Exploring Mars: A Comprehensive Overview of Missions & Scientific Breakthroughs

1. The Australian Centre for Space Photonics Andrew McGrath, Joss Hawthorn,Jeremy Bailey Presentation to the NSSA, October 2003

2. Mars and the Anglo-Australian Observatory Andrew McGrath, Joss Hawthorn,Jeremy Bailey Presentation to the NSSA, October 2003

3. The Australian Centre for Space Photonics • 2002 Proposal to the ARC for a Centre of Excellence • Strong technical basis • Strong reasons for an Australian involvement • Withdrew from ARC proposal on applicability issues • Continuing work – maintaining vision – following different route to involvement

4. Mars • Diameter: 6790 km • Rotation period: 24.6229 hours • Polar inclination: 23.98° • Mass: 0.1074 Earth masses • Escape velocity: 5030 ms-1 • Surface gravity: 3.73 ms-2 • Albedo: 0.16 • Atmosphere: 95% CO2, 3% N2 • Surface pressure: ~10 hPa • Surface temperature: 130K – 300K • Solar orbit diameter: 1.4 AU • Distance from Earth: ~50Mkm to ~400Mkm

5. History • Long term interest • Mythological • Scientific • Similarity to Earth

6. History Percival Lowell, 1906

7. History

8. History

9. Mars • Recent opposition: only ~55 million km Earth to Mars • AAO observations using UKIRT in Hawaii, August 2003 obtained spectral ‘images’ in the NIR

10. Long slit spectroscopy

11. Long slit spectroscopy

12. Long slit spectroscopy

13. Long slit spectroscopy

14. Spectrographic analysis Spectrographic slit ensemble Viking imagery 2.2 to 2.3μm

15. Spectrographic analysis ‘Raw’ spectrum of part of the Martian disk

16. Spectrographic analysis Hellas spectral data – relative to dataset ‘centre’ - spectral features highlighted

17. Spectrographic analysis CO2 absorption retrieved MOLA topography from AAO/UKIRT data

18. Spectrographic analysis • Atmosphere • Geology • Astrobiology But there’s a pretty hard limit to what can be done from Earth. We need to go there.

19. Exploration of Mars • • 1962 Two more Soviet flyby attempts,Mars 1 within 190,000 km • 1964 Mariner 3, Zond 2 • 1965 Mariner 4 (first flyby images), Zond 3 • 1969 Mariners 6 and 7 • 1971 Mariners 8 and 9 • 1971 Kosmos 419, Mars 2 & 3 (first landers) • 1973 Mars 4, 5, 6 & 7 • 1975 Viking 1, 1976 Viking 2 1960 Two Soviet flyby attempts

20. Exploration of Mars • 1992 Mars Observer • 1996 Mars 96 • 1997 Mars Pathfinder, Mars Global Surveyor • 1998 Nozomi launch • 1999 Climate Orbiter, Polar Lander and Deep Space 2 • 2001 Mars Odyssey • 1988 Phobos 1 and 2

21. Exploration of Mars • 2003 Nozomi arrival • 2004 Mars Exploration Rovers 1 & 2 • 2005 Mars Reconnaissance Orbiter • 2005 Rosetta flyby • 2007 Mobile Scientific Laboratory • 2007 Netlanders-07 • 2007 Remote Sensing Orbiter • 2003 Mars Express (Beagle 2)

22. Exploration of Mars • 2009 Smart Lander, Long Range Rover • 2009 Mars 2009 Communications Satellite • 2009 Netlanders-09 • 2009 ExoMars-09 • 2014 Mars 2014 (possible sample return) • 2015 Possible ESA manned mission • 2016 Mars 2016 (possible sample return) • 2019 Possible NASA manned mission • 2007 Small Scout Missions (Phoenix)

23. ExoMars-09 • ESA exobiology mission scheduled to land a 220kg rover in 2009 • ‘Pasteur’ instrument package • Panoramic camera • Drill for sample acquistion (depth 1.5m) • Optical colour microscope • Subsurface electromagnetic sounder • Laser plasma spectrometer • Gas chromatograph • Mass spectrometer

24. ExoMars-09 • 180-day lifetime on surface • Search/sample/process cycle ~6 days

25. ExoMars-09 • Opportunity for Australian involvement • ESA call to international community for interested parties to suggest instrumentation or other project support (due 14-May-03) • Large consortium with ACA and AAO as major partners submitted a proposal

26. ExoMars-09 • “Prospector” proposal • Based on ACA expertise in most closely related search fields – detection of evidence of 3-4 Gyr old microbial life (Western Australia) • Two-fold involvement • Search strategy • Instrument proposal

27. ExoMars-09 Prospector instrument: • A NIR spectrometer boresighted to the stereo PanCam • Allows mineralogical assessment of potential drill/sample targets before the full investment of the expensive sample cycle

28. ExoMars-09

29. ExoMars-09

30. Communications -the bottleneck • Increasing number of missions • Evolution towards more data-intensive instrumentation • Increasing spacecraft data storage capacity • Greater reliance on public support for funding – greater sense of ‘presence’ requires greater data rates

31. Communications -the bottleneck • Radio (microwave) links, spacecraft to Earth • Newer philosophy - communications relay (Mars Odyssey, MGS) • Sensible network topology • 25-W X-band (Ka-band experimental)<100 kbps downlink

33. Communications Bottleneck • Current missions capable of collecting much more data than downlink capabilities (2000%!) • Currently planned missions make the problem 10x worse • Future missions likely to collect ever-greater volumes of data

35. Communications Bottleneck • Increasing downlink rates critical to continued investment in planetary exploration

36. Communications Energy Budget • Theoretical ‘cost’ proportional to transmitting wavelength • X-band transmitter  ~ 40 mm • Laser transmitter  ~ 0.5-1.5 m • Assuming similar aperture sizes and efficiencies, optical wins over microwave by > 3 orders of magnitude

37. Long-term Solution • Optical communications networks

38. Long-term Solution • Optical communications networks • Advantages over radio • Higher modulation rates • More directed energy • Analagous to fibre optics vs. copper cables

39. Lasers in Space • Laser transmitter in Martian orbit with large aperture telescope

40. Lasers in Space • Laser transmitter in Martian orbit with large aperture telescope • Receiving telescope on or near Earth • Preliminary investigations suggest ~100Mbps achievable on 10 to 20 year timescale • Enabling technologies require accelerated development

42. Lasers in Space - challenges • Immature technology cf. radio • Cloud and other weather • Pointing and tracking • Signal acquisition • Reliability

43. Lasers in Space - challenges • Will not replace radio for all applications • Fast-manoeuvring spacecraft • Cheap, highly independent spacecraft • Emergency operations • Entry/descent/landing comms • Dusty/thick atmosphere environments

44. Key Technologies • Suitable lasers • Telescope tracking and guiding • Optical detectors • Cost-effective large-aperture telescopes • Atmospheric properties • Space-borne telescopes

45. NASA approach today • Pursuing two approaches • Enhanced RF communications • Optical communications

46. Optical spacecraft comms • ESA have already run intersatellite test • NASA/JPL and Japan presently researching the concept and expect space-ground communications tests in the near future

47. NASA optical comms plans • Operational demonstration on Mars Telecom Orbiter (2009) • 5W average power (300W peak) • 1064μm wavelength (NIR) • 300mm aperture transmitter • 3 – 10 Mbps • 3-9 х 8-10m receiving telescopes

48. AAO input • Proposed NASA parameters near-identical to AAO suggestions • AAO discussions with NASA to encourage change in wavelength (to 532nm) • Go for Green!

49. AAO input – 532 vs. 1064nm • Achieve change with frequency doubler cell (can conceivably switch in & out) • Better pointing (so higher power density, less spill)  • Worse detector efficiency  • Visible (marginally by eye, certainly by amateur astronomers) – public relations coup comparable to USSR Sputnik • Suggestion favourably received by NASA and under serious consideration

50. An Australian Role • Australian organisations have unique capabilities in the key technologies required for deep space optical communications links • Existing DSN involvement • High-power, high beam quality lasers • Holographic correction of large telescopes • Telescope-based instrumentation • Telescope tracking and guiding