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We try to understand the trends in the mass density slopes as a function ofgalaxy properties. We use the results from the best Jeans Anisotropic Modelling(JAM) of the integral-field stellar kinematics for near 6000 galaxies from theMaNGA DynPop project, with stellar masses of $10^{9-12}\ {\rm M_{\odot}}$,including both early-type and late-type galaxies. We use the mass-weighteddensity slopes for the stellar $\overline{\gamma}_*$, dark$\overline{\gamma}_{\rm DM}$, and total $\overline{\gamma}_{\rm T}$ mass fromZhu et al. (2023b). The $\overline{\gamma}_{\rm T}$ approaches a constant valueof 2.2 for high $\sigma_{\rm e}$ galaxies, and flattens for lg$(\sigma_{\rme}/{\rm km\ s^{-1}})\lesssim2.3$, reaching 1.5 for lg$(\sigma_{\rm e}/{\rm km\s^{-1}})\approx1.8$. The total and stellar slopes track each other tightly,with $\overline{\gamma}_{\rm T}\approx\overline{\gamma}_*-0.174$ over the full$\sigma_{\rm e}$ range. This confirms the dominance of stellar matter within$R_{\rm e}$. We also show that there is no perfect conspiracy between baryonicand dark matter, as $\overline{\gamma}_*$ and $\overline{\gamma}_{\rm DM}$ donot vary inversely within the $\sigma_{\rm e}$ range. We find that the centralgalaxies from TNG50 and TNG100 simulations do not reproduce the observed galaxymass distribution, which we attribute to the overestimated dark matterfraction, possibly due to a constant IMF and excessive adiabatic contractioneffects in the simulations. Finally, we present the stacked dark matter densityprofiles and show that they are slightly steeper than the pure dark mattersimulation prediction of $\overline{\gamma}_{\rm DM}\approx1$, suggestingmoderate adiabatic contraction in the central region of galaxies. Our workdemonstrate the power of stellar dynamics modelling for probing the interactionbetween stellar and dark matter and testing galaxy formation theories.

MaNGA DynPop -- VI. Matter density slopes from dynamical models of 6000  galaxies vs cosmological simulations: the interplay between baryonic and dark  matter