  From a purely photometric perspective galaxies are generally decomposed into
a bulge+disc system, with bulges being dispersion-dominated and discs
rotationally-supported. However, recent observations have demonstrated that
such a framework oversimplifies complexity, especially if one considers galaxy
kinematics. To address this issue we introduced with the GPU-based code
\textsc{bang} a novel approach that employs analytical potential-density pairs
as galactic components, allowing for a computationally fast, still reliable fit
of the morphological and kinematic properties of galaxies. Here we apply
\textsc{bang} to the SDSS-MaNGA survey, estimating key parameters such as mass,
radial extensions, and dynamics, for both bulges and discs of +10,000 objects.
We test our methodology against a smaller subsample of galaxies independently
analysed with an orbit-based algorithm, finding agreement in the recovered
total stellar mass. We also manage to reproduce well-established scaling
relations, demonstrating how proper dynamical modelling can result in tighter
correlations and provide corrections to standard approaches. Finally, we
propose a more general way of decomposing galaxies into "hot" and "cold"
components, showing a correlation with orbit-based approaches and visually
determined morphological type. Unexpected tails in the "hot-to-total"
mass-ratio distribution are present for galaxies of all morphologies, possibly
due to visual morphology misclassifications.
