标题： 非因果且不相关光学类星体对的可观测性用于量子力学实验 显示英文标题

标题： Observability of Acausal and Uncorrelated Optical-Quasar Pairs for Quantum-Mechanical Experiments

摘要： 观测天空中近乎相反方向上的高红移源，可以通过光行时论证来保证它们发射光子之间的非因果性。 其中一个用途是可以生成真正的随机数，通过使用两台独立的望远镜感应这些光子，每台望远镜都根据最新到达的颜色切换开关；例如，用于自主控制量子力学（QM）实验。 尽管这一方法已在遥远的类星体上得到演示，但那些并非完全非因果对，因为从地面任何单一天文台同时观测到的对组受到限制。 在光学波段，如此微弱的源也需要大口径望远镜以避免在高速相机帧率下成像时采样假设：要么它们之间未被感应的固有相关性，要么等效相关的噪声可能破坏纯粹随机性的期望。 考虑到了一种可能会破坏量子力学测试的情况。 基于此，为任意两个地面站点建模了允许的几何形状和仪器限制，并对其数据进行了模拟。 为了比较，展示了双子座8米望远镜的测光分析，使用存档数据中的分离良好的明亮恒星，这些数据由仪器'Alopeke'（在夏威夷的双子座北）和'Zorro'（在智利的双子座南）在同一时间（中心波长分别为562纳米和832纳米）以17赫兹的帧率获取。 没有发现流量的相关性，校准了一个解析模型，预测了在相同仪器下以50赫兹信号与噪声比超过50的搜索位置。 最后，介绍了软件PDQ（Predict Different Quasars），该软件搜索已知类星体的大目录，报告亮度和可见度适合验证非因果、无相关的光子的那些类星体。 显示英文摘要

摘要： Viewing high-redshift sources at near-opposite directions on the sky can assure, by light-travel-time arguments, acausality between their emitted photons. One utility would be true random-number generation, by sensing these via two independent telescopes that each flip a switch based on those latest-arrived colours; for example, to autonomously control a quantum-mechanical (QM) experiment. Although demonstrated with distant quasars, those were not fully acausal pairs, which are restricted in simultaneous view from the ground at any single observatory. In optical light such faint sources also require large telescope aperture to avoid sampling assumptions when imaged at fast camera framerates: either unsensed intrinsic correlations between them or equivalently-correlated noise may ruin the expectation of pure randomness. One such case which could spoil a QM test is considered. Based on that, allowed geometries and instrumental limits are modelled for any two ground-based sites, and their data simulated. To compare, an analysis of photometry from the Gemini twin 8-m telescopes is presented, using archival data of well-separated bright stars, obtained with the instruments 'Alopeke (on Gemini-North in Hawai'i) and Zorro (on Gemini-South in Chile) simultaneously in two bands (centred at 562 nm and 832 nm) with 17 Hz framerate. No flux correlation is found, calibrating an analytic model, predicting where a search at signal-to-noise over 50 at 50 Hz with the same instrumentation can be made. Finally, the software PDQ (Predict Different Quasars) is presented which searches a large catalogue of known quasars, reporting those with brightness and visibility suitable to verify acausal, uncorrelated photons at those limits.