Validating the Angular Sizes of Red Clump Stars with Intensity Interferometry

TL;DR

This paper proposes using intensity interferometry to measure the angular sizes of Red Clump stars, offering a complementary and potentially more practical method to traditional amplitude interferometry for calibrating stellar distances.

Contribution

It develops a framework for extracting limb-darkened angular diameters from intensity interferometry measurements and demonstrates its feasibility for Red Clump stars.

Findings

Intensity interferometry can achieve <1% angular size uncertainties in 2 hours for HD 17652.

Shorter wavelength observations probe secondary visibility maxima, enabling independent error checks.

Using telescope arrays like CTA can make intensity interferometry a practical tool for stellar size validation.

Abstract

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.