  We use a sample of 559 disc galaxies extracted from the eXtended GALEX
Arecibo SDSS Survey (xGASS) to study the connection between baryonic angular
momentum, mass and atomic gas fraction in the local Universe. Baryonic angular
momenta are determined by combining HI and H$_{2}$ integrated profiles with
two-dimensional stellar mass surface density profiles. In line with previous
work, we confirm that specific angular momentum and atomic gas fraction are
tightly correlated, but we find a larger scatter than previously observed. This
is most likely due to the wider range of galaxy properties covered by our
sample. We compare our findings with the predictions of the analytical
stability model developed by Obreschkow et al. and find that, while the model
provides a very good first-order approximation for the connection between
baryonic angular momentum, mass and gas fraction, it does not fully match our
data. Specifically, we find that at fixed baryonic mass, the dependence of
specific angular momentum on gas fraction is significantly weaker, and at fixed
gas fraction, the slope of the angular momentum vs. mass relation is shallower
than what was predicted by the model. The reasons behind this tension remain
unclear, but we speculate that multiple factors may simultaneously play a role,
all related to the fact that the model is not able to encapsulate the full
diversity of galaxy properties in our sample.
