  We build templates of rotation curves as a function of the $I-$band
luminosity via the mass modeling (by the sum of a thin exponential disk and a
cored halo profile) of suitably normalized, stacked data from wide samples of
local spiral galaxies. We then exploit such templates to determine fundamental
stellar and halo properties for a sample of about $550$ local disk-dominated
galaxies with high-quality measurements of the optical radius $R_{\rm opt}$ and
of the corresponding rotation velocity $V_{\rm opt}$. Specifically, we
determine the stellar $M_\star$ and halo $M_{\rm H}$ masses, the halo size
$R_{\rm H}$ and velocity scale ${V_{\rm H}}$, and the specific angular momenta
of the stellar $j_\star$ and dark matter $j_{\rm H}$ components. We derive
global scaling relationships involving such stellar and halo properties both
for the individual galaxies in our sample and for their mean within bins; the
latter are found to be in pleasing agreement with previous determinations by
independent methods (e.g., abundance matching techniques, weak lensing
observations, and individual rotation curve modeling). Remarkably, the size of
our sample and the robustness of our statistical approach allow us to attain an
unprecedented level of precision over an extended range of mass and velocity
scales, with $1\sigma$ dispersion around the mean relationships of less than
$0.1$ dex. We thus set new standard local relationships that must be reproduced
by detailed physical models, that offer a basis for improving the sub-grid
recipes in numerical simulations, that provide a benchmark to gauge independent
observations and check for systematics, and that constitute a basic step toward
the future exploitation of the spiral galaxy population as a cosmological
probe.
