Abstract

We use the stellar kinematics for 2458 galaxies from the MaNGA survey to explore a universal fundamental plane (UFP) described by the equation log(ϒe) = log(S0.52) log(Ie) log(Re) +C, defined by the logarithms of effective radius, R e; the surface brightness within Re, I e; the dynamical mass-to-light ratio within R e, Y e; and the total velocity parameter at R e, SK2 = KVRe2 + σ∗;e2, where VRe is the rotation velocity and σ∗e is the velocity dispersion. The surface brightness is within R e, I e, and the dynamical mass-to-light ratio is within R e, ϒe. We use sophisticated Schwarzschild dynamical models for a subsample of 300 galaxies from the CALIFA survey to calibrate the universal fundamental plane. This calibration allows us to propose both (i) a parameterization to estimate the difficult-to-measure averaged dynamical mass-to-light ratio within Re, ϒefit, once the internal kinematics, surface brightness, and effective radius are known; and (ii) a new, more robust dynamical mass proxy consistent with dynamical models within 0.09 dex. We reproduce the relation between the dynamical mass and the stellar mass in the inner regions of galaxies with lower scatter. We use the estimated ϒefit from our analysis to explore the UFP with the MaNGA data set. We find that all galaxies, from spheroids to disks, follow the UFP with a scatter significantly smaller (0.05 dex) than the one reported for the fundamental plane (∼0.09 dex) and comparable with Tully-Fisher studies (∼0.05 dex), but for a wider range of galaxy types. We also confirm that spheroidal and spiral galaxies follow the same M ∗-S 0.5 scaling relation, with lower scatter than the M∗ - VRe and M∗ - σ∗e ones, which is in agreement with previous studies found in the literature.