Observations with the Southern Connecticut Stellar Interferometer. I. Instrument Description and First Results

TL;DR

This paper presents the design, implementation, and initial results of a new intensity interferometer using portable telescopes and single-photon detectors, demonstrating its capability to measure stellar angular diameters.

Contribution

It introduces a novel, portable intensity interferometer setup and provides first observational results, including stellar diameter estimates, demonstrating its potential for astronomical measurements.

Findings

Detected correlation peaks at 6.76-sigma level for unresolved stars

Measured angular diameter of Arcturus > 15 mas

Estimated Vega's diameter between 0.8 and 17 mas

Abstract

We discuss the design, construction, and operation of a new intensity interferometer, based on the campus of Southern Connecticut State University in New Haven, Connecticut. While this paper will focus on observations taken with an original two-telescope configuration, the current instrumentation consists of three portable 0.6-m Dobsonian telescopes with single-photon avalanche diode (SPAD) detectors located at the Newtonian focus of each telescope. Photons detected at each station are time-stamped and read out with timing correlators that can give cross-correlations in timing to a precision of 48 ps. We detail our observations to date with the system, which has now been successfully used at our university in 16 nights of observing. Components of the instrument were also deployed on one occasion at Lowell Observatory, where the Perkins and Hall telescopes were made to function as an intensity interferometer. We characterize the performance of the instrument in detail. In total, the observations indicate the detection of a correlation peak at the level of 6.76-sigma when observing unresolved stars, and consistency with partial or no detection when observing at a baseline sufficient to resolve the star. Using these measurements we conclude that the angular diameter of Arcturus is larger than 15 mas, and that of Vega is between 0.8 and 17 mas. While the uncertainties are large at this point, both results are consistent with measures from amplitude-based long baseline optical interferometers.