Intensity interferometer results on Sirius with 0.25 m telescopes

被引：0

作者：

Mozdzen, Thomas J. ^{[1
]}

Scott, Richard M. ^{[1
]}

Mauskopf, Philip D. ^{[1
]}

Rodriguez, Ricardo R. ^{[2
]}

机构：

[1] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA

[2] Case Western Reserve Univ, Cleveland, OH 44106 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2025年 / 537卷 / 03期

关键词：

instrumentation: detectors; instrumentation: interferometers; techniques: high angular resolution; techniques: interferometric; telescopes; stars: fundamental parameters; I;

D O I：

10.1093/mnras/staf226

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

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 similar to 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(3.3m)|(2) = 0.94 +/- 0.16. The measured signal-to-noise ratio of the detection is similar to 7 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 +/- 0.01. 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.

引用

页码：2527 / 2534

页数：8

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