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It is generally assumed that galaxies are a bimodal population in both starformation and structure: star-forming galaxies are disks, while passivegalaxies host large bulges or are entirely spheroidal. Here, we test thisscenario by presenting a full census of the kinematic morphologies of avolume-limited sample of galaxies in the local Universe extracted from theMaNGA galaxy survey. We measure the integrated stellar line-of-sight velocityto velocity dispersion ratio ($V/\sigma$) for 4574 galaxies in the stellar massrange $9.75 < \log M_{\star}[\rm{M}_{\odot}] < 11.75$. We show that at fixedstellar mass, the distribution of $V/\sigma$ is not bimodal, and that a simpleseparation between fast and slow rotators is over-simplistic. Fast rotators area mixture of at least two populations, referred to here as dynamically-colddisks and intermediate systems, with disks dominating in both total stellarmass and number. When considering star-forming and passive galaxies separately,the star-forming population is almost entirely made up of disks, while thepassive population is mixed, implying an array of quenching mechanisms. Passivedisks represent $\sim$30% (both in number and mass) of passive galaxies, nearlya factor of two higher than that of slow rotators, reiterating that these arean important population for understanding galaxy quenching. These results painta picture of a local Universe dominated by disky galaxies, most of which becomesomewhat less rotation-supported upon or after quenching. While spheroids arepresent to a degree, they are certainly not the evolutionary end-point for themajority of galaxies.

Beyond galaxy bimodality: the complex interplay between kinematic morphology and star formation in the local Universe