论文标题
通过强度干涉法实现丽莎的极化预测
Towards a Polarisation Prediction for LISA via Intensity Interferometry
论文作者
论文摘要
预计将通过LISA或类似的任务在重力波（GW）中检测到具有轨道周期的紧凑型银河系系统。目前，这些所谓的验证二进制文件为GW频率和振幅提供了预测。一个完整的极化预测将提供一种校准Lisa和其他GW观测值的新方法，但需要解决天空上二进制的方向，目前是不可能的。我们建议使用KM尺度的光学强度干涉法来确定难以捉摸的二进制方向，从而预测GW极化的方法。最有前途的候选人是CD-30 $^{\ circ} $ 11223，由$ M_B = 12 $的热氦小子组成，并且在几乎边缘的轨道上，具有70.5分钟。我们估计，较明亮的恒星潮汐延伸6％。解决潮汐拉伸将提供二进制方向。所需的分辨率远远超出了当前的任何工具，但远远超出了当前的技术。我们考虑的场景中，一系列带有KM尺度基线的望远镜和/或非常大的望远镜（VLT）和极大的望远镜（ELT）配备了最近开发的Kilo-Pixel Sub-NS单光子计数器，并用于强度干扰素。我们估计，VLT和ELT的团队可以在2 $σ$的观察中以2 $σ$信心测量$ \ pm 1^{\ circ} $。
Compact Galactic binary systems with orbital periods of a few hours are expected to be detected in gravitational waves (GW) by LISA or a similar mission. At present, these so-called verification binaries provide predictions for GW frequency and amplitude. A full polarisation prediction would provide a new method to calibrate LISA and other GW observatories, but requires resolving the orientation of the binary on the sky, which is not currently possible. We suggest a method to determine the elusive binary orientation and hence predict the GW polarisation, using km-scale optical intensity interferometry. The most promising candidate is CD-30$^{\circ}$ 11223, consisting of a hot helium subdwarf with $m_B = 12$ and a much fainter white dwarf companion, in a nearly edge-on orbit with period 70.5 min. We estimate that the brighter star is tidally stretched by 6%. Resolving the tidal stretching would provide the binary orientation. The resolution needed is far beyond any current instrument, but not beyond current technology. We consider scenarios where an array of telescopes with km-scale baselines and/or the Very Large Telescope (VLT) and Extremely Large Telescope (ELT) are equipped with recently-developed kilo-pixel sub-ns single-photon counters and used for intensity interferometry. We estimate that a team-up of the VLT and ELT could measure the orientation to $\pm 1^{\circ}$ at 2$σ$ confidence in 24 hours of observation.
