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The stellar mass Tully-Fisher relation (STFR) and its scatter encode valuableinformation about the processes shaping galaxy evolution across cosmic time.However, we are still missing a proper quantification of the STFR slope andscatter dependence on the baryonic tracer used to quantify rotational velocity,on the velocity measurement radius and on galaxy integrated properties. Wepresent a catalogue of stellar and ionised gas (traced by H$\alpha$ emission)kinematic measurements for a sample of galaxies drawn from the MaNGA GalaxySurvey, providing an ideal tool for galaxy formation model calibration and forcomparison with high-redshift studies. We compute the STFRs for stellar and gasrotation at 1, 1.3 and 2 effective radii ($R_e$). The relations for bothbaryonic 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 areconsistent. When accounting for covariances with integrated v/$\sigma$, scatterin the stellar and gas STFRs shows no strong correlation with: opticalmorphology, star formation rate surface density, tidal interaction strength orgas accretion signatures. Our results suggest that the STFR scatter is drivenby an increase in stellar/gas dispersional support, from either external(mergers) or internal (feedback) processes. No correlation between STFR scatterand environment is found. Nearby Universe galaxies have their stars and gas instatistically 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.

The Tully-Fisher relation from SDSS-MaNGA: Physical causes of scatter and variation at different radii