DOI:
10.1016/S0273-1177(97)00282-2
Authors:
Formisano, V; Moroz, VI; Angrilli, F; Bianchini, G; Bussoletti, E; Cafaro, N; Capaccioni, F; Capria, MT; Cerroni, P; Chionchio, G; Colangeli, L; Coradini, A; DiLellis, A; Fonti, S; Orfei, R; Palomba, E; Piccioni, G; Saggin, B; Ekonomov, A; Grigoriev, A; Gnedykh, V; Khatuntsev, I; Kiselev, A; Matsygorin, I; Moshkin, B; Nechaev, V; Nikolsky, Y; Patsaev, D; Russakov, A; Titov, D; Zasova, L; Blecka, MI; Jurewicz, A; Michalska, M; Novosielski, W; Orleanski, P; Arnold, G; Hirsch, H; Driesher, H; LopezMoreno, J; Rodrigo, R; RodriguezGomez, J; Michel, G
Journal:
PLANETARY ATMOSPHERES AND IONOSPHERES AND REFERENCE ATMOSPHERES
Abstract:
The Planetary Fourier Spectrometer PFS has been designed for the study of the atmosphere and soil of Mars. PFS has two infrared channels: a long wavelength (LW) channel with range 250 - 2000 cm(-1) and a short wavelength (SW) channel with range 2000 - 8333 cm(-1). The spectral resolution is 2 cm(-1). Both channels work simultaneously. The field of view is 2 degrees which covers 10 km on the Martian surface being observed from the pericenter at 300 km. The signal to noise ratio is better than 100 in a range of particular scientific interest (at 650 cm(-1), for example). The built-in pointing device allows to study the atmosphere over extreme regions like Hellas Planitia or Olympus Mons. (C) 1997 COSPAR. Published by Elsevier Science Ltd.