Lunar has stable spectral properties with a varying tendency of 10-8 per year. Due to the independent on the scattering and absorbing effects of atmosphere, lunar is a perfect radiometric reference for earth-observing satellite. Researching on the radiometric model of lunar gives a new path to on-orbit radiometric calibration for remote sensing satellite to get rid of the uncertainties of atmosphere on calibration accuracy. GF-4 of China was a geostationary remote sensing satellite with a big array CMOS detector, it can acquire the whole lunar disk image without earth-atmosphere stray light by rolling the satellite, and the instantaneous field of view (IFOV) of VNIR sensor to lunar is about 500m. Firstly, recalibration is implemented before further processing. Secondly, the radiometric properties of lunar are retrieved by the recalibration results. A common used method in researching the radiometry of lunar was adopted in this work: deriving the bidirectional reflectance factor (BRF) on three typical lunar calibration sites of Apollo-16, MS-2 and CE-3 with t GF-4 lunar image, and comparing the BRFs with SP on SELENE, M3 on Chandrayaan-1 and IIM on CE-1. The model of GF-4 VNIR sensor showed a relatively high consistency with other existed models as wavelength increasing. The results indicated that the radiometric model of lunar in this work had the potentiality to join the group of lunar models.
Remote spectroscopic observations of the lunar surface is now complemented by in situ reflectance spectra obtained by the Chang’E 3 and Chang’E 4 missions. The material at landing site includes also a fragment of rock with a small- to medium grained plutonic texture. Current spectral databases primarily contain spectra measured on powder samples, while spectra of coarse-grained rock samples are rare. Rock samples returned from the Apollo missions indicate that lunar anorthosites are typically coarse grained and reach grain sizes larger than 1 cm. We present the extension of the current spectral databases by new spectral data of whole rock samples, crucial for the interpretation of current in situ/remote analyses for lunar and other planetary missions, as Hayabusa2 and OSIRIS-REx. Spectral data is recorded at the Planetary Spectroscopy Laboratory (PSL) of DLR in Berlin. The suite of samples selected for this work includes: - slabs and stone chunks of plagioclases such as anorthosite, diorite, monzodiorite, gabbro and diabas; - salts such as hexahydride; - iron meteorite samples, among them ataxites and octahedrites. Emissivity is measured in vacuum at 100° C, 200° C, 300° C and 400° C in the MIR and FIR spectral ranges. Thermally processed samples are measured in hemispherical and bi-directional reflectance in the full spectral range from UV to FIR. A sample of graphite (measured in emissivity under the same configuration and procedure as for the samples) is used to calibrate the sample emissivity.
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