Atomic and molecular gas scaling ratios. In all figures, the early, ongoing, and advanced pre-processing categories are shown as blue circles, green squares, and red diamonds, respectively and H₂ upper limits are depicted by arrows. Solid markers indicate H I detections and open markers are non-detections. FCC 40 is not assigned to any pre-processing category and is shown as the open black star. Top left panel: H I gas fraction compared to galaxies from the HRS (Boselli et al. 2010, 2014) and VGS (Kreckel et al. 2012) (grey points) that show the typical scatter in F_HI. The orange shaded region indicates the median trend from xGASS (Catinella et al. 2018). Top right panel: total gas fraction of our galaxies compared to the median xGASS-CO trend (Catinella et al. 2018) (orange shaded region). Bottom left panel: molecular-to-atomic-gas ratio of our galaxies compared to the median xGASS-CO trend (Catinella et al. 2018) (orange shaded region). Bottom right panel: H₂ gas fraction as a function of H I gas fraction, showing constant ratios of 100%, 30%, 10%, and 3%. Overall, the galaxies in the early category are H I rich, the galaxies in the ongoing category typically follow the xGASS and xGASS-CO median scaling relations (Catinella et al. 2018), while galaxies in the advanced category have no H I or are H I-deficient with irregularly high H₂-to-H I ratios.