RT Dataset -- Updated radiative transfer model for Titan in the near-infrared wavelength range: Validation against Huygens atmospheric and surface measurements and application to the Cassini/VIMS observations of the Dragonfly landing area

This dataset contains all Radiative Transfer (RT) results made for the paper. The data are stored in 5 zipped-folders names with the Cassini/VIMS cube flyby and id, or explicitly for Huygens/ULIS calibrated observations: TB_C1481624349_1 T40_C1578266417_1 T38_C1575509158_1 T40_C1578263500_1 T40_C1578263152_1 ULIS_observations The HLS folder contains the Cassini/VIMS cubes, the HLS end-member (End_member.txt), and the corresponding surface albedo (Surface_albedo.txt). In these folders, each VIMS pixel is stored in a .txt file with the following pattern: <CUBE_ID>_<PIXEL_SAMPLE>_<PIXEL_LINE> .txt It starts with a header describing the observation: CUBE_ID: the VIMS cube id (`C1234567890_1` format) SAMPLE: the pixel sample number. LINE: the pixel line number. LONG: the pixel longitude (in degree). LAT: the pixel latitude (in degree). INC: the surface incident angle (in degree). EMI: the surface emergent angle (in degree). PHASE: the surface phase angle (in degree). For the Selk crater cubes (T40_C1578266417_1, T38_C1575509158_1, T40_C1578263500_1, T40_C1578263152_1), the header also contains the spatial sampling and the radiative transfer model outputs: Spatial sampling (km/pix). Fh: the haze scaling factor. Fm: the mist scaling factor. 1-sigma (Fh): the 1-sigma uncertainty on Fh. 1-sigma (Fm): the 1-sigma uncertainty on Fm. Reduced chi2: the reduced chi2. Then contains the observed spectra: Column 1: the VIMS channel central wavelength (in micrometers). Column 2: the VIMS pixel I/F. Column 3: the VIMS pixel I/F 1-sigma uncertainty. For the Selk crater cubes (T40_C1578266417_1, T38_C1575509158_1, T40_C1578263500_1, T40_C1578263152_1), 3 columns are added for: Column 4: the surface albedo. Column 5: the upper 1-sigma uncertainty on the surface albedo. Column 6 : the lower 1-sigma uncertainty on the surface albedo. The ULIS folder contains the Huygens/ULIS calibrated observations (in I/F) and the simulations with 1-sigma uncertainties as a function of the altitude (in km): Column 1: the VIMS channel central wavelength (in micrometers), stopped at the end of the Huygens/ULIS wavelength range. Column 2: the ULIS I/F. Column 3 : the simulated I/F. Column 4: the lower 1-sigma uncertainty on the simulation. Column 5 : the upper 1-sigma uncertainty on the simulation.