This is the third of a series of papers that presents an algorithm to search for close binaries with massive, possibly compact, unseen secondaries. The detection of such a binary is based on identifying a star that displays a large ellipsoidal periodic modulation, induced by tidal interaction with its companion. In the second paper of the series, we presented a simple approach to derive a robust modified minimum mass ratio (mMMR), based on the observed ellipsoidal amplitude, without knowing the primary mass and radius, assuming the primary fills its Roche lobe. The newly defined mMMR is always smaller than the actual mass ratio. Therefore, a binary with an mMMR larger than unity is a good candidate for having a massive secondary, which might be a black hole or a neutron star. This paper considers 10 956 OGLE short-period ellipsoidals observed towards the Galactic bulge. We re-analyse their modulation and identify 136 main-sequence systems with mMMR significantly larger than unity as candidates for having compact-object secondaries, assuming their observed periodic modulations reflect indeed the ellipsoidal effect. Obviously, one needs follow-up observations to find out the true nature of these companions.

中文翻译：

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在椭球变量中寻找休眠黑洞——III。OGLE BULGE 短期样本

这是一系列论文中的第三篇，该论文提出了一种算法，用于搜索具有大量、可能紧凑、看不见的次级的紧密二进制。对这种双星的检测是基于识别一颗显示出大椭球周期调制的恒星，这是由与其伴星的潮汐相互作用引起的。在该系列的第二篇论文中，我们提出了一种简单的方法来推导稳健的修正最小质量比 (mMMR)，该方法基于观察到的椭圆体振幅，而不知道初级质量和半径，假设初级填充其罗氏叶。新定义的 mMMR 总是小于实际质量比。因此，一个 mMMR 大于 1 的双星是拥有大质量次级星的良好候选者，它可能是黑洞或中子星。本文考虑了向银河核球观测到的 10 956 个 OGLE 短周期椭球体。我们重新分析了它们的调制，并确定了 136 个 mMMR 显着大于统一的主序列系统作为具有紧凑对象次级的候选者，假设它们观察到的周期性调制确实反映了椭圆体效应。显然，需要后续观察才能找出这些同伴的真实性质。