Dynamical signatures of a LCDM-halo and the distribution of the baryons
  in M33
  We map the neutral atomic gas content of M33 using high resolution VLA and
GBT observations and fit a tilted ring model to determine the orientation of
the extended gaseous disk and its rotation curve. The disk of M33 warps from 8
kpc outwards without substantial change of its inclination with respect to the
line of sight. Rotational velocities rise steeply with radius in the inner
disk, reaching 100 km/s in 4 kpc, then the rotation curve becomes more
perturbed and flatter with velocities as high as 120-130 km/s out to 23 kpc. We
derive the stellar mass surface density map of M33's optical disk, via pixel
-SED fitting methods based on population synthesis models, which highlights
variations in the mass-to-light ratio. The stellar mass surface further out is
estimated from deep images of outer disk fields. Stellar and gas maps are then
used in the dynamical analysis of the rotation curve to constrain the dark
matter distribution which is relevant at all radii. A dark matter halo with a
Navarro-Frenk-White density profile in a LCDM cosmology, provides the best fit
to the rotation curve for a dark halo concentration C=10 and a total halo mass
of 4.3 10^{11}Msun. This imples a baryonic fraction of order 0.02 and the
evolutionary history of this galaxy should account for loss of a large fraction
of its original baryonic content.
