  We have measured gas and stellar velocity dispersions in 5 circumnuclear
starforming regions (CNSFRs) and the nucleus of the barred spiral galaxy NGC
3351. The stellar dispersions have been obtained from high resolution spectra
of the CaT lines at $\lambda\lambda$ 8494, 8542, 8662 \AA, while the gas
velocity dispersions have been measured by Gaussian fits to the H$\beta$
$\lambda$ 4861 \AA line on high dispersion spectra.
  The CNSFRs, with sizes of about 100 to 150 pc in diameter, are seen to be
composed of several individual star clusters with sizes between 1.7 and 4.9 pc
on an HST image. Using the stellar velocity dispersions, we have derived
dynamical masses for the entire starforming complexes and for the individual
star clusters. Values of the stellar velocity dispersions are between 39 and 67
km s$^{-1}$. Dynamical masses for the whole CNSFRs are between 4.9 $\times$
10$^6$ and 4.3 $\times$ 10$^7$ M$_\odot$ and between 1.8 and 8.7 $\times$
10$^6$ M$_\odot$ for the individual star clusters.
  Stellar and gas velocity dispersions are found to differ by about 20 km
s$^{-1}$ with the H$\beta$ lines being narrower than both the stellar lines and
the [O{\sc iii}] $\lambda$ 5007 \AA lines. We have found indications for the
presence of two different kinematical components in the ionised gas of the
regions. The radial velocity curve shows deviation from circular motions for
the ionised hydrogen consistent with its infall towards the central regions of
the galaxy at a velocity of about 25 km s$^{-1}$. To disentangle the origin of
these two components it will be necessary to map these regions with high
spectral and spatial resolution and much better S/N in particular for the
O$^{2+}$ lines.
