The SAMI Galaxy Survey: stellar population and structural trends across
  the Fundamental Plane
  We study the Fundamental Plane (FP) for a volume- and luminosity-limited
sample of 560 early-type galaxies from the SAMI survey. Using r-band sizes and
luminosities from new Multi-Gaussian Expansion (MGE) photometric measurements,
and treating luminosity as the dependent variable, the FP has coefficients
a=1.294$\pm$0.039, b= 0.912$\pm$0.025, and zero-point c= 7.067$\pm$0.078. We
leverage the high signal-to-noise of SAMI integral field spectroscopy, to
determine how structural and stellar-population observables affect the scatter
about the FP. The FP residuals correlate most strongly (8$\sigma$ significance)
with luminosity-weighted simple-stellar-population (SSP) age. In contrast, the
structural observables surface mass density, rotation-to-dispersion ratio,
S\'ersic index and projected shape all show little or no significant
correlation. We connect the FP residuals to the empirical relation between age
(or stellar mass-to-light ratio $\Upsilon_\star$) and surface mass density, the
best predictor of SSP age amongst parameters based on FP observables. We show
that the FP residuals (anti-)correlate with the residuals of the relation
between surface density and $\Upsilon_\star$. This correlation implies that
part of the FP scatter is due to the broad age and $\Upsilon_\star$
distribution at any given surface mass density. Using virial mass and
$\Upsilon_\star$ we construct a simulated FP and compare it to the observed FP.
We find that, while the empirical relations between observed stellar population
relations and FP observables are responsible for most (75%) of the FP scatter,
on their own they do not explain the observed tilt of the FP away from the
virial plane.
