Mars: Sources of Data from the Robotic Missions IVMars: Data from Robotic MissionsSlide 3Slide 4Slide 5Slide 6Slide 7Slide 8Slide 9Slide 10Slide 11Slide 12Slide 13Slide 14Slide 15Slide 16Slide 17Slide 18Slide 19Slide 20Slide 21Slide 22Slide 23Slide 24C.M. Rodrigue, 2007Geography, CSULBMars: Sources of Data from the Robotic Missions IVGeography 494-01S/07Dr. Christine M. RodrigueC.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA Mars Express Orbiter (2003-present)Main objective is to search for sub-surface water from orbit and deploy a lander onto the Martian surface Beagle 2 lander crashed in late 2003: It was to look for life signsC.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA Mars Express Orbiter (2003-present)Orbiter instrumentation:Analyser of Space Plasmas and Energetic Atoms (ASPERA-3)High/Super Resolution Stereo Colour Imager (HSRS)Radio Science Experiment (MaRS)Subsurface Sounding Radar/Altimeter (MARSIS)IR Mineralogical Mapping Spectrometer (OMEGA)Planetary Fourier Spectrometer (PFS)UV and IR Atmospheric Spectrometer (SPICAM)C.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA Mars Express Orbiter (2003-present)Orbiter instrumentation:Analyser of Space Plasmas and Energetic Atoms (ASPERA-3)High/Super Resolution Stereo Colour Imager (HSRS)Originally developed for the Mars 96 mission: The duplicate, since upgraded9 CCD line sensors in pushbroom swathsEach of these arrays has 5184 7 micron pixels (10 m on ground)Super Resolution Channel telescope with 1024 x 1032 CCD array that results in 2.3 m pixels on the groundMultispectral visible light to near infrared imaging plus panchromatic imaging by the forward and aft line sensorsRadio Science Experiment (MaRS)Subsurface Sounding Radar/Altimeter (MARSIS)IR Mineralogical Mapping Spectrometer (OMEGA)Planetary Fourier Spectrometer (PFS)UV and IR Atmospheric Spectrometer (SPICAM)C.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA High Resolution Stereo Colour imagerNew topographic mapsContour lines: “first ‘hikers’ maps’ of Mars”! Here’s 1:200,000C.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA High Resolution Stereo Colour imagerNew topographic mapsContour lines: “first ‘hikers’ maps’ of Mars”! Here’s 1:100,000C.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA High Resolution Stereo Colour imagerNew topographic mapsContour lines: “first ‘hikers’ maps’ of Mars”! And 1:50,000C.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA Mars Express Orbiter (2003-present)Orbiter instrumentation:Analyser of Space Plasmas and Energetic Atoms (ASPERA-3)High/Super Resolution Stereo Colour Imager (HSRS)Radio Science Experiment (MaRS)Subsurface Sounding Radar/Altimeter (MARSIS)Ground-penetrating radar (1.3-5.5 MHz) Deployed from end of 40 m antenna to generate long wlRadio waves reflect back upward from any surface discontinuity: surface itself, liquid layers undergroundIR Mineralogical Mapping Spectrometer (OMEGA)Planetary Fourier Spectrometer (PFS)UV and IR Atmospheric Spectrometer (SPICAM)C.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA MARSISThe idea behind ground-penetrating radarC.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA MARSISHas found crater basin structures buried in Chryse PlanitiaC.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA MARSISHas found crater basin structures buried in Chryse – dark ovalsC.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA Mars Express Orbiter (2003-present)Orbiter instrumentation:Analyser of Space Plasmas and Energetic Atoms (ASPERA-3)High/Super Resolution Stereo Colour Imager (HSRS)Radio Science Experiment (MaRS)Subsurface Sounding Radar/Altimeter (MARSIS)IR Mineralogical Mapping Spectrometer (OMEGA)Building map of surface composition in 100 m squaresDetermines mineral composition through reflected VL & IR (0.5-5.2 microns)Because reflected surface light must pass through atmosphere, OMEGA can also infer atmospheric compositionPlanetary Fourier Spectrometer (PFS)UV and IR Atmospheric Spectrometer (SPICAM)C.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA IR Mineralogical Mapping Spectrometer (OMEGA)Building map of surface composition in 100 m squaresOne focus is water-related/water-affected mineralsWater content of the rocks and clay minerals Abundance of non-silicate materials (carbonates, nitrates, hydrated sufates), which imply standing water or water alterationC.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA IR Mineralogical Mapping Spectrometer (OMEGA)Building map of surface composition in 100 m squaresAnother focus is the carbon dioxide/water composition of the capsWater does not absorb ~2 microns, and carbon dioxide doesSouth polar cap shows absorption at 2, implying CO2 (A & B)Spectrum C shows absorption where A & B don’t ~1.5 microns, indicating more water ice in the mix thereC.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA Mars Express Orbiter (2003-present)Orbiter instrumentation:Analyser of Space Plasmas and Energetic Atoms (ASPERA-3)High/Super Resolution Stereo Colour Imager (HSRS)Radio Science Experiment (MaRS)Subsurface Sounding Radar/Altimeter (MARSIS)IR Mineralogical Mapping Spectrometer (OMEGA)Planetary Fourier Spectrometer (PFS)Another spectrometer, overlapping part of OMEGA’s spectrum but also including spectra far deeper into the infrared: 1.2-5 microns and then 5-45 micronsThis spectrometer focusses more on the atmosphere’s temperature and composition, rather than the surfaceUV and IR Atmospheric Spectrometer (SPICAM)C.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA Planetary Fourier Spectrometer (PFS)Vertical temperature structure of Martian atmosphereC.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA Planetary Fourier Spectrometer (PFS)Optical thickness of Martian atmospheric dust (with surface elevation below the reading also shown)C.M. Rodrigue, 2007Geography, CSULBMars: Data from Robotic MissionsESA Planetary Fourier Spectrometer