与EXO 0748-676 = UY对应的静态光学和红外线
The Quiescent Optical and Infrared Counterpart to EXO 0748-676 = UY Vol
摘要：
本文对低质量X射线双星EXO 0748-676进行了自1985年X射线活动以来24年来的首次光学和红外测光。我们在平均星等R=22.4和J=21.3处找到对应的星等。从2008年11月到2009年1月，我们大约每晚监测一次污染源。在这段时间内，有相当大的夜间光学变化，但没有长期的趋势是明显的。夜间变化揭示了P=0.159331+/-0.000012d的周期性，与X射线轨道周期一致，在0.01%以内。这表明，静态光调制实际上是轨道性质，而不是一个超级驼峰。有趣的是，调制仍然是单峰的，有一个深的最小值与X射线食的时间相一致，没有迹象表明有一个双峰椭球调制。这表明，即使在“静止”发射的吸积盘和/或X射线加热的内表面的伴星占主导地位的光学发射，并意味着获得一个准确的动态质量估计在静止将是具有挑战性的。
英文摘要：
We present optical and infrared photometry of the low-mass X-ray binary EXO 0748-676 in quiescence for the first time in 24 years since it became X-ray active in 1985. We find the counterpart at average magnitudes of R=22.4 and J=21.3. We monitored the source approximately nightly through 2008 November to 2009 January. During this time there was considerable night-to-night optical variability but no long term trends were apparent. The night-to-night variability reveals a periodicity of P=0.159331+/-0.000012d, consistent with the X-ray orbital period to within 0.01%. This indicates that the quiescent optical modulation is indeed orbital in nature rather than a superhump. Interestingly, the modulation remains single-peaked with a deep minimum coincident with the times of X-ray eclipse, and there is no indication of a double-peaked ellipsoidal modulation. This indicates that even in `quiescence' emission from the accretion disk and/or X-ray heated inner face of the companion star dominate the optical emission, and implies that obtaining an accurate dynamical mass estimate in quiescence will be challenging.
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