Repository: Potential for Photosynthesis on Mars within snow and ice

This repository contains:

1. Modeled Spectral Irradiances (W m-2 micron-1) within Vertically Inhomogeneous Glacier Ice from Khuller, Warren, Christensen & Clow (2024)

a) Fig_1_12cm_model: Modeled Spectral Irradiance at 12 cm b) Fig_1_36cm_model: Modeled Spectral Irradiance at 36 cm c) Fig_1_58cm_model: Modeled Spectral Irradiance at 58 cm d) Fig_1_77cm_model: Modeled Spectral Irradiance at 77 cm 

2. Modeled Spectral Actinic Flux (W m-2 micron-1) from Khuller, Warren, Christensen & Clow (2024)

a) Clean Snow/Firn/Ice (without dust) at 33 S latitude    i) Fig_2a: Pure snow with 0.5 mm grain size    ii) Fig_2b: Pure firn with 2.5 mm grain size    iii) Fig_2c: Pure glacier ice with 14 mm grain size

b) Clean Snow/Firn/Ice (without dust) at 54 N latitude    i) Ext_Fig_2a: Pure snow with 0.5 mm grain size    ii) Ext_Fig_2b: Pure firn with 2.5 mm grain size    iii) Ext_Fig_2c: Pure glacier ice with 14 mm grain size    

c) Dusty Snow/Firn/Ice (with 0.01% dust by mass) at 33 S latitude    i) Fig_2d: Dusty snow with 0.5 mm grain size    ii) Fig_2e: Dusty firn with 2.5 mm grain size    iii) Fig_2f: Dusty glacier ice with 14 mm grain size

d) Dusty Snow/Firn/Ice (with 0.01% dust by mass) at 54 N latitude    i) Ext_Fig_2d: Dusty snow with 0.5 mm grain size    ii) Ext_Fig_2e: Dusty firn with 2.5 mm grain size    iii) Ext_Fig_2f: Dusty glacier ice with 14 mm grain size

e) Dusty Snow/Firn/Ice (with 0.1% dust by mass) at 33 S latitude    i) Fig_2g: Dusty snow with 0.5 mm grain size    ii) Fig_2h: Dusty firn with 2.5 mm grain size    iii) Fig_2i: Dusty glacier ice with 14 mm grain size

f) Dusty Snow/Firn/Ice (with 0.1% dust by mass) at 54 N latitude    i) Ext_Fig_2g: Dusty snow with 0.5 mm grain size    ii) Ext_Fig_2h: Dusty firn with 2.5 mm grain size    iii) Ext_Fig_2i: Dusty glacier ice with 14 mm grain size    

3. Modeled Depths for DNA Damage Limit, PAR Upper Limit, and PAR Lower Limit (meters) from Khuller, Warren, Christensen & Clow (2024)

a) Sensitivity to dust contentFILE FORMAT: Dust Content (ppmw), DNA Damage Limit Depth (m), PAR Lower Limit Depth (m), PAR Upper Limit Depth (m)    i) final_Depths_south_dust_sensitivity:  sensitivity to dust content for the martian southern hemisphere    ii) final_Depths_north_dust_sensitivity: sensitivity to dust content for the martian northern hemisphere

b) Sensitivity to ice grain radiusFILE FORMAT: Ice Grain Radius (micron), DNA Damage Limit Depth (m), PAR Lower Limit Depth (m), PAR Upper Limit Depth (m)    i) final_Depths_south_radius_sensitivity:  sensitivity to ice grain radius for the martian southern hemisphere    ii) final_Depths_north_radius_sensitivity: sensitivity to ice grain radius for the martian northern hemisphere

c) Sensitivity to latitudeFILE FORMAT: Latitude (degrees), DNA Damage Limit Depth (m), PAR Lower Limit Depth (m), PAR Upper Limit Depth (m)    i) final_Depths_south_latitude_sensitivity:  sensitivity to latitude for the martian southern hemisphere    ii) final_Depths_north_latitude_sensitivity: sensitivity to latitude for the martian northern hemisphere

d) Sensitivity to solar zenith angleFILE FORMAT: Solar Zenith Angle (degrees), DNA Damage Limit Depth (m), PAR Lower Limit Depth (m), PAR Upper Limit Depth (m)    i) final_Depths_south_zenith_sensitivity:  sensitivity to solar zenith angle for the martian southern hemisphere    ii) final_Depths_north_zenith_sensitivity: sensitivity to solar zenith angle for the martian northern hemisphere

4. Wavelengths used for files listed in 1 from Khuller, Warren, Christensen & Clow (2024)wavelengths_greenland: wavelength in microns

5. Wavelengths used for files listed in 2 and 3 from Khuller, Warren, Christensen & Clow (2024)wavelengths: wavelength in microns

6. Depths used for files listed in 2 from Khuller, Warren, Christensen & Clow (2024)depths: depths in meters

7. Normalized DNA spectrum used in Khuller, Warren, Christensen & Clow (2024)norm_dna_spectrum: normalized DNA spectrum