The second phase of the Chang＇E Program （also named Chang＇E-3） has the goal to land and perform in-situ detection on the lunar surface. A VIS/NIR imaging spectrometer （VNIS） will be carded on the Chang＇E-3 lunar rover to detect the distri-bution of lunar minerals and resources. VNIS is the first mission in history to perform in-situ spectral measurement on the surface of the Moon, the reflectance data of which are fundamental for interpretation of lunar composition, whose quality would greatly affect the accuracy of lunar element and mineral determination. Until now, in-situ de-tection by imaging spectrometers was only performed by rovers on Mars. We firstly review reflectance conversion methods for rovers on Mars （Viking landers, Pathfinder and Mars Exploration rovers, etc）. Secondly, we discuss whether these conversion methods used on Mars can be applied to lunar in-situ detection. We also applied data from a laboratory bidirectional reflectance distribution function （BRDF） using simu- lated lunar soil to test the availability of this method. Finally, we modify reflectance conversion methods used on Mars by considering differences between environments on the Moon and Mars and apply the methods to experimental data obtained from the ground validation of VNIS. These results were obtained by comparing reflectance data from the VNIS measured in the laboratory with those from a standard spectrometer obtained at the same time and under the same observing conditions. The shape and amplitude of the spectrum fits well, and the spectral uncertainty parameters for most samples are within 8%, except for the ilmenite sample which has a low albedo. In conclusion, our reflectance conversion method is suitable for lunar in-situ detection.
Bin LiuJian-Zhong LiuGuang-Liang ZhangZong-Cheng LingJiang ZhangZhi-Ping HeBen-Yong YangYong-Liao Zou
