arXiv 2501.098942025-01-17astro-ph.IM

使用0.25米望远镜开展的天狼星强度干涉仪观测结果

Intensity Interferometer Results on Sirius with 0.25 m Telescopes

Thomas J. Mozdzen, Richard M. Scott, Ricardo R. Rodriguez, Philip D. Mauskopf

AI总结：

本研究利用城市后院的0.25米小型低成本望远镜，在3.3米间距下成功测得天狼星的平方可见度，验证了小型望远镜用于亮星强度干涉测量的可行性，为后续提升灵敏度、构建高分辨天体观测系统奠定基础。

摘要：

我们展示了在城市后院环境中，使用小型0.25米牛顿式望远镜，在3.3米的望远镜间距下成功测量天狼星平方可见度的结果。小型强度干涉仪的核心科学目标一直是测量恒星的角直径。低抖动时间标记设备与Single Photon Avalanche Detectors（单光子雪崩探测器）的最新进展，使得利用小型低成本望远镜探测二阶光子相关信号成为可能。我们以天狼星为目标恒星，在589.3纳米波长、匹配的1.2纳米宽滤光片条件下，观测到每个探测器的光子计数率约为1.9 Mcps，并在3.3米望远镜间距下测得空间平方可见度为$|V_{12}(3.3\text{m})|^2 = 0.94\neq0.16$。经过13.55小时的积分，测得的探测显著性约为7σ。测得的可见度不确定性包含仪器响应函数的不确定性。该平方可见度与预期值$0.94\neq0.01$高度吻合。这些结果表明，使用小型低成本望远镜开展亮星强度干涉测量是可行的。这为通过进一步切实改进仪器响应抖动、增加光谱波段数量和望远镜数量来简单提升灵敏度提供了可能，最终可构建能够分辨类星体、白矮星和银河系造父变星等天体的系统。

英文摘要：

We present the successful measurement of the squared visibility of Sirius at a telescope separation of 3.3 m using small 0.25 m Newtonian-style telescopes in an urban backyard setting. The primary science goal for small-scale intensity interferometers has been to measure the angular diameters of stars. Recent advances in low jitter time-tagging equipment and Single Photon Avalanche Detectors have made the detection of second-order photon correlation signals feasible with small low-cost telescopes. Using Sirius as a target star, we observe a photon count rate of $\sim$1.9 Mcps per detector with matched 1.2 nm wide filters at 589.3 nm and measured the spatial squared visibility at a telescope separation of 3.3 m to be $|V_{12}(3.3\text{m})|^2 = 0.94\pm0.16$. The measured detection significance is $\sim7 σ$ after 13.55 h of integration. The uncertainty in the measured visibility includes uncertainty in the instrument response function.The squared visibility agrees closely with the expected value of $0.94\pm0.01$. These results demonstrate that using small low-cost telescopes is feasible for intensity interferometry of bright stars. This enables a simple scaling in sensitivity by further realistic improvements in the instrument response jitter as well as increasing both the number of spectral bands and the number of telescopes towards systems capable of resolving objects such as quasars, white dwarfs, and galactic Cepheid variable stars.

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