Modelling the Beagle 2 landing site in Isidis Planitia and comparison with results from the planetary fourier spectrometer

Within its first orbits Mars Express has passed over Isidis Planitia and the Beagle 2 landing site. From these passes we have derived first estimates on the surface temperature for the likely landing site of Beagle 2 using in the Long Wavelength Channel (5 to 45 µm) of the Planetary Fourier Spectrometer (PFS) on Mars Express. In our group the Berlin Mars near Surface Thermal model (BMST) has been developed of the last years, to study the thermal behaviour of the near surface layer on Mars (Helbert and Benkhoff 2003). Using this model various locations on Mars have been studied, including the Beagle 2 landing site in Isidis Planitia. For this location temperature gradients within the top 100m below the surface have been calculated. Based on the modelling it was possible to derive estimates on the minimal burial depth of possible ground ice deposits (Helbert and Benkhoff 2003, 2004). The model yields also maps of the surface temperatures for LS 340-70, which can now be compared to first estimates on the surface temperature derived from PFS data. This comparison can be used to further refine the modelling and derive constraints on the thermo-physical properties of the surface material in Isidis Planitia.