The ouput simulation data of the Exo-FMS GCM and of the post-processing with gCMCRT for Modelling the 3D atmospheric structure of the cold Jupiter WD1856+534b orbiting a white dwarf

White Dwarf (WD) systems can provide insights into the Earth's future after the Sun has entered the red giant branch (RGB). The cold Jupiter WD-1856b+534b (WD-1856b) can provide useful information about habitability conditions of planets after the RGB phase like their metallicity and temperature structure. Recent JWST observations targeted WD-1856b, and more observations are on schedule. For supporting the interpretation of observations, we computed the first simulations with a 4D general circulation model (GCM) and post-processed emission spectra of a planet orbiting a WD. We used the Exo-FMS GCM with a correlated-k radiative transfer (RT) scheme and mixing length theory (MLT). Additionally, we computed the chemical abundances of 13 chemical species with the miniature chemical kinetics model mini-chem and with FastChem 2. Because there are uncertainties in the metallicity and internal temperature of WD-1856b, we run simulations with 1x, 10x, and 100x Solar compositions, and with low and high internal temperatures (Tint=100 and 500 K). We generated emission spectra and brightness temperature curves with the GCM output by the gCMCRT method. Our results suggest an increase of the frequent elements like H2O, CO and CH4. CO and CO2 at higher Tint=500 K if the metallicity is set higher. At Tint=100 K, H2O and CH4 become more relevant and increase to a few percentages at 100x Solar. We expect H2O cloud formation in the upper atmosphere in the 100x Solar case at Tint=500 K and in all cases with Tint=100$ K. Therefore, H2O is likely removed in the upper atmosphere.