Fig. 4: The OH absorption features comparison between the lunar mineralogical spectrometer (LMS) in situ spectra and remote sensing spectra of the Moon Mineralogy Mapper (M3).
From: Evidence of water on the lunar surface from Chang’E-5 in-situ spectra and returned samples
a The examples of LMS 0012 (red solid line), the representative broader 3 μm (dashed line), and 2.8 μm (dotted line) absorption features of M3. b The examples of two M3 spectra of Chang’E-5 landing site obtained at different times, the representative broader 3 μm (dashed line) and 2.8 μm (dotted line) absorption features of M3. c The lunar surface temperatures derived from three thermal correction models (Clark model, Li model, and Groussin model, see “Methods”) at the time of LMS in situ observations. The average temperatures derived from three models are 347.9, 351.2, and 348.1 K. The purple curve shows the variation of the lunar surface temperature with local time fitted from the Diviner data of the Chang’e-5 landing site at different lunar local times. d–f are projections of LMS ~2.85 μm band depth data to the M3 global ~2.81 μm band depth data varied with temperatures, 2 μm integrated band depths and latitudes (data of shaded areas, which are from Fig. 12b, Fig. 10c, and Fig. 8b of ref. 26). g ARTEMIS P1 ion energy flux spectrogram from 20 November 2020 to 10 December 2020. The area derived from the red dashed lines in the figure indicates the low energy fluxes of the received solar wind particles during LMS in situ observation period (2020.12.01–2021.12.02), when the Moon is under the protection of the Earth’s magnetosphere.
