Mars Dust Activity Database for Mars South Pole

This version only replaces the MDAD_Bstorm.ipynb in the tar file to fix a bug in the final figure.  All figures are exactly reproduced from the paper version.  The original MY30.tar.gz file is copied from the previous version for completeness.

The Mars Dust Activity Database for the South Pole includes storm boundaries for every instance from the Mars Color Imager (MARCI) for the period of Ls=255–280° in MY 30 centered around 90°S.  A single tar file contains two folders, the "MDADbstormMY30.csv" file, a Jupyter notebook "MDAD_Bstorm.ipynb", and two figures that are generated by the notebook for the paper Campbell et al. (2025).

The csv folder contains  395 *.csv files, each of which corresponds to a single dust storm instance on a single MARCI swath.  The csv files are named with the following convention:  SWATH#_LSS#_MEM_ZZZb.csv, where SWATH# is the swath number, ranging 021717–022214 and LSS is the areocentric longitude of the swath.  The last seven characters are the member ID for the storm instance, with ZZZ ranging 200–329 and "MEM" the subphase on which the member starts.  For storms that have merged, only the member ID with the smallest ZZZ is included in the file name, and the character "b" is only included in the file name for splitting storms.  Each *.csv file consists of a two column matrix.  Column 1 is cartesian x coordinate in the frame of the png files, and column 2 is the y coordinate, with (0,0) at the bottom left corner of the png images.  Each x, y point is a pixel on the boundary of the storm instance.

MDADbstormMY30.csv is a table with each row identifying specific properties of each of the individual dust storm instances in a single swath. The format of an entry is: Mars Year, Mission subphase, swath number, Ls, Centroid longitude, Centroid latitude, Area (square km), Member ID, Maximum latitude, Minimum latitude, Confidence interval, Missing data. Each entry has a member ID that can be carried across sols if the motion of the dust storm is feasible. The member ID has the format: SUB_XXX, where “SUB” is the Mission subphase containing the storm, and “XXX” is a number from 001 to 133. Different members can merge into a single member, noted in the member ID with a “+”. The ID of the combining member that is numerically smallest is always listed first in the combined ID. Conversely, a single member can split into multiple members, noted at the end of the member ID with a “b” or “c”. A confidence level of 50,75,100 is assigned to each dust storm to describe the accuracy of boundaries, with 50 being the least confident. A confidence level of 100 means that the entire perimeter of the dust storm is distinct. Any storm suffering from missing data is labeled with a “yes” under the “missing data” column.

MDAD_Bstorm.ipynb demonstrates how the read the files from the dataset and recreate two of the figures (provided as figure13.png and figure15.png) from Campbell et al. (2025)

Campbell, C.L., Guzewich, S.D., Battalio, J.M., Robbins, S.J., Batterson, C.M.L., 2025. Martian South Polar Summer Dust Storms in Observations, Reanalyses, and Modeling. JGR Planets 130, e2025JE009268. https://doi.org/10.1029/2025JE009268