The radiometric performances of the Planetary Fourier Spectrometer for Mars exploration |
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| Institution: | 1. Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy;2. Istituto di Fisica dello Spazio Interplanetario, CNR, Via Fosso del Cavaliere, 00133 Roma, Italy;3. Istituto di Astrofisica Spaziale-Reparto di Planetologia, CNR, Via Fosso del Cavaliere, 00133 Roma, Italy;4. IKI-Space Research Institute of the Russian Academy of Science, Profsojuznaja 84/32, 117810 Moscow, Russia;1. U.S. Geological Survey, 2255 North Gemini Drive, Flagstaff, Arizona, 86001, USA;1. Centro de Estudios Geof??sicos de Viña del Mar, Callao 231, CerroCastillo, Viña del Mar, Chile;1. DLR Institute of Planetary Exploration, Rudower Chaussee 5, 12484 Berlin, F.R.G.;2. Space Research Institute, Russian Academy of Science, Profsoyuznaya 84/32, Moscow 117810, Russia;1. Département de Recherche Spatiale (CNRS-URA 264), Observatoire de Paris-Meudon, 92195 Meudon Cedex, France;1. Aerospatiale, Cannes and University of Nice, Sophia Antipolis, Nice, France;2. Cornell University, Ithaca, USA;3. MIT, Cambridge, USA;4. Harvard–Smithsonian Center for Astrophysics, Cambridge, USA |
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| Abstract: | The Planetary Fourier Spectrometer (PFS) is a Fourier transform interferometer, operating in the range 1.2–45 μm. The instrument, previously included in the payload of the failed mission Mars ′96, is proposed for the future space mission Mars Express, under study by ESA. The present paper is aimed at presenting the radiometric performances of PFS. The two channels (LW and SW) forming PFS were analysed and characterised in terms of sensitivity and noise equivalent brightness. To cover the wide spectral range of PFS, different blackbodies were used for calibration. The built-in blackbodies, needed for the in-flight calibrations, were also characterised. The results show that the LW channel is comparable with IRIS Mariner 9 in terms of noise equivalent brightness. The SW channel performances, while satisfactorily, could be improved by lowering the sensor operative temperature. A simple model of the Mars radiance is used in order to calculate the signal-to-noise ratio on the spectra in typical observation conditions. The computed signal-to-noise ratio for the LW channel varies between 430 and 40, while for the SW channel it ranges from 150 to 30. The radiometric analyses confirm that PFS performances are compliant with the design requirements of the instrument. PFS is fully validated for future remote exploration of the atmosphere and the surface of Mars. |
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