Our methodology works by gridding the available retrievals of column dust optical depth (CDOD) from TES and THEMIS nadir observations, as well as the estimates of this quantity from MCS limb observations. The resulting (irregularly) gridded maps were validated with independent observations of CDOD by PanCam cameras and Mini-TES spectrometers aboard the Mars Exploration Rovers "Spirit" and "Opportunity", by the Surface Stereo Imager aboard the Phoenix lander, and by the Compact Reconnaissance Imaging Spectrometer for Mars aboard MRO.
Finally, regular maps of CDOD are produced by spatially interpolating the irregularly gridded maps using a kriging method. These latter maps are used as dust scenarios in the Mars Climate Database (MCD) version 5, and are useful in many modelling applications.
The two data sets (irregularly gridded maps and regularly kriged maps) for the ten available Martian years are publicly available and can be downloaded below (version 2.x).
The detailed description of the methodology and data sets can be found in the following scientific article:
Montabone, L., Forget, F., Millour, E., Wilson, R.J., Lewis, S.R., Cantor, B., Kass, D.,
Kleinböhl, A., Lemmon, M.T., Smith, M.D., Wolff, M.J., Eight-year Climatology of Dust Optical Depth on Mars,
Icarus (2015), doi: http://dx.doi.org/10.1016/j.icarus.2014.12.034 [Access the article]
If you have no subscription to the journal Icarus and cannot access the article, please send an email to the contact below.
MY24 MY25 MY26 MY27 MY28 MY29 MY30 MY31 MY32 !New! : MY33 Animation All MYs (tar.gz file)
Complete-coverage reconstructed maps (for Mars Climate Modeling): Daily dust scenarios (regularly kriged maps of 9.3 μm absorption column dust optical depth) for several Martian years (MY). Resolution: 3° longitude x 3° latitude. Data files are available in NetCDF format (56 MB for single year file; 448 MB for the complete zipped tar file including all years). Plotted maps for the 10 years (MY 24-33) are available as animated GIF (42 MB; each frame represents a sol-of-year with 10 maps, one for each available Martian year).
MY24 MY25 MY26 MY27 MY28 MY29 MY30 MY31 MY32 !New! : MY33 Animation All MYs (tar.gz file)
N.B.1 To get the extinction optical depth, you can multiply the absorption optical depth by 1.3. Equivalent visible column optical depths can be obtained by multiplying the 9.3 μm absorption column dust optical depth by 2.6. See detailed discussion in Montabone et al., Icarus, 2015, Section 2.3.4
N.B.2 The data files include both the column dust optical depth normalized to the 610 Pa reference level and the column dust optical depth normalized to the gridded surface pressure value (surface pressure is gridded from the Mars Climate Database). If you require a local column optical depth, you could either interpolate the provided variable normalized to the gridded MCD surface pressure, or multiply the provided variable normalized to 610 Pa by "surface pressure (Pa)/610", where "surface pressure" is the local surface pressure of your choice.
N.B.3 The files for MY 33 are version 2.1. Two things have changed with respect to version 2.0 of previous Martian years: 1) We use the latest release of MCS retrievals (version 5.2 with "2-dimensional" retrievals, see Kleinböhl, A., et al., J. Quant. Spectrosc. Radiat. Transf. 187, pp 511-522, 2016), and 2) We give less weight to THEMIS retrievals of CDOD with respect to MCS estimates of CDOD: 50% weight with time window of 1 sol, 10% with time windows of 3, 5, 7 sols (see Montabone et al., Icarus, 2015, for an explanation of time windows).
Figures: (Left) Zonal means of the daily irregularly gridded maps of 9.3 μm absorption column dust optical depth normalized to the reference 610 Pa pressure level for the different Martian Years. (Right) Zonal means of the daily regularly kriged maps of 9.3 μm absorption column dust optical depth normalized to the reference 610 Pa pressure level for the different Martian Years.
Although we do not require any formal registration to download the data sets, we would highly appreciate if you tell us who you are if you download the files, by sending an informal email to the contact email address above, including at least your name, affiliation (if applicable), and planned use of the data sets. This would help us a lot to assess the impact of our work, and would make sure that we will keep you updated about possible errors, warnings, and future versions. We will not use your contact details for anything else than just keeping you updated about the data sets when needed. Even if you do not want to be updated, please consider sending us an email to tell us who you are, and make explicit that you do not want to be contacted further.
These data are made publicly available on the condition that we provide no warranties regarding the reliability, validity or accuracy of the data, and we bear no responsibility for any use made of such data.