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We study the present-day connection between galaxy morphology and angularmomentum using the {\sc Dark Sage} semi-analytic model of galaxy formation. Forgalaxies between $ 10^{11}-10^{12} \mathrm{M}_{\odot}$ in stellar mass, themodel successfully predicts the observed trend whereby galaxies with moreprominent disks exhibit higher {\em stellar} disk specific angular momentum($j_{\rm stellar, disk}$) at fixed stellar mass. However, when we include thegas in the disk, bulge-dominated galaxies have the highest {\em total} diskspecific angular momentum ($j_{\rm total, disk}$). We attribute this to a largecontribution from an extended disk of cold gas in typical bulge-dominatedgalaxies. We find the relationship between $j_{\rm dark matter}$ and morphologyto be quite complex. Surprisingly, in this stellar mass range, not only dobulge-dominated galaxies tend to live in halos with higher $j_{\rm darkmatter}$ than disk-dominated galaxies, but intermediate galaxies (those withroughly equal fractions of bulge and disk mass) have the lowest $j_{\rm darkmatter}$ of all. Yet, when controlling for halo mass, rather than stellar mass,the relationship between $j_{\rm dark matter}$ and morphology vanishes. Basedon these results, halo mass rather than angular momentum is the main driver ofthe predicted morphology sequence at high masses. In fact, in our stellar massrange, disk-dominated galaxies live in dark matter halos that are roughly1/10th the mass of their bulge-dominated counterparts.

Angular momentum and morphological sequence of massive galaxies through Dark Sage