Late-type galaxies morpho-kinematic class

Each galaxy in our sample is classified into one of the five new morpho-kinematic categories proposed in this study: j*- ring, j*- spiral, j*- bar, j*- clump and j*- irregular. These classes are named after the predominant galactic substructure of their stellar sAMSD map and form a new classification scheme that combines both morphological characteristics and dynamic properties. For 14 galaxies, the morphological classification does not coincide with the corresponding morpho-kinematic category.

As expected, there is a high correlation between j* and M* for our sample. Similarly, our galaxies exhibit a correlation between j* and their star formation rate, and between j* and their total mass. The mean j* and M* are distributed along different regions along the Fall relation for all j*- types, although there is a considerable scatter within each type.

There is a link between the two-dimensional distribution of stellar sAMSD and j*. The location of the different j*- types in the j*-M* diagram could indicate a morpho-kinematic evolution of late-type galaxies within the hierarchical paradigm of galaxy formation. The physical mechanisms capable of modifying the shape of galaxies in the stellar sAMSD space seem to be related with the stability of the galactic disc.

The spatial redistribution of angular momentum for low-mass late-type galaxies may be driven by a combination of feedback, dynamical friction, shock waves and resonances, while the quasi-stationary rotating density wave can be responsible for the aforementioned process in the massive spirals.