We assessed the degradation of the radiance lamp in the onboard calibration system of the Spectral Profiler, a hyperspectral sensor onboard the Japanese Selenological and Engineering Explorer (SELENE), which was launched in September 2007 and observed the Moon until June 2009. We found that the output of the radiance lamp soon after launch increased by 3.2%–4.6% as compared with the prelaunch output, after which it decreased over time. The total decrease during the mission lifetime of about 1.5 years after the increase of 3.2%–4.6% was ~1.1%–1.5%, which is slightly larger than the < 1% degradation of the sensitivity of the sensor, as derived from vicarious calibration using the Apollo 16 landing site observations. Thus, we confirmed that the radiance lamp became degraded, but the degree of degradation was within 1% during ~1.5 years. We also found a wavelength dependence in the degradation, in which degradation was larger for shorter wavelengths, especially for wavelengths less than ~

$0.8\,\mu \text{m}$

. The trend of the wavelength dependence was shown to be consistent with a model of blackbody radiance with a decrease in temperature of the lamp of about −5 K, suggesting that the degradation of the lamp was mostly due to temperature decrease of about −3 K/yr. Our results may provide an important constraint on the quantitative assessment of the degradation of the sensitivity of remote-sensing sensors using an onboard calibration system, such as the Advanced Spaceborne Thermal Emission and Reflection Radiometer.

Degradation

Black-body radiation

10.1109/tgrs.2021.3127163

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Pontine haemorrhage causing disturbance of taste

Neuroradiology (1995)

Ichiro Sunada Yoshinori Akano S. Yamamoto Takahiko Tashiro

Medial lemniscus

Neuroradiology

Pons

10.1007/bf00593388

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Citations (18)

Geologic structure generated by large‐impact basin formation observed at the South Pole‐Aitken basin on the Moon

Geophysical Research Letters (2014)

M. Ohtake K. Uemoto Y. Yokota Tomokatsu Morota S. Yamamoto

Abstract The South Pole‐Aitken (SPA) basin is the largest clearly recognized basin on the lunar surface. Determining the composition and structure of the SPA basin interior provides critical constraints on the deep crustal and/or mantle composition of the Moon and improves our understanding of large‐basin‐forming impact processes. Here we present a new mineralogical map of the SPA basin interior, based on high‐spatial‐resolution reflectance spectra using the SELENE (Kaguya) multiband imager, which is combined with topographic data in order to interpret the geologic context. The derived mineralogical map suggests extensive distribution of ejected low‐Ca pyroxene‐dominant mantle material with the presence of purest anorthosite crustal materials surrounding a possible melt pool of 0.26 to 0.33 of the basin diameter near the basin center, which is significantly smaller than that suggested by the crater‐scaling law. The absence of clear evidence of lower crustal material is consistent with recent impact simulation results.

Anorthosite

Impact structure

10.1002/2014gl059478

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Citations (57)

Thermal radiation from dust grains in Edgeworth-Kuiper Belt

Earth Planets and Space (2014)

S. Yamamoto T. Mukai

We calculate the temperature of dust grains produced in Edgeworth-Kuiper Belt (EKB) based on the grain model for water-ice and silicate mixtures. The dust grains with radii ranging from 0.1 μm to 1 mm have low temperatures of about 20 K to 50 K in EKB, depending on their size, solar distance, and a volume mixing ratio of silicate to water-ice. We also estimate the thermal radiation from dust cloud in EKB. The result of thermal emission shows the spectral feature of water-ice at the wavelength of about 60 μm. Although it is difficult to estimate the possibility to detect the thermal emission spectrum of EKB dust cloud, due to large uncertainties in its spatial density, we found that the thermal emission of dust cloud in EKB lies below the IRAS data of foreground zodiacal emission. The maximum value of the thermal emission derived from the acceptable dust cloud model in EKB, however, becomes to be comparable to that of foreground zodiacal emission in far-infrared and submillimeter wavelength domains. Since the EKB dust cloud seems to concentrate near the ecliptic plane, a scanning of infrared observation along a line perpendicular to the ecliptic plane may reveal the presence of such dust cloud in the future.

Zodiacal light

10.1186/bf03352145

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Citations (9)

Estimating Composition of Dark Mantle Deposit in Schrödinger Basin Using SELENE Spectral Data

Lunar and Planetary Science Conference (2010)

Y. Kobayashi M. Ohtake J. Haruyama Tsuneo Matsunaga Takahiro Iwata

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