  We study the spatially-resolved stellar specific angular momentum $j_*$ in a
high-quality sample of 24 CALIFA galaxies covering a broad range of visual
morphology, accounting for stellar velocity and velocity dispersion. The shape
of the spaxel-wise probability density function of normalised
$s=j_*/j_{*mean}$, PDF($s$), deviates significantly from the near-universal
initial distribution expected of baryons in a dark matter halo and can be
explained by the expected baryonic effects in galaxy formation that remove and
redistribute angular momentum. Further we find that the observed shape of the
PDF($s$) correlates significantly with photometric morphology, where late-type
galaxies have PDF($s$) that is similar to a normal distribution, whereas early
types have a strongly-skewed PDF($s$) resulting from an excess of low-angular
momentum material. Galaxies that are known to host pseudobulges (bulge Sersic
index $n_b <2.2$) tend to have less skewed bulge PDF($s$), with skewness
$(b_{1rb})\lesssim0.8$. The PDF($s$) encodes both kinematic and photometric
information and appears to be a robust tracer of morphology. Its use is
motivated by the desire to move away from traditional component-based
classifications which are subject to observer bias, to classification on a
galaxy's fundamental (stellar mass, angular momentum) properties. In future,
PDF($s$) may also be useful as a kinematic decomposition tool.
