Data for: Coupled Photochemical-Climate Modeling of Plausible Tenuous Outgassed Atmospheres on the TRAPPIST-1 Planets

This dataset contains the TRAPPIST-1 planet modeled atmospheric gas volume mixing ratios, pressure-temperature profiles, and spectra presented in Gialluca, et al. (2026). Python scripts that can be used to recreate plots from the paper can be found on GitHub. We briefly describe the data files uploaded here. There are 7 json files, one for each of the TRAPPIST-1 planets (b, c, d, e, f, g, and h). Each can be loaded as a Python dictionary with the following (example given for T-1b): import json f = open('T1b_Atmospheres_Database.json', 'r') data_dictionary = json.load(f) f.close() In the data dictionary, for b, c, d, and e there are 4 keys corresponding to sub-dictionaries: ['H2O', 'H2O-CO2', 'SO2-H2O', 'SO2-H2O-CO2']. For f, g, and h, there are 2 keys: ['H2O-CO2', 'SO2-H2O-CO2'], as no atmospheres outgassed by water only were stable for these planets (see Gialluca, et al. 2026, for further explanation). These keys group atmospheres into their source, "H2O" refers to atmospheres sustained by water outgassing only, "H2O-CO2" are atmospheres with both water and carbon dioxide outgassing, "SO2-H2O" are atmospheres with water outgassing and a trace SO2 injection, and "SO2-H2O-CO2" are atmospheres with both water and carbon dioxide outgassing along with a trace SO2 injection. Within a subdictionary given by one of the outgassing types described above (e.g., data_dictionary['H2O']), there will be one key called 'AtmIDs' with a list of possible ID numbers, and then a series of keys denoted by 'AtmX' where X is any of the ID numbers in the list corresponding to 'AtmIDs'. For a given atmosphere (e.g., data_dictionary['H2O']['Atm1']), there is a dictionary containing all of the data for that atmosphere broken into the following keys: 'MetaData' - Gives the boundary conditions sampled for that atmopshere in a list: For 'H2O' atmopsheres, this list corresponds to: [H2O Outgassing Rate [cm^-2 s^-1], O Effusion Velocity [cm/s], O2 Effusion Velocity [cm/s], O3 Deposition Velocity [cm/s], H2O2 Deposition Velocity [cm/s]] For 'H2O-CO2' atmospheres, this list corresponds to: [H2O Outgassing Rate [cm^-2 s^-1], CO2 Outgassing Rate [cm^-2 s^-1], O Effusion Velocity [cm/s], O2 Effusion Velocity [cm/s], O3 Deposition Velocity [cm/s], H2O2 Deposition Velocity [cm/s], CO Deposition Velocity [cm/s], CO2 Effusion Velocity [cm/s]] For 'SO2-H2O' atmopsheres, this list corresponds to: [H2O Outgassing Rate [cm^-2 s^-1], Trace SO2 Volume Mixing Ratio at the Surface Layer, O Effusion Velocity [cm/s], O2 Effusion Velocity [cm/s], O3 Deposition Velocity [cm/s], H2O2 Deposition Velocity [cm/s]] For 'SO2-H2O-CO2' atmospheres, this list corresponds to: [H2O Outgassing Rate [cm^-2 s^-1], CO2 Outgassing Rate [cm^-2 s^-1], Trace SO2 Volume Mixing Ratio at the Surface Layer, O Effusion Velocity [cm/s], O2 Effusion Velocity [cm/s], O3 Deposition Velocity [cm/s], H2O2 Deposition Velocity [cm/s], CO Deposition Velocity [cm/s], CO2 Effusion Velocity [cm/s]] 'SurfPress' - Gives the surface pressure of the atmosphere in Bars 'PTZOut' - Gives a subdictionary with the pressure, temperature, and volume mixing ratio profiles for the atmosphere as a function of altitude. In this subdictionary 'ALT' is altitude in cm (e.g., data_dictionary['H2O']['Atm1']['PTZOut']['ALT']), 'PRESS' is pressure in bars, 'TEMP' is temperature in K, and after that there are a number of species VMRs that can be accessed, use the following command to see all the species: print(data_dictionary['H2O']['Atm1']['PTZOut'].keys()) 'Trnst_Wav' - Gives the list of wavelength [microns] that correspond to the transit spectrum 'Trnst_Depth' - Gives the transit depth corresponding to the wavelength array (multiply by 1e6 to get transit depth in ppm) 'Dayside_Wav' - Gives the secondary eclipse emission spectrum wavelength array in microns 'Dayside_Fp' - Gives the planetary flux corresponding to the dayside wavelength array [w m^-2 um^-1] 'Dayside_Fstar' - Gives the stellar flux corresponding to the dayside wavelength array [w m^-2 um^-1]. To get the emission in ppm, do: (Fp/Fstar) * (Rp/a)^2 * 1e6, where Rp is the radius of the planet and a is the semi-major axis. 'Nightside_Wav' - Gives the nightside emission spectrum wavelength array in microns 'Nightside_Fp' and 'Nightside_Fstar' are the same as their dayside counterparts, except for the nightside emission. Note: Only the interior planets (b, c, and d) have emission spectra (dayside and nightside). All spectra are at high resolution, plots in the paper typically bin spectra to an R of 120.