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MOLA Radiometry in Syrtis Major

Below are some examples of MOLA radiometry observations in Syrtis Major, the darkest area of Mars. The charts below show temporal changes, and a comparison to TES Lambert albedo results for the same area.

Location Map of Syrtis major that shows the study area. (Credit: MOLA Science Team)

MOLA radiometry along a profile over polar layered terrain sampled at 8-Hz showing decreased reflectivity in a chasm. A MOLA topographic profile is shown for comparison.

MOLA reflectivity and radiometry data vs L_s for Syrtis Major. Error bar values are standard deviation over 1 day, when measurements were taken. Note that the time series are clearly anti-correlated, especially during the dust storm season (L_s=210-270.). (Credit: MOLA Science Team)

MOLA radiometry and TES Lambert Albedo for relatively dust free period (L<sub>s</sub>=165-190). Overall, TES Lambert albedo is 10% brighter than MOLA radiometry. Missing data in the TES image is due to numerous limb observations by that instrument in order to study the Martian atmosphere. (Credit: MOLA Science Team)

MOLA radiometry and TES Lambert Albedo for relatively dust free period (L_s=165-190). Overall, TES Lambert albedo is 10% brighter than MOLA radiometry. Missing data in the TES image is due to numerous limb observations by that instrument in order to study the Martian atmosphere. (Credit: MOLA Science Team)

MOLA radiometry and TES Lambert albedo vs L<sub>s</sub> for Syrtis Major. Error bar values are standard deviation over 1 day, when measurements were taken. Note that the time series are clearly correlated. TES albedo values are slightly (about 10%) higher than MOLA's I/F values, but further calibration must be done for the MOLA data. (Credit: MOLA Science Team)

MOLA radiometry and TES Lambert albedo vs L_s for Syrtis Major. Error bar values are standard deviation over 1 day, when measurements were taken. Note that the time series are clearly correlated. TES albedo values are slightly (about 10%) higher than MOLA's I/F values, but further calibration must be done for the MOLA data. (Credit: MOLA Science Team)


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Location Map of Syrtis major that shows the study area. (Credit: MOLA Science Team)

MOLA reflectivity and radiometry data vs Ls for Syrtis Major. Error bar values are standard deviation over 1 day, when measurements were taken. Note that the time series are clearly anti-correlated, especially during the dust storm season (Ls=210-270.). (Credit: MOLA Science Team)

MOLA reflectivity and radiometry data vs L_s for Syrtis Major. Error bar values are standard deviation over 1 day, when measurements were taken. Note that the time series are clearly anti-correlated, especially during the dust storm season (L_s=210-270.). (Credit: MOLA Science Team)