Optical/UV/IR interferometry from lunar baselines

Details Optical/UV/IR interferometry from lunar baselines Optical/UV/IR interferometry from lunar baselines

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994adspr..14..107l&link_type=abstract

Advances in Space Research, vol. 14, no. 6, p. (6)107-(6)113

Astronomy and Astrophysics

Astronomy

1

Astronomical Interferometry, Lunar Atmosphere, Lunar Bases, Very Large Array (Vla), Angular Resolution, Atmospheric Attenuation, Ultraviolet Radiation, Moon, Space, Utilization, Astronomy, Science Aspects, Interferometry, Moon-Based Observations, Telescopes, Technical Aspects, Wavelength, Ultraviolet, Infrared, Interferometers, Position (Location), Power

Scientific paper

The Earth-based optical interferometers currently operated or under construction provide a vast improvement of the angular resolution, but remain severely affected by the inhomogeneity of the atmosphere and its absorbtion of ultra-violet wavelengths. In these respects, sites in Earth orbit or on the Moon are expected to provide an observational breakthrough. On the Moon, the darkness favors long coude beams between the telescopes and the central station, with low levels of stray light. The rigid substrate helps achieving a stable geometry, and detectors may be buried for protection against solar protons and cosmic rays. In contrast with other concepts proposed for the Moon, the Lunar Optical Very Large Array has telescopes which move slowly during the observation in order to maintain the equality of optical path lengths. It can change its geometry according to observing needs, and progressively expand its baselines. Starting with the delivery of 3 to 6 telescopes, and their automated deployment, additional deliveries at intervals of 2 to 5 years can provide replacement for failed components and increase the number of telescopes up to several dozens.

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