Newtonian acceleration scales in spiral galaxies
  We revisit the issue of the constancy of the dark matter (DM) and baryonic
Newtonian acceleration scales within the DM scale radius by considering a large
sample of late - type galaxies. We rely on a Markov Chain Monte Carlo (MCMC)
method to estimate the parameters of the halo model and the stellar mass - to -
light ratio and then propagate the uncertainties from the rotation curve data
to the estimate of the acceleration scales. This procedure allows us to compile
a catalog of 58 objects with estimated values of the $B$ band absolute
magnitude $M_B$, the virial mass $M_{vir}$, the DM and baryonic Newtonian
accelerations (denoted as $g_{DM}(r_0)$ and $g_{bar}(r_0)$, respectively)
within the scale radius $r_0$ which we use to investigate whether it is
possible to define a universal acceleration scale. We find a weak but
statistically meaningful correlation with $M_{vir}$ thus making us argue
against the universality of the acceleration scales. However, the results
somewhat depend on the sample adopted so that a careful analysis of selection
effects should be carried out before any definitive conclusion can be drawn.
