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

Roberto Soria, PASA, 16 (2), 147
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Contents Page: Volume 16, Number 2

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

Roberto Soria 1

1 Mount Stromlo Observatory, Private Bag, Weston Creek P.O., 2611, ACT, Australia
roberto@mso.anu.edu.au

Abstract:

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 B0.5IIIe with a mass

$M_* = (18 \pm 2) M_{\odot}$ and bolometric magnitude

$M_{\mbox{{\scriptsize bol}}} = -7.4 \pm 0.2$. The main spectral features are strong H$\alpha $ emission, H$\beta $ and H$\gamma$ emission cores with absorption wings, and narrow He I and O II absorption lines. Equivalent width and full width at half maximum of the main lines are listed. The average systemic velocity over our observing run is

$v_r = (184 \pm 4)$ km ${\rm s}^{-1}$; 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

$v \sin i = (145 \pm 10)$ km ${\rm s}^{-1}$for the Be star; if we assume a true rotational velocity at the equator

$v = (400 \pm 50)$ km ${\rm s}^{-1}$, we deduce that the inclination angle of the system is

$i = (21 \pm 3)\deg$.

Keywords:

galaxies: Magellanic Clouds--stars: individual (RX J0117.6-7330)--X-ray: binaries





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