Abstract
Lunar reflectance data is useful not only for lithorogical identification of lunar surface but for radiometric calibration and determination of exposure time for optical sensors of lunar probe. To gain lunar reflectance, multi-band images of the lunar surface and those of some standard stars had been acquired with a liquid-crystal tunable filter (LCTF) telescope at the peak of Mt. Haleakala (Hawaii, USA) at 5 bands (650, 750, 900, 950, and 1000 nm) by the members of Advanced Lunar Imaging Spectrometer (ALIS) project. LCTF telescope is a multi-band tele-scope using a tunable liquid-crystal filter covering 650 - 1100 nm. It is composed of a refract-ing telescope (Vixen, ED80S) equipped with a cooling CCD camera (Apogee, U260) and a tunable liquid-crystal filter (Cambridge Res. Inc., NIR-07). Obtained data indicates that the reflectance data of Clementine UVVIS is too high. The reflectance value of Clementine is about 60 – 70 % brighter than our new data. The lunar reflectance images, the software tools, and the raw data are open to public at my web site. This study reports the method of deriving the lunar reflectance images from the observed images and the ideas for applying the data to lithorogical identification, exposure determination, etc.
