Abstract This is the second part of an investigation of water vapor in the Martian atmosphere using solar occultation observations by the Nadir and Occultation for MArs Discovery (NOMAD) spectrometer on board the ExoMars Trace Gas Orbiter. Following the analysis of six Earth years of NOMAD observations performed in the first part, a cross‐validation between NOMAD and ACS results is presented, showing global as well as profile‐by‐profile comparisons. The results reveal an overall good agreement between different teams and instruments, taking into account the different retrieval methodologies. In order to compare with model predictions, we perform an exhaustive analysis of the water vapor simulated by Mars Planetary Climate Model (MPCM). It shows that the MPCM reproduces most of the water vapor climatological features observed in the atmosphere. However, several discrepancies between model and observations are noticed. Some of these are possibly related to the vertical distribution of dust and its effect on the global circulation and on the water vapor vertical transport. Other data‐model differences found at 60 km seem to be related to discrepancies on the water ice cloud formation in the MPCM. We include a cluster analysis of Martian water vapor vertical profiles for the first time. This technique applied to MPCM and NOMAD water vapor retrievals reveal distinct groups of profiles being representative of specific seasons and latitudinal regions, similarly distributed in both model and observations. Moreover, it allows us to provide a simplified water vapor climatology, useful to detect out‐of‐season events and biases in the retrieval processes.
Brines et al. (2026) studied this question.