Climatologies of the Martian Atmospheric Dust Optical Depth

Introduction

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, by the Compact Reconnaissance Imaging Spectrometer for Mars and the Mars Color Imager camera aboard MRO, and by the MastCam camera aboard the Mars Science Laboratory "Curiosity".

Finally, regular maps of CDOD are produced by spatially interpolating the irregularly gridded maps using a kriging method. These latter maps are used as column-integrated dust scenarios in the Mars Climate Database (MCD) version 5, and are useful in many modelling applications.

The two types of data set (irregularly gridded maps and regularly kriged maps) for the twelve 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 articles:

• 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 251, pp. 65-95 (2015), doi: https://doi.org/10.1016/j.icarus.2014.12.034 [Access the article]
• Montabone, L., Spiga, A., Kass, D. M., Kleinböhl, A., Forget, F., Millour, E., Martian Year 34 Column Dust Climatology from Mars Climate Sounder Observations: Reconstructed Maps and Model Simulations. J. Geophys. Res. - Planets (2020), doi: https://doi.org/10.1029/2019JE006111 [Access the article]

If you have no subscriptions to the journal Icarus or JGR, and cannot access the articles, please send an email to the address in the 'Contact' section below. Check the 'Contact' section also if you want to receive updates on future versions of the dust climatology.

Data sets

Daily irregularly gridded maps of 9.3 μm absorption column dust optical depth for several Martian years (MY). Spatial Resolution: 6° longitude x 3° latitude for MY24, 25, 26; 6° longitude x 5° latitude for the other Martian years. Temporal resolution: 24 hours (i.e. 1 map per sol). Data files are available in NetCDF format (74 MB for MY 24, 25, 26; 45 MB for MY 27 through 33; 50 MB for MY 34; 61 MB for MY 35; 312 MB for the complete zipped tar file including all years). Plotted maps for the first 10 years (MY 24-33) are available as animated GIF (53 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 MY33 Animation MY34 !New! : MY35 All MYs (tar.gz file)

Sub-daily irregularly gridded maps of 9.3 μm absorption column dust optical depth for MY 34 and MY 35. Spatial resolution: 6° longitude x 5° latitude. Temporal resolution: 6 hours (i.e. 4 maps per sol). Data file is available in NetCDF format (177 MB for MY 34, 221 MB for MY 35).

MY34 !New! : MY35

Complete-coverage reconstructed maps (for Mars Climate Modeling):

Daily column-integrated dust scenarios (regularly kriged maps of 9.3 μm absorption column dust optical depth) for several Martian years (MY). Spatial resolution: 3° longitude x 3° latitude. Temporal resolution: 24 hours (i.e. 1 map per sol). Data files are available in NetCDF format (56 MB for single year files; 543 MB for the complete zipped tar file including all years). Plotted maps for the the first 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 MY33 Animation MY34 !New! : MY35 All MYs (tar.gz file)

Important notes:

• 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;
• 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;
• 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);
• The files for MY 34 and MY 35 are version 2.5 (daily gridded and kriged maps) and version 2.5.1 (four gridded maps per sol). The details on the production of MY 34 data sets included in Montabone et al. (2020) are also valid for MY 35. We just remind here that the daily gridded maps v2.5 are the diurnal averages of the maps in v2.5.1, and the daily kriged maps v2.5 interpolate the daily gridded maps v2.5. We have not produced kriged maps directly from v2.5.1, for reasons explained in Montabone et al., 2020.
• !New! : Note that in MY 35 data sets we have added new variables to estimate the Earth date and time of the CDOD values in the maps. This could be useful if one wants to compare our CDOD values to other types of observations, and requires an accurate time reference. The details of these new variables (earliest, average, latest Modified Julian Date of all observations used to reconstruct a gridded or kriged map at a given time, as well as Modified Julian Date anomaly of each grid point in a gridded map at a given time with respect to the corresponding average Modified Julian Date of all observations) are included in the header of the NetCDF files. We would appreciate feedback from users on this new feature.

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.

Contact

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, and you will receive (sporadic) updates on future developments of the dust climatology. In order to do that, please fill and submit this very short Google Form including your name, affiliation (if applicable), email address, 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. You will always be able to unsuscribe by sending a request to the contact email above, should you no longer be interested in the MCD dust climatology.

Copyright and disclaimer

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.