Icarus

Each FITS file contains spectra used and the thermal and abundances profiles (C2H2, C2H4, C2H6, CH3CCH, C3H8, C4H2, C6H6, CO2, HCN, HC3N) for a given observation sequence (the FITS file name). The FITS file contains also the NESR (Noise Equivalent Spectral Radiance) used in the study. We add a README.txt file to help the user to extract the information contains in the FITS file with an IDL or Python environment.

The supporting information consists of: 1. A text file with seven supporting figures with captions (referred to as S1-S7 in the paper), as well as additional text (and Figures S8 – S10) that gives detail on the Monte Carlo model used to assign ages to martian landforms in the Gale Crater region. 2. Matlab scripts to generate Figures 2, 5, 7, and 8 in the main text, and an example crater counting file (.diam) 3. Crater count data for the features mapped in Figure 9 (and S7), as well as Table S1 and S2 (both in .xlsx and .csv format)

Database of classified craters including center point latitude and longitude, diameter (km), and degradation class. Craterstats output files used to generate Figure 6.

Ion mobility mass spectrometry data of tholins

Rb, Sr concentrations, 87Sr/86Sr and 87Rb/86Sr ratios of standards and heated CM chondrites. Age estimation of the heating event of five CM chondrites

All CRISM spectra from plots are stored in an Excel worksheet. Includes ratio spectra as shown in figures as well as original reflectance spectra and alternative ratio spectra. Mosaics of Jezero CRISM RGB combinations over CTX basemaps are included at various zooms and resolutions, as used in figures.

We provide three separate .csv files that contain the supplementary material requested by Reviewer 1. An explanation of the contents of each file is given in the file description.

Data files for the submitted Icarus paper: "Modeled Small-scale Crack Orientations on Martian Surface Rocks caused by Differential Insolation-Mobilized Water". Data files contain the results of the combination of geometric and radiative transfer models. Data files are for a specific depth, width and length of V-shaped crack (as specified in the filename, where d is the depth, w is the width, and l is the length). These files are for those runs with no diurnal or seasonal restrictions. The files themselves are in the following format: planetary latitude (degrees) \t Solar longitude (degrees) \t crack offset clockwise from north (degrees) \t total energy received by the bottom third of the crack (J). Energy is calculated using the dimensions in meters so these values should be scaled according to the actual dimensions of the crack or can be used as a relative energy for different geometries and orientations (as in the paper).

This file contains supplementary figures as well as a description of datasets and code developed for this project. Section 1 is full elevation, slope, orientation, and thermal inertia histograms for all studied sites. Section 2 is a description of data and Matlab code.

Tabulation of CRISM observation IDs, mineral identifications, and coordinates of regions of interest of mineral identifications. For spectra in Figure 2, wavelength in nm, numerator spectrum, denominator spectrum of nearby bland area, and ratio spectrum.