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A ground-based observation of the LCROSS impact events using the Subaru Telescope |
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| Authors: | Peng K Hong Seiji Sugita Yasuhito Sekine Naruhisa Takatoh Tetsuharu Fuse Hideyo Kawakita Eliot F Young Kosuke Kurosawa Junichi Haruyama Toshihiko Kadono Shunichi Kamata Tomohiko Sekiguchi Hirotomo Noda |
| Institution: | a Department of Complexity Science and Engineering, The University of Tokyo, Kashiwa, Chiba 277-8561, Japan b Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720, USA c Kashima Space Research Center, National Institute of Information and Communications Technology, Kashima, Ibaraki 314-8501, Japan d Department of Physics, Kyoto Sangyo University, Kita-ku, Kyoto 603-8555, Japan e NASA Ames Research Center, Moffett Field, CA 94035, USA f Southwest Research Institute, San Antonio, TX 78238, USA g Hawaii Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA h Department of Earth and Planetary Science, The University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan i Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 252-5210, Japan j National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan k Institute of Laser Engineering, Osaka University, Suita, Osaka 565-0871, Japan l National Institute of Advanced Industrial Science and Technology, Tsukuba, Ibaraki 305-8568, Japan m Hokkaido University of Education, Kita-ku, Sapporo 002-8501, Japan n National Astronomical Observatory of Japan, Mizusawa, Oshu, Iwate 023-0861, Japan |
| Abstract: | The Lunar Crater Observation and Sensing Satellite (LCROSS) mission was an impact exploration searching for a volatile deposit in a permanently shadowed region (PSR) by excavating near-surface material. We conducted infrared spectral and imaging observations of the LCROSS impacts from 15 min before the first collision through 2 min after the second collision using the Subaru Telescope in order to measure ejecta dust and water. Such a ground-based observation is important because the viewing geometry and wavelength coverage are very different from the LCROSS spacecraft. We used the Echelle spectrograph with spectral resolution λ/Δλ ∼ 10,000 to observe the non-resonant H2O rotational emission lines near 2.9 μm and the slit viewer with a K′ filter for imaging observation of ejecta plumes. Pre-impact calculations using a homogeneous projectile predicted that 2000 kg of ejecta and 10 kg of H2O were excavated and thrown into the analyzed area immediately above the slit within the field of view (FOV) of the K′ imager and the FOV of spectrometer slit, respectively. However, no unambiguous emission line of H2O or dust was detected. The estimated upper limits of the amount of dust and H2O from the main Centaur impact were 800 kg and 40 kg for the 3σ of noise in the analyzed area within the imager FOV and in the slit FOV, respectively. If we take 1σ as detection limit, the upper limits are 300 kg and 14 kg, respectively. Although the upper limit for water mass is comparable to a prediction by a standard theoretical prediction, that for dust mass is significantly smaller than that predicted by a standard impact theory. This discrepancy in ejecta dust mass between a theoretical prediction and our observation result suggests that the cratering process induced by the LCROSS impacts may have been substantially different from the standard cratering theory, possibly because of its hollow projectile structure. |
| Keywords: | Moon Surface Ices Infrared observations Impact processes |
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