|
|||||
|
|
The Planetary Fourier Spectrometer (PFS) onboard the European Mars Express mission |
|
| Authors: | V. Formisano F. Angrilli S. Atreya D. Biondi M.I. Blecka L. Colangeli F. Esposito M. Giuranna V. Gnedykh G. Hansen I. Khatuntsev N. Ignatiev A. Jurewicz J. Lopez Moreno A. Mattana E. Mencarelli V. Moroz F. Nespoli R. Orfei V. Orofino D. Patsaev M. Rataj J. Rodriguez B. Saggin L. Zasova |
| Affiliation: | a Istituto di Fisica dello Spazio Interplanetario INAF-IFSI, Via del Fosso del Cavaliere 100, 00133 Roma, Italy b Universita’ di Padova, CISAS, Via Venezia 1, 35131 Padova, Italy c Space Research Institute of Russian Academy of Sciences (IKI) Profsojuznaja 84/32, 117997 Moscow, Russia d The University of Michigan, Department of Atmospheric, Oceanic, and Space Sciences, Ann Arbor, MI 48109-2143, USA e Universita’ degli Studi di Lecce, Dipartimento di Fisica Via Arnesano, 73100 Lecce, Italy f Space Research Center of Polish Academy of Sciences (SRC PAS), Bartycka 18A, 00716 Warsaw, Poland g Osservatorio Astronomico di Capodimonte (INAF-OAC) Via Moiariello 16, 80131 Napoli, Italy h Planetary Science Institute, Pacific Northwest Division, Department of Earth and Space Science, seattle, WA, USA i Instituto de Astrofisica de Andalusia CSIC, p.o.b. 3004,18080 Granada, Spain j Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique (LESIA), Observatoire de Paris 5 Place Janssen, 92195 Meudon, France k Istituto Astrofisica Spaziale INAF-IASF, Via Fosso del Cavaliere 100, 00133 Roma, Italy l Politecnico di Milano, Dipartimento di Meccanica, sede di Lecco, Italy m German Aerospace Center (DLR), Optical Information System, Rutherfordstr.2, D-12489, Berlin, Germany |
| Abstract: | The Planetary Fourier Spectrometer (PFS) for the Mars Express mission is an infrared spectrometer optimised for atmospheric studies. This instrument has a short wave (SW) channel that covers the spectral range from 1700 to  (1.2- ) and a long-wave (LW) channel that covers 250- (5.5- ). Both channels have a uniform spectral resolution of  . The instrument field of view FOV is about 1.6° (FWHM) for the Short Wavelength channel (SW) and 2.8° (FWHM) for the Long Wavelength channel (LW) which corresponds to a spatial resolution of 7 and 12 km when Mars is observed from an height of 250 km. PFS can provide unique data necessary to improve our knowledge not only of the atmosphere properties but also about mineralogical composition of the surface and the surface-atmosphere interaction.The SW channel uses a PbSe detector cooled to 200-220 K while the LW channel is based on a pyroelectric (LiTaO3) detector working at room temperature. The intensity of the interferogram is measured every 150 nm of physical mirrors displacement, corresponding to 600 nm optical path difference, by using a laser diode monochromatic light interferogram (a sine wave), whose zero crossings control the double pendulum motion. PFS works primarily around the pericentre of the orbit, only occasionally observing Mars from large distances. Each measurements take 4 s, with a repetition time of 8.5 s. By working roughly 0.6 h around pericentre, a total of 330 measurements per orbit will be acquired 270 looking at Mars and 60 for calibrations. PFS is able to take measurements at all local times, facilitating the retrieval of surface temperatures and atmospheric vertical temperature profiles on both the day and the night side. |
| Keywords: | Instrumentation Atmosphere Mars Mars Express |
| 本文献已被 ScienceDirect 等数据库收录！ | |