Comparisons of the simulated martian HDO cycle with the upgraded LMD Mars GCM

We present here simulations of the HDO cycle on Mars, using an updated version of the LMD Mars GCM. This is a follow-up from Rossi et al. (2021), this time including more physical processes: microphysics of cloud formation, radiatively active clouds, effect of kinetics during fractionnation by condensation. The simulations pertain to two dust scenarios representative of martian years 34 and 35. There are different types of files: * yearly file (MY34 and 35 combined) representing column integrated quantities interpolated at local time of 14h, zonally averaged, as a function of latitude and solar longitude * yearly file (MY34 and 35 combined) representing quantities interpolated at local time of 14h at altitudes of 30 and 60~km, zonally averaged, as a function of latitude and solar longitude * yearly file (MY34 and 35 separately) representing quantities interpolated at local time of 14h, zonally averaged, as a function of altitude above the areoid and for solar longitudes of 180, 200, 210, 260. * GCM outputs colocated to the coordinates of TGO/ACS-MIR observations (in altitude above areoid and time). * The data used from ACS-MIR, processed by Juan Alday (https://doi.org/10.1038/s41550-021-01389-x), reinterpolated vertically and stored in a netcdf