Interferometry from the Moon

Details Interferometry from the Moon Interferometry from the Moon

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.354...51l&link_type=abstract

In ESA, Targets for Space-Based Interferometry p 51-55 (SEE N93-31750 12-89)

Astronomy and Astrophysics

Astronomy

Astronomical Interferometry, Interferometers, Lunar Based Equipment, Spaceborne Astronomy, Deployment, Design Analysis, Maintenance

Scientific paper

Advantages and disadvantages of the Moon for the site for large optical interferometers as opposed to Earth orbits are addressed. The permanent darkness, in some polar craters, avoids the contamination of long, unprotected, coude beams by solar straylight. The optics in such sites can be cooled passively, as well as the detectors which may also be buried for protection against energetic particles. Long baselines, up to perhaps 10 km, may be possible. Unlike orbital sites, however, lunar sites require delicate optical delay lines or movable telescopes to deal with a substrate which cannot be rotated as desired for pointing various objects. This, and the automated deployment, is achieved with robotic walking telescopesin the case of the Lunar Optical Very Large Array (LOYLA) concept. The design principles, fine geometry control, optical structure, automated deployment, maintenance and power of lunar telescopes are discussed. LOYLA's scientific goals are considered. Among these is the lunar Optical Very Large Array concept - the imaging of exoplanets, with a few pixels of resolution on their disk in some cases. The construction of the ground based OVLA, which has a similar design and which may provide valuable operating experience, is also discussed.

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