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SXP 7.92: a recently rediscovered Be/X-ray binary in the Small Magellanic Cloud, viewed edge on
Bartlett, E. S.; Coe, M. J.; Israel, G. L.; Clark, J. S.; Esposito, P.; D'Elia, V.; Udalski, A.
AA(ESO - European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago de Chile, Chile; Astrophysics, Cosmology and Gravity Centre, Department of Astronomy, University of Cape Town, Rondebosch 7701, South Africa), AB(School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ, UK), AC(INAF - Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone (Roma), Italy), AD(Department of Physical Science, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK), AE(Anton Pannekoek Institute for Astronomy, University of Amsterdam, Postbus 94249, NL-1090-GE Amsterdam, the Netherlands), AF(INAF - Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone (Roma), Italy; ASI Science Data Center (ASDC), via del Politecnico snc, I-00133 Roma, Italy), AG(Warsaw University Observatory, Aleje Ujazdowskie 4, PL-00-478 Warszawa, Poland)
Monthly Notices of the Royal Astronomical Society, Volume 466, Issue 4, p.4659-4671 (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
stars: emission-line, Be, Magellanic Clouds, X-rays: binaries
Abstract Copyright:
2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Bibliographic Code:


We present a detailed optical and X-ray study of the 2013 outburst of the Small Magellanic Cloud Be/X-ray binary SXP 7.92, as well as an overview of the last 18 years of observations from OGLE (Optical Gravitational Lensing Experiment), RXTE, Chandra and XMM-Newton. We revise the position of this source to RA(J2000) = 00:57:58.4, Dec(J2000) = -72:22:29.5 with a 1sigma uncertainty of 1.5 arcsec, correcting the previously reported position by Coe et al. by more than 20 arcmin. We identify and spectrally classify the correct counterpart as a B1Ve star. The optical spectrum is distinguished by an uncharacteristically deep narrow Balmer series, with the Halpha line in particular having a distinctive shell profile, i.e. a deep absorption core embedded in an emission line. We interpret this as evidence that we are viewing the system edge on and are seeing self-obscuration of the circumstellar disc. We derive an optical period for the system of 40.0 ± 0.3 d, which we interpret as the orbital period, and present several mechanisms to describe the X-ray/optical behaviour in the recent outburst, in particular the 'flares'and 'dips' seen in the optical light curve, including a transient accretion disc and an elongated precessing disc.
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