We study the relation between the properties of the bulge/disc components and the H I mass fraction of galaxies. We find that at fixed stellar mass, disc colours are correlated with the H I mass fraction, while bulge colours are not. The lack of a correlation between the bulge colour and the H I mass fraction is regardless whether the bulges are pseudo, or whether the galaxies host bars or are interacting with a neighbour. There is no strong correlation between the colours of the discs and bulges either. These results suggest that the current total amount of H I is closely related to the formation of discs, but does not necessarily fuel the formation of (pseudo) bulges in an efficient way. We do not find evidence for the star formation in the discs to be quenched by the bulges.