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The evolution and distribution of the angular momentum of dark matter (DM)halos have been discussed in several studies over the past decades. Inparticular, the idea arose that angular momentum conservation should allow toinfer the total angular momentum of the entire DM halo from measuring theangular momentum of the baryonic component, which is populating the center ofthe halo, especially for disk galaxies. To test this idea and to understand theconnection between the angular momentum of the DM halo and its galaxy, we usethe Magneticum simulations. We successfully produce populations of spheroidaland disk galaxies self-consistently. Thus, we are able to study the dependenceof galactic properties on their morphology. We find that (1) the specificangular momentum of stars in disk and spheroidal galaxies as a function oftheir stellar mass compares well with observational results; (2) the specificangular momentum of the stars in disk galaxies is slightly smaller compared tothe specific angular momentum of the cold gas, in good agreement withobservations; (3) simulations including the baryonic component show a dichotomyin the specific stellar angular momentum distribution when splitting thegalaxies according to their morphological type (this dichotomy can also be seenin the spin parameter, where disk galaxies populate halos with slightly largerspin compared to spheroidal galaxies); (4) disk galaxies preferentiallypopulate halos in which the angular momentum vector of the DM component in thecentral part shows a better alignment to the angular momentum vector of theentire halo; and (5) the specific angular momentum of the cold gas in diskgalaxies is approximately 40 percent smaller than the specific angular momentumof the total DM halo and shows a significant scatter.

Connecting Angular Momentum and Galactic Dynamics: The complex Interplay between Spin, Mass, and Morphology