arXiv 2201.105122022-01-25astro-ph.IM

恒星强度干涉测量方法的比较

Comparing Different Approaches for Stellar Intensity Interferometry

Sebastian Karl, Andreas Zmija, Stefan Richter, Naomi Vogel, Dmitry Malyshev, Adrian Zink, Thilo Michel, Gisela Anton, Joachim von Zanthier, Stefan Funk

备注：: submitted to MNRAS
DOI：: 10.1093/mnras/stac489

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摘要：

恒星强度干涉仪在其相干时间内关联光子，可以克服现有振幅干涉仪的基线限制。强度干涉仪不依赖于光学元件的相位相干性，因此在没有高级光学器件和光组合延迟线的情况下起作用。然而，用实际的光学滤波器带宽（> 0.1 nm）观察到的星光的相干时间通常比检测系统的时间分辨率（> 10 ps）小得多，导致相关信号大大降低。在合理短的测量时间内达到高信噪比可以通过不同的方式实现：通过增加时间分辨率，这增加了相关信号高度，或者通过增加光子速率，这降低了测量的统计不确定性。我们目前的实验室测量采用这两种方法，并直接比较它们的信噪比。将为中小型光学望远镜设计的高时间分辨率干涉测量装置与计划安装在碟形直径大于10米的切伦科夫望远镜上的能够测量高光子率的装置进行比较，前者是为中小型光学望远镜设计的，因此光子率较低（直径小于数米）。我们使用氙灯作为模拟星光的普通光源。这两种设置都测量预期的相关信号，并在10 min和23 h之间的测量时间内在统计不确定性的预期散粒噪声限值下工作。我们讨论了定量的测量结果的差异，并给出了一个合适的操作制度的概述，为每个干涉仪的概念。

英文摘要：

Stellar intensity interferometers correlate photons within their coherence time and could overcome the baseline limitations of existing amplitude interferometers. Intensity interferometers do not rely on phase coherence of the optical elements and thus function without high grade optics and light combining delay lines. However, the coherence time of starlight observed with realistic optical filter bandwidths (> 0.1 nm) is usually much smaller than the time resolution of the detection system (> 10 ps), resulting in a greatly reduced correlation signal. Reaching high signal to noise in a reasonably short measurement time can be achieved in different ways: either by increasing the time resolution, which increases the correlation signal height, or by increasing the photon rate, which decreases statistical uncertainties of the measurement. We present laboratory measurements employing both approaches and directly compare them in terms of signal to noise ratio. A high time-resolution interferometry setup designed for small to intermediate size optical telescopes and thus lower photon rates (diameters < some meters) is compared to a setup capable of measuring high photon rates, which is planned to be installed at Cherenkov telescopes with dish diameters of > 10 m. We use a Xenon lamp as a common light source simulating starlight. Both setups measure the expected correlation signal and work at the expected shot-noise limit of statistical uncertainties for measurement times between 10 min and 23 h. We discuss the quantitative differences in the measurement results and give an overview of suitable operation regimes for each of the interferometer concepts.

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