Revisiting the stellar mass -- angular momentum -- morphology relation:
  extension to higher bulge fraction, and the effect of bulge type
  We present the relation between stellar specific angular momentum $j_*$,
stellar mass $M_*$, and bulge-to-total light ratio $\beta$ for THINGS, CALIFA
and Romanowsky \& Fall datasets, exploring the existence of a fundamental plane
between these parameters as first suggested by Obreschkow \& Glazebrook. Our
best-fit $M_*-j_*$ relation yields a slope of $\alpha = 1.03 \pm 0.11$ with a
trivariate fit including $\beta$. When ignoring the effect of $\beta$, the
exponent $\alpha = 0.56 \pm 0.06$ is consistent with $\alpha = 2/3$ predicted
for dark matter halos. There is a linear $\beta - j_*/M_*$ relation for $\beta
\lesssim 0.4$, exhibiting a general trend of increasing $\beta$ with decreasing
$j_*/M_*$. Galaxies with $\beta \gtrsim 0.4$ have higher $j_*$ than predicted
by the relation. Pseudobulge galaxies have preferentially lower $\beta$ for a
given $j_*/M_*$ than galaxies that contain classical bulges. Pseudobulge
galaxies follow a well-defined track in $\beta - j_*/M_*$ space, consistent
with Obreschkow \& Glazebrook, while galaxies with classical bulges do not.
These results are consistent with the hypothesis that while growth in either
bulge type is linked to a decrease in $j_*/M_*$, the mechanisms that build
pseudobulges seem to be less efficient at increasing bulge mass per decrease in
specific angular momentum than those that build classical bulges.
