An improvement to the volcano-scan algorithm for atmospheric correction of CRISM and OMEGA spectral data

• Published in: Planetary and space science Vol. 57; no. 7; pp. 809 - 815
• Main Authors: McGuire, Patrick C., Bishop, Janice L., Brown, Adrian J., Fraeman, Abigail A., Marzo, Giuseppe A., Frank Morgan, M., Murchie, Scott L., Mustard, John F., Parente, Mario, Pelkey, Shannon M., Roush, Ted L., Seelos, Frank P., Smith, Michael D., Wendt, Lorenz, Wolff, Michael J.
• Format: Journal Article
• Language: English
• Published: Elsevier Ltd 01.06.2009
• Subjects: Correction for atmospheric CO 2; Hyperspectral imaging; Mars; Surface Hydration; Mars; Correction for atmospheric CO 2; Surface Hydration; Hyperspectral imaging
• ISSN: 0032-0633; 1873-5088
• DOI: 10.1016/j.pss.2009.03.007

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 and 2.1 μm. 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 and 2.011 μm, 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 μm to be instead within the gas bands at 1.980 μm, and for CRISM data, our adaptation shifts the second wavelength slightly, to 2.007 μm. We also report on our efforts to account for a slight ∼0.001 μm shift in wavelengths due to thermal effects in the CRISM instrument.