  Empirical correlations connecting starlight to galaxy dynamics (e.g., the
fundamental plane (FP) of elliptical/quiescent galaxies and the Tully--Fisher
relation of spiral/star-forming galaxies) provide cosmology-independent
distance estimation and are central to local Universe cosmology. In this work,
we introduce the mass hyperplane (MH), which is the stellar-to-dynamical mass
relation $(M_\star/M_\mathrm{dyn})$ recast as a linear distance indicator.
Building on recent FP studies, we show that both star-forming and quiescent
galaxies follow the same empirical MH, then use this to measure the peculiar
velocities (PVs) for a sample of 2496 galaxies at $z<0.12$ from GAMA. The
limiting precision of MH-derived distance/PV estimates is set by the intrinsic
scatter in size, which we find to be $\approx$0.1~dex for both quiescent and
star-forming galaxies (when modeled independently) and $\approx$0.11~dex when
all galaxies are modeled together; showing that the MH is as good as the FP. To
empirically validate our framework and distance/PV estimates, we compare the
inferred distances to groups as derived using either quiescent or star-forming
galaxies. A good agreement is obtained with no discernible bias or offset,
having a scatter of $\approx$0.05~dex $\approx$12\% in distance. Further, we
compare our PV measurements for the quiescent galaxies to the previous PV
measurements of the galaxies in common between GAMA and the Sloan Digital Sky
Survey (SDSS), which shows similarly good agreement. Finally, we provide
comparisons of PV measurements made with the FP and the MH, then discuss
possible improvements in the context of upcoming surveys such as the 4MOST
Hemisphere Survey (4HS).
