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We use a combination of data from the MaNGA survey and MaNGA-likeobservations in IllustrisTNG100 to determine the prevalence of misalignmentbetween the rotational axes of stars and gas. This census paper outlines thetypical characteristics of misaligned galaxies in both observations andsimulations to determine their fundamental relationship with morphology andangular momentum. We present a sample of ~4500 galaxies from MaNGA withkinematic classifications which we use to demonstrate that the prevalence ofmisalignment is strongly dependent on morphology. The misaligned fractionsharply increases going to earlier morphologies (28$\pm$3% of 301 early-typegalaxies, 10$\pm$1% of 677 lenticulars and 5.4$\pm$0.6% of 1634 pure late-typegalaxies). For early-types, aligned galaxies are less massive than themisaligned sample whereas this trend reverses for lenticulars and purelate-types. We also find that decoupling depends on group membership forearly-types with centrals more likely to be decoupled than satellites. Wedemonstrate that misaligned galaxies have similar stellar angular momentum togalaxies without gas rotation, much lower than aligned galaxies. Misalignedgalaxies also have a lower gas mass than the aligned, indicative that gas lossis a crucial step in decoupling star-gas rotation. Through comparison to a mockMaNGA sample, we find that the strong trends with morphology and angularmomentum hold true in IllustrisTNG100. We demonstrate that the lowered angularmomentum is, however, not a transient property and that the likelihood ofstar-gas misalignment at z = 0 is correlated with the spin of the dark matterhalo going back to z = 1.

Decoupling the rotation of stars and gas -- I: the relationship with morphology and halo spin