PDS_VERSION_ID        = PDS3

^PDF_DOCUMENT         = "PFS_ON_MARS_EXPRESS.PDF"
PRODUCT_ID            = PFS_ON_MARS_EXPRESS
RELEASE_ID            = 0001
REVISION_ID           = 0000
RECORD_TYPE           = FIXED_LENGTH
DATA_SET_ID           = "MEX-M-PFS-2-EDR-EXT3-V1.0"
PRODUCT_CREATION_TIME = 2010-12-07T12:01:23.260


OBJECT                = PDF_DOCUMENT
DOCUMENT_NAME         = "THE PLANETARY FOURIER SPECTROMETER (PFS) ONBOARD THE
                      EUROPEAN MARS EXPRESS MISSION"
PUBLICATION_DATE      = 2010-12-07
DOCUMENT_TOPIC_TYPE   = "INSTRUMENT DESCRIPTION"
INTERCHANGE_FORMAT    = BINARY
DOCUMENT_FORMAT       = "ADOBE PDF"
DESCRIPTION           = "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 8200.0 cm-1 (1.2 to 5.5 um) and  a long-wave 
(LW) channel that covers 250 to 1700 cm-1 (5.5 to 45 um). Both channels have 
a uniform spectral resolution of 1.3 cm-1 . The instrument field of view FOV 
is  about 1.6 degrees ( FWHM) for the Short Wavelength channel (SW) and 2.8 
degrees (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 (Li Ta O3) 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 takes 4 seconds , with a repetition time of 
8.5 sec. By working roughly  0.6 hour 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." 
END_OBJECT            = PDF_DOCUMENT
END