  The stellar mass Tully-Fisher relation (STFR) and its scatter encode valuable
information about the processes shaping galaxy evolution across cosmic time.
However, we are still missing a proper quantification of the STFR slope and
scatter dependence on the baryonic tracer used to quantify rotational velocity,
on the velocity measurement radius and on galaxy integrated properties. We
present a catalogue of stellar and ionised gas (traced by H$\alpha$ emission)
kinematic measurements for a sample of galaxies drawn from the MaNGA Galaxy
Survey, providing an ideal tool for galaxy formation model calibration and for
comparison with high-redshift studies. We compute the STFRs for stellar and gas
rotation at 1, 1.3 and 2 effective radii ($R_e$). The relations for both
baryonic components become shallower at 2$R_e$ compared to 1$R_e$ and 1.3$R_e$.
We report a steeper STFR for the stars in the inner parts ($\leq 1.3 R_e$)
compared to the gas. At 2$R_e$, the relations for the two components are
consistent. When accounting for covariances with integrated v/$\sigma$, scatter
in the stellar and gas STFRs shows no strong correlation with: optical
morphology, star formation rate surface density, tidal interaction strength or
gas accretion signatures. Our results suggest that the STFR scatter is driven
by an increase in stellar/gas dispersional support, from either external
(mergers) or internal (feedback) processes. No correlation between STFR scatter
and environment is found. Nearby Universe galaxies have their stars and gas in
statistically different states of dynamical equilibrium in the inner parts
($\leq 1.3 R_e$), while at 2$R_{e}$ the two components are dynamically coupled.
