Repository: Evidence of Exposed Dusty Water Ice within Martian Gullies
Khuller and Christensen (2020)

Contents:

1. Blaney et al. (2009) Ice and Soil Spectra
a) DG_after: Ice spectra on Sol 82
b) DG_initial: Ice spectra on sol 28
c) Soil: Soil spectra
d) DG_Hirise: Spectra in 1a-c sampled at HiRISE wavelengths


2. Dust spectrum derived from dust refractive index data from Wolff et al. (2009)
a) Dust_1.8: Pure dust spectra
b) Dust_1.8: Pure dust spectra, sampled at HiRISE wavelengths
c) Wolff_2009_Dust_k and Wolff_2009_dust_n: Dust refractive indices

3. Snow-dust mixture albedos from Khuller and Christensen (2020)
a) Snow_1000_pure_550: Pure snow albedo 
b) Snow_1000_pure_550_hirise: Pure snow albedo, sampled at HiRISE wavelengths
c) Dusty_Snow_1000_pure_550: Dusty snow albedos (1-1000 ppmw dust)
d) Dusty_Snow_1000_pure_550_hirise: Dusty snow albedos (1-1000 ppmw dust), sampled at HiRISE wavelengths
e) Dusty_Snow_1000_pure_550_2: Dusty snow albedos (10,000-100,000 ppmw dust)
f) e) Dusty_Snow_1000_pure_550_hirise_2: Dusty snow albedos (10,000-100,000 ppmw dust), sampled at HiRISE wavelengths

4. Martian snow and ice effective thermal conductivity, based on Clow (1987)
Mars_Snow_Ice_Conductivity: Effective martian snow (50,400,550 kg/m^3 densities and ice effective thermal conductivity

5. Image Details for HiRISE, CTX and THEMIS images used in this work
Evidence of Exposed Dusty Water Ice within Martian Gullies_Image_Details

6. Supplementary Animations (1-3) of changes observed within gully seen in HiRISE images ESP_013067_1470 and ESP_065800_1470