Laser Guided Space Interferometer

被引：3

作者：

Pogorelyuk, Leonid ^{[1
]}

Serra, Paul ^{[1
]}

Kacker, Shreeyam ^{[1
]}

Vlahakis, Sophia ^{[1
]}

Belsten, Nicholas ^{[1
]}

Rau, Gioia

Carpenter, Kenneth G. ^{[2
]}

Pueyo, Laurent ^{[3
]}

Monnier, John D. ^{[4
]}

Douglas, Ewan S. ^{[5
]}

Cahoy, Kerri L. ^{[1
]}

机构：

[1] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA

[2] NASA Goddard Space Flight Ctr, Greenbelt, MD USA

[3] Space Telescope Sci Inst, Baltimore, MD USA

[4] Univ Michigan, Dept Astron & Steward Observ, Ann Arbor, MI USA

[5] Univ Arizona, Dept Astron & Steward Observ, Tucson, AZ USA

来源：

OPTICAL AND INFRARED INTERFEROMETRY AND IMAGING VIII | 2022年 / 12183卷

关键词：

Interferometery; Laser Guide Star; SmallSat; CubeSat; CHARA ARRAY; SATELLITE; OPTICS;

D O I：

10.1117/12.2630605

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The mirrors of astronomical interferometers need to be aligned within a fraction of a wavelength relative to one another. This would be especially challenging for optical instruments with mirrors separated by hundreds of meters flying in Earth's orbit. However, in this work, we show that this alignment can be achieved by means of: (i) flying the mirror cluster in a particular orbital configuration; (ii) closing a coarse positioning loop using GNSS (Global Navigation Satellite System); and (iii) closing a fine wavefront-control loop using light from a laser guide star. The orbital configuration is designed to keep the mirrors passively pointing at the target star (up to a small orbital perturbation) while the interferometer cluster is orbiting and changing its baseline. The laser guide star would be flying in the same orbit but in the opposite direction. In medium- or high-Earth orbit, the interferometer would be able to observe a star for several hours per orbit. In this work, we analyzed the performance of an optical space interferometer consisting of nine 20 cm mirrors mounted on CubeSats and flying 3 km apart (together with a combiner and a laser guide star small satellite). This configuration supports a resolution of 0.04 milliarcseconds - an order of magnitude better than current ground-based interferometers. We estimate the performance of this system imaging stellar surfaces assuming perfect wavefront estimation and control.

引用

页数：14

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