  We present a detailed study of the stellar mass vs. specific angular momentum
(AM) relation (Fall relation) for a representative sample of 564 nearby
galaxies in the eXtended GALEX Arecibo SDSS Survey (xGASS). We focus on the
dependence of the Fall relation's slope on galaxy type and the galaxy
properties regulating its scatter. Stellar specific AM is determined by
combining single-dish H{\sc i} velocity widths and stellar mass profiles for
all H{\sc i} detections in the xGASS sample. At fixed morphology (or
bulge-to-total ratio), we find that the power law slope of the Fall relation is
consistent with 2/3. However, when all galaxy types are combined, we recover a
much shallower slope of $\sim$0.47. We show that this is a consequence of the
change in galaxy morphology as a function of mass, highlighting that caution
should be taken when using the slope of the Fall relation to constrain galaxy
formation models without taking sample selection into account. We quantify the
Fall relations scatter and show that H{\sc i} gas fraction is the strongest
correlated parameter for low stellar masses (Spearman correlation: $\rho_{s} =
0.61$), while the bulge-to-total ratio becomes slightly more dominant at higher
masses ($\rho_{s} = -0.29$). Intriguingly, when only the disc components of
galaxies are considered, H{\sc i} gas fraction remains the strongest correlated
parameter with the scatter of the relation (regardless of disc stellar mass).
Our work provides one of the best characterisations of the Fall relation for a
representative sample of galaxies in the local Universe.
