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Optical Counterpart of the X-ray Transient RX J0117·6–7330: Spectroscopy and Photometry

Published online by Cambridge University Press:  05 March 2013

Roberto Soria
Roberto Soria*
Affiliation:
Mount Stromlo Observatory, Private Bag, Weston Creek PO, Weston Creek, ACT 2611, Australia; roberto@mso.anu.edu.au
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Abstract

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We conducted spectroscopic and photometric observations of the optical companion of the X-ray transient RX J0117·6–7330 in the Small Magellanic Cloud, during a quiescent state. The primary star is identified as a B0·5 IIIe with a mass M* = (18 ± 2)M⨀ and bolometric magnitude Mbol = –7·4 ± 0·2. The main spectral features are strong Hα emission, Hβ and Hγ emission cores with absorption wings, and narrow He I and O II absorption lines. Equivalent widths and full widths at half maximum of the main lines are listed. The average systemic velocity over our observing run is vr = (184 ± 4) km s−1; measurements over a longer period of time are needed to determine the binary period and the K velocity of the primary. We determine a projected rotational velocity v sin i = (145 ± 10) km s−1 for the Be star; if we assume a true rotational velocity at the equator v = (400 ± 50) km s−1, we deduce that the inclination angle of the system is i = (21 ± 3) deg.

Keywords

galaxies: Magellanic Cloudsstars: individual (RX J0117·6–7330)X-ray: binaries
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 16 , Issue 2 , 1999 , pp. 147 - 151
Copyright
Copyright © Astronomical Society of Australia 1999

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