通过强度干涉仪验证红团星的角直径
Validating the Angular Sizes of Red Clump Stars with Intensity Interferometry
AI总结：
本文探讨利用强度干涉仪测量红团星的角直径，以验证其表面亮度-颜色关系，通过多波段观测和望远镜阵列减少观测时间，提高红团星校准样本的角直径精度。
摘要：
红团星的表面亮度-颜色关系为精确距离阶梯测量提供了关键基础，包括对大麦哲伦星云的1%距离确定。当前的SBC校准依赖于通过甚大望远镜干涉仪进行的长基线光学干涉测量获得的附近红团星角直径测量。本文探讨了利用强度干涉仪测量红团星的边缘暗化角直径的应用，提供了一种补充传统幅度干涉测量的方法。我们描述了从强度干涉测量的平方可见度测量中提取角直径的框架，并通过恒星大气模型考虑边缘暗化。对于红团星HD~17652，我们表明在H波段基线匹配PIONIER（约100米）的情况下，通过测量可见度函数的主峰可以在2小时内实现<1%的角直径不确定性，从而与现有测量进行直接比较。关键的是，在更短的波长下探测二次可见度最大值，提供独立的测量和系统误差检查，这些误差大多对边缘暗化假设不敏感。利用多波段同时观测的多乘优势和望远镜阵列（如切伦科夫望远镜阵列观测站）提供的大量基线数量，可以将观测时间减少到实用水平，使强度干涉仪成为验证红团星校准样本子集角直径的可行工具。
英文摘要：
The surface-brightness-color (SBC) relationship for Red Clump stars provides a critical foundation for precision distance ladder measurements, including the 1\% distance determination to the Large Magellanic Cloud. Current SBC calibrations rely on angular diameter measurements of nearby Red Clump stars obtained through long-baseline optical interferometry using the Very Large Telescope Interferometer. We explore the application of intensity interferometry to measure limb-darkened angular diameters of Red Clump stars, offering a complementary approach to traditional amplitude interferometry. We describe the framework for extracting angular diameters from squared visibility measurements in intensity interferometry, accounting for limb darkening through the stellar atmosphere models. For the Red Clump star HD~17652, we show that intensity interferometry in the $H$ band at baselines matching PIONIER ($\sim$100~m) could achieve $<1$\% angular size uncertainties in 2-hour exposures by measuring the primary peak of the visibility function, enabling direct comparison with existing measurements. Critically, observations at shorter wavelengths probe the secondary visibility maximum, providing independent checks of both measurement and systematic errors that are largely insensitive to limb-darkening assumptions. Exploiting the multiplex advantage of simultaneous multi-bandpass observations and the large number of baselines available with telescope arrays such as the Cherenkov Telescope Array Observatory can reduce observing times to practical levels, making intensity interferometry a viable tool for validating the angular sizes for a subset of the Red Clump star calibration sample.
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