AbstractThe 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 absorption of ultra-violet wavelenghts. 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 coudé 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.
Optical/UV/IR interferometry from lunar baselines
Advances in Space Research ; 14 , 6 ; 107-113
1994-01-01
7 pages
Article (Journal)
Electronic Resource
English
Optical/UV/IR Interferometry from Lunar Baselines
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