Why do we care about Mars? To understand the distribution of life in the solar system, we have to look for clues in environments that are presently different.

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Presentation transcript:

Why do we care about Mars? To understand the distribution of life in the solar system, we have to look for clues in environments that are presently different from Earth. Earth’s past is gone– that period of time is still present on Mars. Could life have formed at the same time on Earth and on Mars? What ate the planetary requirements for habitability? Does Mars meet these requirements or has it ever?

Explore and quantitatively assess a local region on Mars’ surface as a potential habitat for life, past or present. A.Assess the biological potential of at least one target environment. B.Characterize the geology and geochemistry of the landing region at all appropriate spatial scales (i.e., ranging from micrometers to meters). C.Investigate planetary processes of relevance to past habitability, including the role of water. D.Characterize the broad spectrum of surface radiation, including galactic cosmic radiation, solar proton events, and secondary neutrons. MSL Science Goals & Objectives

Mission Overview SURFACE MISSION Prime mission is one Mars year (687 days) Latitude-independent and long-lived power source Ability to drive out of landing ellipse 84 kg of science payload Direct (uplink) and relayed (downlink) communication Fast CPU and large data storage ENTRY, DESCENT, LANDING Guided entry and powered “sky crane” descent 20×25-km landing ellipse Access to landing sites ±30° latitude, <0 km elevation 900-kg rover CRUISE/APPROACH 8 to 9-month cruise Arrive August 6-20, 2012 LAUNCH Window is Nov. 25 to Dec. 18, 2011 Atlas V (541)

Rover Family Portrait Spirit and Opportunity 2003 Sojourner 1996 Curiosity 2011

Curiosity

Curiosity’s Driving Test

MSL Science Payload REMOTE SENSING Mastcam (M. Malin, MSSS) - Color and telephoto imaging, video, atmospheric opacity ChemCam (R. Wiens, LANL/CNES) – Chemical composition; remote micro-imaging CONTACT INSTRUMENTS (ARM) MAHLI (K. Edgett, MSSS) – Hand-lens color imaging APXS (R. Gellert, U. Guelph, Canada) - Chemical composition ANALYTICAL LABORATORY (ROVER BODY) SAM (P. Mahaffy, GSFC/CNES) - Chemical and isotopic composition, including organics CheMin (D. Blake, ARC) - Mineralogy ENVIRONMENTAL CHARACTERIZATION MARDI (M. Malin, MSSS) - Descent imaging REMS (J. Gómez-Elvira, CAB, Spain) - Meteorology / UV RAD (D. Hassler, SwRI) - High-energy radiation DAN (I. Mitrofanov, IKI, Russia) - Subsurface hydrogen Rover Width:2.8 m Height of Deck:1.1 m Ground Clearance:0.66 m Height of Mast:2.2 m DAN REMS ChemCam Mastcam RAD MAHLI APXS Brush Drill / Sieves Scoop MARDI

Sampling System Cleans rock surfaces with a brush Places and holds the APXS and MAHLI instruments Acquires samples of rock or soil with a powdering drill or scoop Sieves the samples (to 150 μm or 1 mm) and delivers them to instruments or an observation tray Exchanges spare drill bits 2.25-m Robot Arm Extra Drill Bits Sample Observation Tray Turret Organic Check Material Drill CHIMRA APXS MAHLI Brush

The Sample Analysis at Mars Suite SAM

SAM Core Science Goals GOAL #1: Explore sources and destruction paths for carbon compounds GOAL #2: Search for organic compounds of biotic and prebiotic relevance including methane GOAL #3: Reveal chemical and isotopic state of other light elements that are important for life as we know it on Earth GOAL #4: Study habitability of Mars by atmospheric/surface interactions expressed in trace species compositions GOAL #5: Understand atmosphere & climate evolution through isotope measurements of noble gases & light elements Met by measurements of the identity and abundance of organic molecules and their distribution of oxidation states, molecular weights, and chemical structures Met by measurements of: amino acids, nucleobases, carboxylic acids by solvent extraction and chemical derivatization methane abundance in the atmosphere & its 13 C/ 12 C ratio with TLS. Met by measurement of inorganic gases such as SO 2, H 2 O, and CO 2 evolved from solid samples Met by measurement of abundance of multiple minor and trace atmospheric species including those with short photochemical atmospheric lifetimes diurnal and seasonal variation of atmospheric species such as H 2 O, O 2, N 2, Ar, O 3, H 2, and CH 4 Met by measurement in the atmosphere and in gas evolved from fines and powdered rocks isotope ratios for noble gases 13 C/ 12 C, 15 N/ 14 N, 18 O/ 16 O, 17 O/ 16 O, and D/H in simple compounds provides a database that constrains models of atmospheric evolution and identifies reservoirs of the light elements that contribute to the present atmosphere.

SAM Overview Quadrupole Mass Spectrometer (QMS) – Goddard Space Flight Center – Molecular and isotopic composition in the Dalton mass range for atmospheric and evolved gas samples Gas Chromatograph (GC) – University of Paris, CNES – Resolves complex mixtures of organics into separate components Tunable Laser Spectrometer (TLS) – Jet Propulsion Laboratory – Abundance and precision isotopic composition of CH 4, H 2 O and CO 2 SAM is a Suite of 3 Instruments SAM supporting subsystems Gas Processing System (GPS) – Goddard Space Flight Center – Includes valves, manifolds, carrier gas, enrichment cells, Wide Range Pump (WRP), and Pyrolysis Ovens Sample Manipulation System (SMS) – Honeybee Robotics – Positions 74 sample cups to below a sample inlet tube or into SAM pyrolysis ovens Common Infrastructure Systems – Goddard Space Flight Center – Electrical, Mechanical, Thermal, Flight Software QMS TLS GC

Candidate Landing Sites Eberswalde Crater (24°S, 327°E, -1.5 km) contains a clay-bearing delta formed when an ancient river deposited sediment, possibly into a lake. Gale Crater (4.5°S, 137°E, -4.5 km) contains a 5-km sequence of layers that vary from clay-rich materials near the bottom to sulfates at higher elevation. Mawrth Vallis (24°N, 341°E, -2.2 km) exposes layers within Mars’ surface with differing mineralogy, including at least two kinds of clays. Holden Crater (26°S, 325°E, -1.9 km) has alluvial fans, flood deposits, possible lake beds, and clay- rich sediment.