|
|
|
|
|
|
| Experimental Ground Validation of Spectral Quality of the Chang’E-5 Lunar Mineralogical Spectrometer |
| CAI Ting-ni1, 2, LI Chun-lai1*, HE Zhi-ping3, REN Xin1, LIU Bin1, XU Rui3 |
1. Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
2. School of Physical and Science, University of Chinese Academy of Sciences, Beijing 100049, China
3. Shanghai Institute of Technical Physics of the Chinese Academy of Sciences, Shanghai 200083, China |
|
|
|
|
Abstract As the last stage of China’s Chang’e (CE) lunar program, the Chang’e-5 lunar rover will land on the surface of moon, obtain lunar samples and then return back to Earth. The Lunar Mineralogical Spectrometer (LMS) is one of CE-5’s onboard payloads, which is an important data source for the lunar exploration project. LMS spectral data is used to identify the composition of lunar minerals to aid in rock classification and stratigraphic analysis—all of which provide data required to support research on moon formation, geologic evolution and rock-water interactions. Compared with the CE-3 VIS/NIR imaging spectrometer (VNIS), the CE-5 LMS extends the spectral range from 450～2 400 to 480～3 200 nm. In addition to identifying the major minerals such as pyroxene and olivine, it can also detect absorption peaks around 3 000 nm characteristic of hydrous minerals. In addition, Chang’e-5 will sample thematerialbelow the surface of the moon, and LMS can detect the area before and after sampling, to analyze the spectral characteristics of lunar soil under different depths and weathering degrees, then compared with the laboratory spectra of the later return samples. In order to ensure the reliability of LMS lunar data, a pre-flight LMS ground validation experiment was carried out, using a variety of minerals and mineral mixed samples, collecting the detection data of LMS under different test environment, combining with a standard instrument to analyze the spectral quality. In this paper, spectral uncertainty parameters of all experiment samples were calculated and evaluated. Moreover, the LMS spectral data were consistent with those simultaneously obtained from standard comparison spectrometers under the same conditions, indicating that LMS could effectively identify the spectral profile and absorption peak of the targets.
|
|
Received: 2017-12-18
Accepted: 2018-04-22
|
|
|
|
Corresponding Authors:
LI Chun-lai
E-mail: licl@nao.cas.cn
|
|
[1] Cheek L C, Hanna K, Pieters C M, et al. Journal of Geophysical Research: Plants, 2013，118(9)：1805.
[2] Di Kaichang, Xu Bin, Peng Man, et al. Planetary and Space Science, 2016，120：103.
[3] Dingwell D B. Geochimica et Cosmochimica Acta, 1992，56(9)：3403.
[4] Foing B H, Racca G D, Marini A, et al. Advances in Space Research, 2006，37：6.
[5] Green R O, Pieters C M, Mouroulis P, et al. Journal of Geophysical Research: Planets, 2011，116(E10): 6.
[6] Hapke B. Icarus, 1986，67(2)：264.
[7] Harald H, James W. Reviews in Mineralogy and Geochemistry, 2006，60：1.
[8] Isaacson P J, Pieters C M. Icarus, 2010，210(1)：8.
[9] Jin S, Arivazhagan S, Araki H. Advances in Space Research, 2013，52(2)：285.
[10] Keller J W, Petro N E, Vondrak R R. Icarus, 2016，273(SI)：2.
[11] Klima R L, Dyar M D, Pieters C M. Meteoritics & Planetary Science, 2011，46(3)：379.
[12] Klima R, Hapke B. Meteoritics & Planetary Science, 2012，47(8)：1403.
[13] Liu Bin, Liu Jianjun, Zhang Guangliang, et al. Research in Astronomy and Astrophysics, 2013，13(7)：862.
[14] Pieters C M, Head J W, Sunshine J M, et al. Journal of Geophysical Research: Planets, 1993，98(E9)：17127.
[15] Pieters C M, Staid M I, Fischer E M, et al. Science, 1994，266(5192)：1844.
[16] Sunshine J M, Mcfadden L A, Pieters C M. Icarus, 1993，105(1)：79.
[17] Varatharajan I, Srivastava N, Murty S. Icarus, 2014，236：56.
[18] Yamamoto, Nakamura Ryosuke, Matsunaga Tsuneo, et al. Nature Geoscience, 2010，3(8)：533. |
|
|
|
