CRISM和OMEGA光谱数据大气校正火山扫描算法的改进
An improvement to the volcano-scan algorithm for atmospheric correction of CRISM and OMEGA spectral data
摘要：
CRISM和OMEGA高光谱成像光谱仪对火星的观测需要在解释光谱中可能的矿物学特征之前对光度、大气和热效应进行校正。在这里，我们报告了一个简单的，但不平凡的，适应常用的火山扫描校正技术的大气CO_2，它允许改进的矿物检测与内在的吸收带在1.9-2.1 $μ$ m之间的波长。这种火山扫描技术通过确保朗伯吸收度在两个波长（1.890 $μ$ m和2.011 $μ$ m）处相同来消除CO_2的吸收带，其中第一波长在CO_2气体带之外，第二波长在CO_2气体带之内深处。我们对火山扫描技术的调整将第一个波长从1.890 $μ$ m移动到1.980 $μ$ m的气体带内，对于CRISM数据，我们的调整将第二个波长略微移动到2.007 $μ$ m。我们还报告了我们的努力，占轻微的~0.001 $μ$ m的波长偏移，由于在CRISM仪器的热效应。
英文摘要：
The observations of Mars by the CRISM and OMEGA hyperspectral imaging spectrometers require correction for photometric, atmospheric and thermal effects prior to the interpretation of possible mineralogical features in the spectra. Here, we report on a simple, yet non-trivial, adaptation to the commonly-used volcano-scan correction technique for atmospheric CO_2, which allows for the improved detection of minerals with intrinsic absorption bands at wavelengths between 1.9-2.1 $μ$m. This volcano-scan technique removes the absorption bands of CO_2 by ensuring that the Lambert albedo is the same at two wavelengths: 1.890 $μ$m and 2.011 $μ$m, with the first wavelength outside the CO_2 gas bands and the second wavelength deep inside the CO_2 gas bands. Our adaptation to the volcano-scan technique moves the first wavelength from 1.890 $μ$m to be instead within the gas bands at 1.980 $μ$m, and for CRISM data, our adaptation shifts the second wavelength slightly, to 2.007 $μ$m. We also report on our efforts to account for a slight ~0.001 $μ$m shift in wavelengths due to thermal effects in the CRISM instrument.
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