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We use HI and H2 global gas measurements of galaxies from xGASS and xCOLDGASS to investigate quenching paths of galaxies below the star formation mainsequence (SFMS). We show that the population of galaxies below the SFMS is nota 1:1 match with the population of galaxies below the HI and H2 gas fractionscaling relations. Some galaxies in the transition zone (TZ) 1-sigma below theSFMS can be as HI-rich as those in the SFMS, and have on average longer gasdepletion timescales. We find evidence for environmental quenching ofsatellites, but central galaxies in the TZ defy simple quenching pathways. Someof these so-called "quenched" galaxies may still have significant gasreservoirs and be unlikely to deplete them anytime soon. As such, a correctmodel of galaxy quenching cannot be inferred with SFR (or other opticalobservables) alone, but must include observations of the cold gas. We also findthat internal structure (particularly, the spatial distribution of old andyoung stellar populations) plays a significant role in regulating the starformation of gas-rich isolated TZ galaxies, suggesting the importance of bulgesin their evolution.

xGASS: Cold gas content and quenching in galaxies below the star forming main sequence