Stellar surface imaging

Rachael M. Roettenbacher

doi:10.1117/12.2561881

13 December 2020 Stellar surface imaging

Rachael M. Roettenbacher

Proceedings Volume 11446, Optical and Infrared Interferometry and Imaging VII; 114460B (2020) https://doi.org/10.1117/12.2561881
Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online Only

Abstract

Long-baseline optical interferometry has provided a method with which stars are not only resolved, but directly imaged. Resolving features on stellar surfaces is becoming routine for observers using the Center for High Angular Resolution Astronomy (CHARA) Array or the Very Large Telescope Interferometer (VLTI), in particular. The CHARA Array presently has six 1-m telescopes at permanent locations with baselines ranging from 34-331 m.¹ Currently for imaging, the six CHARA Array telescopes are combined with the Michigan InfraRed Combiner-eXeter (MIRC-X; formerly the Michigan Infrared Combiner, MIRC).² Working in H- and J -bands, MIRC-X provides an angular resolution of θ_H ∼ 0.5 mas and θ_J ∼ 0.4 mas, respectively. Four telescopes at a time can be combined at VLTI, either the 8.2-m Unit Telescopes (UTs) or the 1.8-m Auxiliary Telescopes (ATs). The ATs can be moved to provide multiple configurations to increase the possible baselines (up to 130 m). The Precision Integrated-Optics Near-Infrared Imaging ExpeRiment (PIONIER),³ which operates in H-band (θ_H ∼ 1.3 mas), is the current beam combiner frequently used for imaging. In the following sections, the types of stars imaged by long-baseline optical interferometry will be discussed with significant astrophysical results highlighted.

Conference Presentation

Citation Download Citation

Rachael M. Roettenbacher "Stellar surface imaging", Proc. SPIE 11446, Optical and Infrared Interferometry and Imaging VII, 114460B (13 December 2020); https://doi.org/10.1117/12.2561881

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