  We present a comprehensive test of the relation between stellar and total
mass in galaxies as predicted by popular models based on abundance matching
(AM) techniques. We use the ``Spectroscopy and H-band Imaging of Virgo cluster
galaxies'' (SHIVir) survey with photometric and dynamical profiles for 190
Virgo cluster galaxies to establish a relation between the stellar and
dynamical masses measured within the isophotal radius $r_{23.5}$. Various dark
matter and galaxy scaling relations are combined with results from the NIHAO
suite of hydrodynamical simulations to recast AM predictions in terms of these
observed quantities. Our results are quite insensitive to the exact choice of
dark matter profile and halo response to baryon collapse. We find that
theoretical models reproduce the slope and normalization of the observed
stellar-to-halo mass relation (SHMR) over more than three orders of magnitude
in stellar mass $(10^8 < M_*/M_{\odot} < 2 \times 10^{11})$. However, the
scatter of the observed SHMR exceeds that of AM predictions by a factor
$\sim$5. For systems with stellar masses exceeding $5 \times
10^{10}~M_{\odot}$, AM overpredicts the observed stellar masses for a given
dynamical mass. The latter offset may support previous indications of a
different stellar initial mass function in these massive galaxies. Overall our
results support the validity of AM predictions on a wide dynamical range.
