Magnetic properties experiments and the Surface Stereo Imager calibration target onboard the Mars Phoenix 2007 Lander: Design, calibration, and science goals

[1] The first NASA scout mission to Mars, Phoenix, launched 4 August will land in the northern part of Mars in the locality of 68°N and 233°E on 25 May 2008. Part of the science payload is the Magnetic Properties Experiments (MPE) that consists of two main experiments: the Improved Sweep Magnet Experiment (ISWEEP) and 10 sets of two Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) magnet substrates with embedded permanent magnets of different strength. The ISWEEP experiment is, as the name indicates, an improved version of the Sweep Magnet Experiments flown onboard the two Mars Exploration Rovers (MERs) Spirit and Opportunity. The sweep magnet is ring shaped and is designed to allow only nonmagnetic particles to enter a small circular area at the center of the surface of this structure. Results from this experiment have shown that on the MERs hardly any particles can be detected in the central area of this ring-shaped magnet. From this we have concluded that essentially all particles in the Martian atmosphere are magnetic in the sense that they are attracted to permanent magnets. In order to improve the sensitivity of the Sweep Magnet Experiment for detection of nonmagnetic or very weakly magnetic particles, the ISWEEP holds six ring-shaped magnets, somewhat larger than the sweep magnet of the MERs, and with six different background colors in the central area. The six different colors provide new possibilities for improved contrast between these background colors, i.e., any putative nonmagnetic particles should render these more easily detectable. The Surface Stereo Imager will also take advantage of the small clean areas in the ISWEEPs and use the presumably constant colors for radiometric calibration of images. The MECA magnets work as substrates in the MECA microscopy experiments; they are built to attract and hold magnetic particles from dust samples. The collected dust will then be examined by the optical microscope and the atomic force microscope in the MECA package.

[1]  P. A. J. Englert,et al.  Distribution of Hydrogen in the Near Surface of Mars: Evidence for Subsurface Ice Deposits , 2002, Science.

[2]  U. Bonnes,et al.  Athena MIMOS II Mossbauer spectrometer investigation , 2003 .

[3]  Ricardo Garcia,et al.  Dynamic atomic force microscopy methods , 2002 .

[4]  S. T. Elliot,et al.  Mars Exploration Rover Athena Panoramic Camera (Pancam) investigation , 2003 .

[5]  Klaus Keil,et al.  Geochemical and mineralogical interpretation of the Viking inorganic chemical results , 1977 .

[6]  Robert O. Reynolds,et al.  Microscopy capabilities of the Microscopy, Electrochemistry, and Conductivity Analyzer , 2008 .

[7]  R. Hargraves.  Magnetic anisotropy and remanent magnetism in hemo‐ilmenite from ore deposits at Allard Lake, Quebec , 1959 .

[8]  W. Boynton,et al.  Maps of Subsurface Hydrogen from the High Energy Neutron Detector, Mars Odyssey , 2002, Science.

[9]  Analysis of the magnetic properties experiment data on Mars: results from Mars Pathfinder , 2000 .

[10]  Mark T. Lemmon,et al.  Phoenix Robotic Arm Camera , 2008 .

[11]  Richard V. Morris,et al.  Phyllosilicate-poor palagonitic dust from Mauna Kea Volcano (Hawaii): A mineralogical analogue for magnetic Martian dust? , 2001 .

[12]  D. Ming,et al.  Indication of drier periods on Mars from the chemistry and mineralogy of atmospheric dust , 2005, Nature.

[13]  M B Madsen,et al.  Magnetic properties experiments on the Mars Pathfinder lander: preliminary results. , 1997, Science.

[14]  Peter W. H. Smith,et al.  The Phoenix mission to Mars , 2004, 2004 IEEE Aerospace Conference Proceedings (IEEE Cat. No.04TH8720).

[15]  U. Schwertmann,et al.  Mineralogy of a burned soil compared with four anomalously red Quaternary deposits in Denmark , 2004, Clay Minerals.

[16]  J. M. Knudsen,et al.  The magnetic properties experiments on Mars Pathfinder , 1996 .

[17]  Raul A. Romero,et al.  Athena Mars rover science investigation , 2003 .

[18]  R. Arvidson,et al.  Viking magnetic properties experiment - Extended mission results , 1979 .

[19]  Steven W. Squyres,et al.  The new Athena alpha particle X‐ray spectrometer for the Mars Exploration Rovers , 2003 .

[20]  J F Bell,et al.  Magnetic Properties Experiments on the Mars Exploration Rover Spirit at Gusev Crater , 2004, Science.

[21]  V. Sautter,et al.  Pyrrhotite and the remanent magnetization of SNC meteorites: a changing perspective on Martian magnetism , 2001 .

[22]  Miles J. Johnson,et al.  Athena Microscopic Imager investigation , 2003 .

[23]  Raymond E. Arvidson,et al.  Rock Abrasion Tool: Mars Exploration Rover mission , 2003 .

[24]  Thin film surface treatments for lowering dust adhesion on Mars Rover calibration targets , 2008 .

[25]  Per Nornberg,et al.  Magnetic Properties Experiments on the Mars Exploration Rover mission , 2003 .

[26]  G. Kletetschka,et al.  The role of hematite ilmenite solid solution in the production of magnetic anomalies in ground- and satellite-based data , 2002 .

[27]  H Y McSween,et al.  The chemical composition of Martian soil and rocks returned by the mobile alpha proton X-ray spectrometer: preliminary results from the X-ray mode. , 1997, Science.

[28]  C. Spitzer,et al.  The Viking magnetic properties experiment - Primary mission results. [on Mars landing sites , 1977 .