Insight Into MARSIS Radar Data Analysis
Paris (ESA) Sep 20, 2005 Following completion of its deployment on 17 June, MARSIS, the Mars Advanced Radar for Subsurface and Ionospheric Sounding onboard the ESA Mars Express spacecraft, has started collecting scientific data from the surface, the subsurface and the ionosphere of Mars. The major scientific goals of this ground penetrating radar experiment are to characterise the subsurface layers of sediments and possibly detect and map underground water or ice, to characterise the radar properties of the surface and to provide data on the planet's ionosphere. Part of the primary objective is the search for water and ice reservoirs, aimed at addressing key issues in the hydrological, geological, and climatic evolution of Mars. These include the current and past global inventory of water, mechanisms of transport and storage of water, the role of liquid water and ice in shaping the landscape of Mars, and the stability of liquid water and ice at the surface as an indication of climatic conditions.
The MARSIS Instrument MARSIS is a multi-frequency, coherent pulse, synthetic aperture radar sounder. Frequencies are selectable in order to adapt the experiment to the Mars environment. Lower frequencies are best suited to probe the deep subsurface and the highest frequencies are used to probe shallow subsurface depths, while all four frequency channels (1.8, 3.0, 4.0, and 5.0 MHz) are suited to study the surface and the upper atmospheric layer of Mars. The two 20-metre long antenna booms (dipole) are sending radio signals towards the Martian surface and are receiving echoes back. The secondary, receive-only, 7-metre long monopole antenna is to be used in conjunction with the MARSIS dipole, to correct for off-nadir surface roughness effects. The monopole will, therefore, find its best use during the investigations of areas where the surface roughness is higher, that is where it can minimize the effects of surface "clutter" on subsurface feature detection.
The MARSIS Scientific Data Collection MARSIS has a unique capability of sounding the Martian environment with coherent long-wavelength wide-band pulses that allow the collection of a large amount of significant data about the subsurface, surface and ionosphere. For subsurface probing, MARSIS must operate under 800 kilometres altitude from the Martian surface, while for ionospheric sounding MARSIS provides acceptable results from a distance of up to 2000 kilometres. The radar vertical depth resolution is 150 metres (in the free space), while echo profiles of the subsurface are acquired at a lateral spacing of about 5 to 9 km, depending on the spacecraft altitude. The MARSIS radar is designed to operate around the pericentre of the orbit, when the spacecraft is closer to the planet�s surface. In each orbit available to MARSIS, the radar is switched on for 36 minutes around this pericentre point, dedicating the central 26 minutes to subsurface observations and the first and last five minutes of the slot to active ionosphere sounding. Nighttime is the environmental condition favourable to subsurface sounding, as the ionospheric plasma frequency is lowest. The ionosphere is more energised during the daytime and disturbs the radio signals used for subsurface observations. Although even during the daytime, the MARSIS instrument can detect signals from the surface and subsurface after proper ionospheric corrections are made. The radar is for the first time making measurements of the ionosphere in the sub-solar and night side regions that were not accessible to previous Mars missions. MARSIS will probe the Martian plasma environment for electron densities in the range from 30 to 3.5�106 electrons per cm3, with increased spatial resolution of vertical profiles. The active sounding ionospheric mode consists of transmitting sinusoidal pulses with a nominal duration of 91.4 ms in 160 frequency steps from 0.1 MHz to 5.5 MHz. Such measurements, with the aim of global coverage, will explore the relationships between the neutral atmosphere and ionosphere, and the interactions of the solar wind with the planet.
The MARSIS Data Processing Goals Regarding the ground processing, the main goals of the analysis of the MARSIS scientific data sets include:
The processing scheme of the MARSIS data sets involves the in-depth analysis, at each frequency, of a set of parameters that are consolidated into a database for interpretation of local and regional behaviour and comparison with other data sets and simulations:
The discrimination of ground-ice boundaries should be within reach of the MARSIS detection capabilities. Other stratigraphic and structural boundaries could be identified, providing a view of the vertical dimension of the Martian geology. For a number of regions of interest, modelling of the electrical properties of the layers and interfaces will be performed to estimate the thickness of layers, the depth to interfaces, the composition and dielectric properties of the materials. With respect to instrument performance, one challenge that must be overcome is the presence of radar scattering from the surface of Mars, which will be simultaneously detected with the echoes from subsurface interfaces. To solve this problem, the monopole signal will be used in conjunction with predictions of the scattering behaviour that may be expected from Martian surface topography, through simulations and comparisons with existing theoretical scattering models.
Ionospheric Sounding Data Investigation MARSIS ionospheric measurements are performed in both passive and active mode. In passive mode, the thermal emission line at the local electron plasma frequency is used to measure the local electron density. The active technique uses radar soundings to measure the vertical range to the ionospheric reflection point as a function of frequency. The various parameters and factors to be investigated as part of the ionospheric sounding data processing are:
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