The analysis of affections to the cold space calibration source of ChangE-1 payload Microwave Detector

Zhang, Huiya; Zhang, Xiao-Hui; Yang, Jun‐Li

doi:10.1016/j.asr.2007.04.010

Cited by 7 publications

(4 citation statements)

References 10 publications

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“…The CE-1 MWR was calibrated onboard periodically (the calibration performs every 11.6 s, i.e., once every MWR measurement cycle) to assure its reliability and accuracy, using a two-point calibration method [22], [23]. The calibration and accuracy of CE-2 MWR, which is the same payload as CE-1 MWR, is similar to that of CE-1 MWR.…”

Section: A Data Set From Cementioning

confidence: 99%

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Brightness Temperature Calculation of Lunar Crater: Interpretation of Topographic Effect on Microwave Data From Chang'E

Chen

Huang

et al. 2014

IEEE Trans. Geosci. Remote Sensing

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In order to quantitatively interpret topographic effect on Chang'E (CE) microwave data, a detailed method to compute brightness temperature (TB) over a lunar crater is proposed, which incorporated the effect of surface tilts. The method improves the effective solar irradiance model of the lunar surface to obtain the temperature profile of the lunar crater. The calculated TB at 37 GHz with the proposed computation method, which is based on three digital elevation models (DEMs) from different sources, are consistent with the observed TB from the CE-2 microwave radiometer. The simulated behavior of TB across crater Hercules reproduces the TB undulation observed by CE in a single swath. TB is significantly affected by the lunar dust of a lunar crater and affected by albedo and emissivity in a lesser degree. Based on the explanation with simplified models, the TB variation over a crater is proved to be significantly affected, through physical temperature, by the crater shape described by DEMs. With the simplified crater model, the amplitude of the TB oscillatory curves is proved to depend on the crater shape.Index Terms-Brightness temperature (TB), Chang'E (CE), digital elevation model (DEM), lunar crater.

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Section: A Data Set From Cementioning

confidence: 99%

“…The calibration and accuracy of CE-2 MWR, which is the same payload as CE-1 MWR, is similar to that of CE-1 MWR. Detail description about data calibration and data quality can be found in the relevant literatures [16]- [18], [22], [23].…”

Section: A Data Set From Cementioning

confidence: 99%

Brightness Temperature Calculation of Lunar Crater: Interpretation of Topographic Effect on Microwave Data From Chang'E

Chen

Huang

et al. 2014

IEEE Trans. Geosci. Remote Sensing

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“…The calibration of CE-1 microwave radiometer is a real-time and periodical on-orbit calibration system that uses a calibration antenna pointing towards the cold space (2.73 K) and a match-loaded hot reference [13]. During observation, as the satellite flies at different attitudes (e.g.…”

Section: Validation and Calibration Of Brightness Temperaturementioning

confidence: 99%

Analysis of microwave brightness temperature of lunar surface and inversion of regolith layer thickness: Primary results of Chang-E 1 multi-channel radiometer observation

Jin

2010

Sci. China Inf. Sci.

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In China's first lunar exploration project, Chang-E 1 (CE-1), a multi-channel microwave radiometer was aboard the satellite, with the purpose of measuring microwave brightness temperature from lunar surface and surveying the global distribution of lunar regolith layer thickness. In this paper, the primary 621 tracks of swath data measured by Chang-E 1 microwave radiometer from November 2007 to February 2008 are collected and analyzed. Using nearest neighbor interpolation based on the sun incidence angle in observations, global distributions of microwave brightness temperature from lunar surface at lunar daytime and nighttime are constructed. Using the three-layer model (the top dust-soil, regolith and underlying rock media) for microwave thermal emission of lunar surface, the measurements of brightness temperature and dependence upon latitude, frequency and FeO+TiO 2 content, etc. are discussed. On the basis of the ground measurements at Apollo landing sites, the observed brightness temperature at these locations are validated and calibrated by numerical three-layer modeling. Using the empirical dependence of physical temperature upon the latitude verified by the measurements at Apollo landing sites, the global distribution of regolith layer thickness is then inverted from the brightness temperature data of CE-1 at 3 GHz channel. Those inversions at Apollo landing sites are compared with the Apollo in situ measurements. Finally, the statistical property of regolith thickness distribution is analyzed and discussed. KeywordsChang-E 1, multi-channel brightness temperature, Apollo landing site, physical temperature, inversion of regolith layer thickness CitationFa W Z, Jin Y Q. Analysis of microwave brightness temperature of lunar surface and inversion of regolith layer thickness: Primary results of Chang-E 1 multi-channel radiometer observation.

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“…The data applied in this paper are the level 2C TB data after pre-calibrations collected from CE-2. Their calibration and a discussion of their accuracy can be found in [22][23][24][25][26][27][28]. Recent recalibration works [26,27] suggest that the pre-calibrated TB data at 37 GHz can well fit both the infrared and TB models and the correction is smaller than other channels.…”

Section: Introductionmentioning

confidence: 99%

Inversion of the Lunar Subsurface Rock Abundance Using CE-2 Microwave Brightness Temperature Data

Yang,

Hu,

Yang

et al. 2023

Remote Sensing

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The rock strongly affects the surface and subsurface temperature due to its different thermophysical properties compared to the lunar regolith. The brightness temperature (TB) data observed by Chang’E-1 (CE-1) and Chang’E-2 (CE-2) microwave radiometers (MRM) give us a chance to retrieve the lunar subsurface rock abundance (RA). In this paper, a thermal conductivity model with an undetermined parameter β of the mixture has been employed to estimate the physical temperature profile of the mixed layer (rock and regolith). Parameter β and the physical temperature profile of the mixed layer are constrained by the Diviner Channel 7 observations. Then, the subsurface RA on the 16 large (Diameter > 20 km) Copernican-age craters of the Moon is extracted from the average nighttime TB of the CE-2 37 GHz channel based on our previous rocky TB model. Two conclusions can be derived from the results: (1) the subsurface RA values are usually greater than the surface RA values retrieved from Diviner observations of the studied craters; (2) the spatial distribution of subsurface RA extracted from CE-2 MRM data is not necessarily consistent with the surface RA detected by Diviner data. For example, there are similar RA spatial distributions on both the surface and subsurface in Giordano Bruno, Necho, and Aristarchus craters. However, the distribution of subsurface RA is obviously different from that of surface RA for Copernicus, Ohm, Sharonov, and Tycho craters.

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The analysis of affections to the cold space calibration source of ChangE-1 payload Microwave Detector

Cited by 7 publications

References 10 publications

Brightness Temperature Calculation of Lunar Crater: Interpretation of Topographic Effect on Microwave Data From Chang'E

Brightness Temperature Calculation of Lunar Crater: Interpretation of Topographic Effect on Microwave Data From Chang'E

Analysis of microwave brightness temperature of lunar surface and inversion of regolith layer thickness: Primary results of Chang-E 1 multi-channel radiometer observation

Inversion of the Lunar Subsurface Rock Abundance Using CE-2 Microwave Brightness Temperature Data

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