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We present dynamical scaling relations, combined with the stellar populationproperties, for a subsample of about 6000 nearby galaxies with the mostreliable dynamical models extracted from the full MaNGA sample of 10K galaxies.We show that the inclination-corrected mass plane (MP) for both early-typegalaxies (ETGs) and late-type galaxies (LTGs), which links dynamical mass,projected half-light radius $R_{\rm e}$, and the second stellar velocity moment$\sigma_{\rm e}$ within $R_{\rm e}$, satisfies the virial theorem and is eventighter than the uncorrected one. We find a clear parabolic relation between$\lg(M/L)_{\rm e}$, the total mass-to-light ratio within a sphere of radius$R_{\rm e}$, and $\lg\sigma_{\rm e}$, with the $M/L$ increasing with$\sigma_{\rm e}$ and for older stellar populations. However, the relation forETGs is linear and the one for the youngest galaxies is constant. We confirmand improve the relation between average logarithmic total density slopes$\overline{\gamma_{\rm T}}$ and $\sigma_{\rm e}$: $\overline{\gamma_{\rm T}}$become steeper with increasing $\sigma_{\rm e}$ until $\lg(\sigma_{\rm e}/{\rmkm\,s^{-1}})\approx 2.2$ and then remain constant around $\overline{\gamma_{\rmT}}\approx -2.2$. The $\overline{\gamma_{\rm T}}-\sigma_{\rm e}$ variation islarger for LTGs than ETGs. At fixed $\sigma_{\rm e}$ the total density profilessteepen with galaxy age and for ETGs. We find generally low dark matterfractions, median $f_{\rm DM}(<R_{\rm e})=8$ per cent, within a sphere ofradius $R_{\rm e}$. However, we find that $f_{\rm DM}(<R_{\rm e})$ depends on$\sigma_{\rm e}$ better than stellar mass: dark matter increases to a median$f_{\rm DM}(<R_{\rm e})=33$ percent for galaxies with $\sigma_{\rme}\lesssim100{\rm km\,s^{-1}}$. The increased $f_{\rm DM}(<R_{\rm e})$ at low$\sigma_{\rm e}$ explains the parabolic $\lg(M/L)_{\rm e}-\lg\sigma_{\rm e}$relation.

monthly notices of the royal astronomical society

MaNGA DynPop -- III. Stellar dynamics versus stellar population  relations in 6000 early-type and spiral galaxies: Fundamental Plane,  mass-to-light ratios, total density slopes, and dark matter fractions