Figs. A.3 and A.4 show explicitly the evolution of the star, cold and hot gas mass in SAMs and simulations based on the trees of the two re-simulated individual halos for a 2 × (dashed lines) and 4 × (solid lines) resolution. As expected from the similar
evolution of the dark matter component, for both, the low and the high mass halo re-simulations, we find between SAMs and simulation no significant difference in the evolution of the central galaxy/main halo. Therefore, due to computational costs, we restrict our study to 2× re-simulations of40 individual halos.
Figure A.1: Upper panel: comparison of aggregation history (Resim M0501) of the halo mass for two different mass resolutions (2x: red, dotted line and 4x: black, solid line) in the SPH-re-simulations of a3.0×1012M
" halo. Intermediate panel: Number of
minor mergers (>10 : 1) as a function of lookback time for the two different resolution limits. Lower panel: Number of major mergers (< 10 : 1) as a function of lookback time for the two different resolution limits.
Figure A.2: Same as Fig. A.1, but for the halo M1646 with a smaller halo mass
8.0×1011M
Figure A.3: Evolution of the baryonic components for two different mass resolutions (2x: dotted lines, 4x: solid lines) for the halo M0501. The upper panel shows the evolution of the stellar component, the middle panel the evolution of the cold gas fraction and the lower panel corresponds the hot halo gas component. Black lines illustrate the re-simulations, colored lines the different SAM versions.
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