP700 and SXP65.8 were previously unknown. Many optical ground-based telescopes have been utilized in the optical follow-up, providing coverage in both the red and blue bands. This has led to the classification of all of the counterparts as Be stars and confirms that three lie within the Galactic spectral distribution of known Be/X-ray binaries. SXP101 lies outside this distribution and is the latest spectral type known. Monitoring of the Hα emission line suggests that all the sources barring SXP700 have highly variable circumstellar discs, possibly a result of their comparatively short orbital periods. Phase-resolved X-ray spectroscopy has also been performed on SXP65.8, revealing that the emission is indeed harder during the passage of the X-ray beam through the line of sight.
Tags Be, MAGELLANIC CLOUDS, X-Rays: Binaries, stars: emission-line
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