Mass models of disk galaxies from the DiskMass Survey in MOND
  This article explores the agreement between the predictions of Modified
Newtonian Dynamics (MOND) and the rotation curves and stellar velocity
dispersion profiles measured by the DiskMass Survey. A bulge-disk decomposition
was made for each of the thirty published galaxies, and a MOND Poisson solver
was used to simultaneously compute, from the baryonic mass distributions, model
rotation curves and vertical velocity dispersion profiles, which were compared
to the measured values. The two main free parameters, the stellar disk's
mass-to-light ratio ($M/L$) and its exponential scale-height ($h_z$), were
estimated by Markov Chain Monte Carlo modelling. The average best-fit K-band
stellar mass-to-light ratio was $M/L \simeq 0.55 \pm 0.15$. However, to match
the DiskMass Survey data, the vertical scale-heights would have to be in the
range $h_z=200$ to $400$ pc which is a factor of two lower than those derived
from observations of edge-on galaxies with a similar scale-length. The reason
is that modified gravity versions of MOND characteristically require a larger
$M/L$ to fit the rotation curve in the absence of dark matter and therefore
predict a stronger vertical gravitational field than Newtonian models. It was
found that changing the MOND acceleration parameter, the shape of the velocity
dispersion ellipsoid, the adopted vertical distribution of stars, as well as
the galaxy inclination, within any realistic range, all had little impact on
these results.
