Investigating the UV properties of Martian terrains with the NOMAD/UVIS channel data
Description
The behavior of the Martian surface reflectance factor is poorly constrained between 200 and 350 nm. In this spectral range the albedo is very low with no significant deviations that can be correlated with the different mineralogy observed on Mars. Here we investigate possible variations of the Martian terrains reflectance in the UV by exploiting the data of the NOMAD/UVIS channel. We focus first on a dark region and a bright one, covered by observations collected before the occurrence of the global dust storm that started at the end of May 2018.
Citation
Altieri, F.; Bellucci, G.; Carrozzo, F.G.; Willame, Y.; Depiesse, C.; Mason, J.; Hewson, W.; Oliva, F.; D’Aversa, E.; Thomas, I.R.; Vandaele, A.C.; Patel, M.R.; Wolff, M.J.; Aoki, S.; Amoroso, M.; Piccialli, M.; Daerden, F.; Ristic, B.; Lòpez Puertas, M.; Lòpez-Moreno, J.J.; Da Pieve, F.; the NOMAD Team (2019). Investigating the UV properties of Martian terrains with the NOMAD/UVIS channel data. , EPSC-DPS Joint Meeting 2019, 15-20 September 2019, Geneva, Switzerland, Vol. 13, EPSC-DPS2019-1369-1,Identifiers
Type
Conference
Peer-Review
No
Language
eng