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° 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. © 1997 COSPAR. Published by Elsevier Science Ltd.
PFS:A fourier spectrometer for the study of Martian atmosphere
Saggin B.;
1997
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° 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. © 1997 COSPAR. Published by Elsevier Science Ltd.
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