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

Abstract

We present dynamical scaling relations, combined with the stellar population properties, for a subsample of about 6000 nearby galaxies with the most reliable dynamical models extracted from the full MaNGA sample of 10K galaxies. We show that the inclination-corrected mass plane (MP) for both early-type galaxies (ETGs) and late-type galaxies (LTGs), which links dynamical mass, projected half-light radius $R_{\mathrm{e}}$, and the second stellar velocity moment ${\sigma }_{\mathrm{e}}$ within $R_{\mathrm{e}}$, satisfies the virial theorem and is even tighter than the uncorrected one. We find a clear parabolic relation between $\lg (M/L{)}_{\mathrm{e}}$, the total mass-to-light ratio within a sphere of radius $R_{\mathrm{e}}$, and $\lg {\sigma }_{\mathrm{e}}$, with the $M/L$ increasing with ${\sigma }_{\mathrm{e}}$ and for older stellar populations. However, the relation for ETGs is linear and the one for the youngest galaxies is constant. We confirm and improve the relation between average logarithmic total density slopes $\overline{{\gamma }_{\mathrm{T}}}$ and ${\sigma }_{\mathrm{e}}$: $\overline{{\gamma }_{\mathrm{T}}}$ become steeper with increasing ${\sigma }_{\mathrm{e}}$ until $\lg ({\sigma }_{\mathrm{e}}/\mathrm{km}{\mathrm{s}}^{-1})\approx 2.2$ and then remain constant around $\overline{{\gamma }_{\mathrm{T}}}\approx -2.2$. The $\overline{{\gamma }_{\mathrm{T}}}-{\sigma }_{\mathrm{e}}$ variation is larger for LTGs than ETGs. At fixed ${\sigma }_{\mathrm{e}}$ the total density profiles steepen with galaxy age and for ETGs. We find generally low dark matter fractions, median $f_{\mathrm{DM}}(<R_{\mathrm{e}})=8$ per cent, within a sphere of radius $R_{\mathrm{e}}$. However, we find that $f_{\mathrm{DM}}(<R_{\mathrm{e}})$ depends on ${\sigma }_{\mathrm{e}}$ better than stellar mass: dark matter increases to a median $f_{\mathrm{DM}}(<R_{\mathrm{e}})=33$ percent for galaxies with ${\sigma }_{\mathrm{e}}\lesssim 100\mathrm{km}{\mathrm{s}}^{-1}$. The increased $f_{\mathrm{DM}}(<R_{\mathrm{e}})$ at low ${\sigma }_{\mathrm{e}}$ explains the parabolic $\lg (M/L{)}_{\mathrm{e}}-\lg {\sigma }_{\mathrm{e}}$ relation.

arXiv comment26 pages, 21 figures, 1 table; Accepted by MNRAS

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