DATA REPOSITORY for Matsubara, Y., Howard, A. D., and Irwin, R. P., III (2018). Constraints on the Noachian paleoclimate of the martian highlands from landscape evolution modeling.  Journal of Geophysical Research: Planets. https://doi.org/10.1029/2018JE005572.

SOURCE FILES FOR MARSSIM LANDSCAPE EVOLUTION MODELING:

marssim_program_source_files.zip
The program Fortran source files (Fortran95). These should be compiled and then linked to form an executable file. The program is compatible with the GFORTRAN distribution available on most programming environments as well as for Intel Fortran. An example batch compilation file for Intel Fortran in a Linux environment is included as the file “compile” and the program linking file “link”. Documentation for the program is included as “Marssim_program.doc”. This documentation is for an earlier version of the program, so that a few newer features are not discussed. A new distribution of the MARSSIM program is currently being prepared, and anyone contemplating using the source files for new projects should contact Alan Howard (ah6p@virginia.edu or ahoward@psi.edu).

parameter_files_for_Noachis_and_Cimmeria.zip
The parameter files necessary to run example simulations for the Noachis and Cimmeria regions discussed in the paper. Depending upon the region to be simulated, the “Noachis_..” or “Cimmeria_..” titled files should be renamed without the region prefix, for example, “Noachis_MARSSIM.PRM” should be renamed “MARSSIM.PRM”. In addition to the renamed files for the given region, the files “INRATES.DAT”, “GRAVEL_MIXTURE.PRM”, “RESIST.IN”, and “ERODE.STOP” should be present in the directory where the program is executed, although only “ERODE.STOP” is actually used.  “ERODE.STOP” is read every 10 iterations and if the leading letter is changed from 0 to 1 the program will terminate gracefully with full output files.

STUDY AREA IMAGE MOSAICS AND TOPOGRAPHY:
All image mosaics and topography are geographic (lat/long). The base images were used in Figures 3a (Noachis) and 4a (Cimmeria) in the paper.

noachis_base_TDIR593_MOLA128.tif
Mars Odyssey Thermal Emission Imaging System (THEMIS) daytime infrared mosaic, version 11, 100 m/pixel (USGS Astrogeology Science Center, Edwards et al., 2011), colorized with Mars Global Surveyor Mars Orbiter Laser Altimeter (MOLA) Mission Experiment Gridded Data Record (MEGDR) topography, 128 pixel/degree (NASA Planetary Data System, Smith et al., 2003), for the Noachis study area bounded by 21.6–28.6°S, 22–34°E. The elevation color scheme is shown in Figures 3 and 4 in the paper.

noachis_base_TDIR593_MOLA128.tfw
ArcGIS world file to georeference the above referenced mosaic.

cimmeria_base_TDIR593_MOLA128.tif
THEMIS daytime infrared mosaic, version 11, 100 m/pixel, colorized with MOLA MEGDR topography, 128 pixel/degree, for the Cimmeria study area bounded by 16.5–26.5°S, 132.25–144.25°E. The elevation color scheme is shown in Figures 3 and 4 in the paper.

cimmeria_base_TDIR593_MOLA128.tfw
ArcGIS world file to georeference the above referenced mosaic.

noachis_MOLA128.tif
MOLA MEGDR topography, 128 pixel/degree, for the Noachis study area, geoTIFF format.

cimmeria_MOLA128.tif
MOLA MEGDR topography, 128 pixel/degree, for the Cimmeria study area, geoTIFF format.

INITIAL CONDITIONS DIGITAL ELEVATION MODELS:
These DEMS are shown in Figures 3b (Noachis) and 4b (Cimmeria) in the paper.

noachis_initial_DEM.tif
Initial conditions DEM for the Noachis study area, 32 pixels/degree, 301 pixels wide by 251 high, GeoTIFF format. The study area boundaries correspond to the centers of the corner pixels.

cimmeria_initial_DEM.tif
Initial conditions DEM for the Cimmeria study area, 25 pixels/degree, 385 pixels wide by 225 high, GeoTIFF format. The study area boundaries correspond to the centers of the corner pixels.

EXAMPLE MODEL RESULTS:
These DEMs were used in Figures 9b (Noachis) and 11b (Cimmeria) in the paper.

noachis_best_NTa3X15w1R10_41
Output DEM for Noachis study area, 32 pixels/degree, 301 pixels wide by 251 high, GeoTIFF format. The study area boundaries correspond to the centers of the corner pixels.

cimmeria_best_TCa3X15w05R100_28
Output DEM for Cimmeria study area, 25 pixels/degree, 385 pixels wide by 225 high, GeoTIFF format. The study area boundaries correspond to the centers of the corner pixels.

REFERENCES:

Edwards, C. S., Nowicki, K. J., Christensen, P. R., Hill, J., Gorelick, N., and Murray, K. (2011). Mosaicking of global planetary image datasets: 1. Techniques and data processing for Thermal Emission Imaging System (THEMIS) multi-spectral data. J. Geophys. Res., 116, E10008. doi:10.1029/2010JE003755 or http://dx.doi.org/10.1029/2010JE003755

Smith, D. E., Zuber, M. T., Neumann, G. A., Guinness, E. A., and Slavney S. (2003). Mars Global Surveyor Laser Altimeter Mission Experiment Gridded Data Record, MGS-M-MOLA-5-MEGDR-L3-V1.0. NASA Planetary Data System.