MARSIS Overview J. J. Plaut G. Picardi and the MARSIS Team.

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Presentation transcript:

MARSIS Overview J. J. Plaut G. Picardi and the MARSIS Team

MARSIS Mars Advanced Radar for Subsurface and Ionospheric Sounding Science Objectives Primary “Map the distribution of water, solid and liquid, in the upper portions of the crust of Mars.” How?: Detect, map and characterize subsurface material discontinuities in the upper crust of Mars. These may include boundaries of: Liquid water-bearing zones Icy layers Geologic units Geologic structures Secondary Characterize and map the elevation, roughness and electromagnetic properties of the surface. Probe the ionosphere of Mars to characterize the interaction of the atmosphere and solar wind.

Antenna Sizes Dipole: 40 meters tip-to-tip. Monopole: 7 meters. MARSIS Deployed on Mars Express Radar Channels 1.8, 3.0, 4.0, 5.0 MHz (166, 100, 75, 60 m)

MARSIS Antennas 20 meter dipoles (2) 7 meter monopole

MARSIS Science Themes Global reconnaissance, subsurface sounding Aquifer search Polar region studies Stratigraphy and geologic structure Ionospheric sounding

MARSIS Science Themes Ionospheric sounding Reconnaissance of ionosphere under varying conditions: Solar zenith angle, latitude, season. Solar activity/cycle and distance. Crustal magnetic field. Nightside behavior (“holes”; other variations) Crustal magnetism: Effect on ionosphere. Active ionospheric and subsurface sounding to map crustal fields.

10 km Power Time (Depth) Swath MappingSingle Footprint ~ 500 contiguous footprints per orbitUp to 4 profiles for each footprint MARSIS Data Acquisition Scheme

Detected by monopole and dipole Detected by dipole only Subsurface interface Surface Dipole Monopole Incoming wave MARSIS Clutter Cancellation

MARSIS Summary - As of Spring 2005! MARSIS is an experiment! First objective: Detect something in the subsurface. (Mars must cooperate.) Second objective: Characterize that “something”. Critical phases coming up: deployment, check-out, data(!!!) Unambiguous aquifer detection will be a challenge, but… …models suggest that if aquifers are present within the upper ~3 km, we have a good chance of seeing them.

MARSIS Summary - As of Now

MARSIS Some Recent PR

2682 MARSIS Radargram South Polar Layered Deposits (SPLD) 500 km MARSIS Data MOLA Topo Nadir groundtrack SPLD surface Basal interface 50  s

SPLD Thickness From MARSIS

Morgan et al. JGR. U.Iowa Gurnett Co-I