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

xGASS: characterizing the slope and scatter of the stellar mass - angular momentum relation for nearby galaxies