Global lunar-surface mapping experiment using the Lunar Imager/Spectrometer on SELENE

By J. Haruyama, T. Matsunaga, M. Ohtake, T. Morota, C. Honda, Y. Yokota, M. Torii, Y. Ogawa, Lism Working Group. 2008

242 citations recorded by the source corpus.

The Moon is the nearest celestial body to the Earth. Understanding the Moon is the most important issue confronting geosciences and planetary sciences. Japan will launch the lunar polar orbiter SELENE (Kaguya) (Kato et al., 2007) in 2007 as the first mission of the Japanese long-term lunar exploration program and acquire data for scientific knowledge and possible utilization of the Moon. An optical sensing instrument called the Lunar Imager/Spectrometer (LISM) is loaded on SELENE. The LISM requirements for the SELENE project are intended to provide high-resolution digital imagery and spectroscopic data for the entire lunar surface, acquiring these data for scientific knowledge and possible utilization of the Moon. Actually, LISM was designed to include three specialized sub-instruments: a terrain camera (TC), a multi-band imager (MI), and a spectral profiler (SP). The TC is a high-resolution stereo camera with 10-m spatial resolution from a SELENE nominal altitude of 100 km and a stereo angle of 30° to provide stereo pairs from which digital terrain models (DTMs) with a height resolution of 20 m or better will be produced. The MI is a multi-spectral imager with four and five color bands with 20 m and 60 m spatial resolution in visible and near-infrared ranges, which will provide data to be used to distinguish the geological units in detail. The SP is a line spectral profiler with a 400-m-wide footprint and 300 spectral bands with 6–8 nm spectral resolution in the visible to near-infrared ranges. The SP data will be sufficiently powerful to identify the lunar surface’s mineral composition. Moreover, LISM will provide data with a spatial resolution, signal-to-noise ratio, and covered spectral range superior to that of past Earth-based and spacecraft-based observations. In addition to the hardware instrumentation, we have studied operation plans for global data acquisition within the limited total data volume allotment per day. Results show that the TC and MI can achieve global observations within the restrictions by sharing the TC and MI observation periods, adopting appropriate data compression, and executing necessary SELENE orbital plane change operations to ensure global coverage by MI. Pre-launch operation planning has resulted in possible global TC high-contrast imagery, TC stereoscopic imagery, and MI 9-band imagery in one nominal mission period. The SP will also acquire spectral line profiling data for nearly the entire lunar surface. The east-west interval of the SP strip data will be 3–4 km at the equator by the end of the mission and shorter at higher latitudes. We have proposed execution of SELENE roll cant operations three times during the nominal mission period to execute calibration site observations, and have reached agreement on this matter with the SELENE project. We present LISM global surface mapping experiments for instrumentation and operation plans. The ground processing systems and the data release plan for LISM data are discussed briefly.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a013325b29bfa14176081a2ffb1c263b4b14e868

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Citations in the corpus

How old are young lunar craters (2012, methodology): “…0.5 to 2.0 m/pixel) and Wide-angle Camera (WAC; ≤100 m/pixel) [Robinson et al., 2010], as well as the SELENE/Kaguya Terrain Camera (TC; 10 m/pixel) [Haruyama et al., 2008], we update CSFDmeasurements for young craters North Ray, Tycho, and Copernicus, which represent the y axis of the chronology.”
Possible mantle origin of olivine around lunar impact basins detected by SELENE (2010, methodology): “Taking into account the local geologic context, based on images obtained by Kaguya’s Multiband Imager (MI) or Terrain Camera (TC) during the SP observatio”
Possible lunar lava tube skylight observed by SELENE cameras (2009, background): “Lava-tube formation is a significant factor controlling the distribution of volcanic materials on the Moon [e.g., Greeley, 1987; Pinkerton and Wilson, 1994; Keszthelyi, 1995; Sakimoto et al., 1997].”
Performance and scientific objectives of the SELENE (KAGUYA) Multiband Imager (2008, unknown): “Global, detailed investigation of the topography and geographical features of the Moon will be derived through TC data (Haruyama et al., 2008, this issue).”
Gravity and Topography of the Terrestrial Planets (2015, methodology): “In addition to including laser altimeters, the acquisition of stereo imagery from these missions has led to the construction of both regional and global terrane models (e.g., Haruyama et al., 2008; Scholten et al., 2012).”
Lunar Reconnaissance Orbiter Camera (LROC) Instrument Overview (2010, methodology): “…common minerals found at the lunar surface and will complement Clementine UVVIS (415, 750, 900, 950, 1000 nm) and NIR datasets (1100, 1250, 1500, 2000, 2600, 2780 nm) (Nozette et al. 1994) as well as VIS-NIR data being collected by Chandrayaan-1 and Selene (Haruyama et al. 2008; Green et al. 2007).”