Mars PCM temperature results from MY 36 LS = 0° to MY 37 LS = 60°

We present here the numerical simulation results of the temperature in the Martian atmosphere from Martian Year (MY) 36 solar longitude (LS) 0° to MY 37 LS 60°. The data is based on the Mars PCM (version 6). A description of the model setting is presented in Fan et al. (2024), and a general description of the model architecture is given in Forget et al. (1999). The model has a 64×48×73 grid in longitude, latitude, and pressure levels, which corresponds to a horizontal resolution of 5.625° and 3.75° in longitude and latitude, respectively, and 73 hybrid terrain-following vertical pressure levels (σ-grid) from surface to ~2×10^-3 Pa. The run has 960 dynamical timesteps in each Martian day, and the physical timestep is 7.5 Martian minutes.The dust injection is semi-interactive regulated by the MY 36 and MY 37 dust scenarios.The data is seven NetCDF files, each including two Martian months. They are self-explanatory with the meanings of variables included in their headers, which contain atmosphere temperature, surface temperature, and surface pressure in the simulation, together with information about the four-dimensional grid in longitude, latitude, pressure level, and time, and also the corresponding LS at each timestep. The variable names of the longitude, latitude, pressure level, and time of grid points and their units are latitude [degree], longitude [degree], altitude [Pa], and Time [sol], respectively. The names of the variables and their corresponding units and dimensions are below.Temperature [K]: temp[Time, altitude, latitude, longitude]Surface temperature [K]: tsurf[Time, latitude, longitude]Surface pressure [Pa]: ps[Time, latitude, longitude]Solar longitude [degree]: Ls[Time] Reference: (1) Forget et al. (1999) Improved general circulation models of the Martian atmosphere from the surface to above 80 km. Journal of Geophysical Research, 104(E10), 24155-24176. (2) Fan et al. (2025) Diurnal temperature variations and migrating thermal tides in the Martian lower atmosphere observed by the Emirates Mars InfraRed Spectrometer. Journal of Geophysical Research: Planets. 130, e2025JE009092.