  For the intermediate-type barred galaxy NGC2336 stationary models are
constructed which reproduce in a consistent manner the observed distribution of
the luminous matter and the observed gas kinematics in those regions affected
by the bar. We present 2D fits to the observed NIR-band luminosity distribution
that consist of three components: a bulge, a bar, and a disk. The brightness
distribution of each component is converted into an underlying mass
distribution by means of a suitable M/L-conversion. The resulting coadded
potential of NGC2336 is implemented into a numerical code for the computation
of closed orbits for gas clouds (HII-gas). Using the resulting tracks, the
phase space accessible to the models is examined with regard to the main orbit
families. For different orbit energies complete sets of closed orbits are
computed. By projection to the reference frame of the galaxy, artificial
rotation curves for every model are obtained and are compared with the observed
rotation curves of the HII-gas. In an iterative procedure, the parameters of
the NGC2336-models are optimized by computing and evaluating a large number of
parameters. The result is a final model that reproduces the morphological
structure of NGC2336 as well as the observed kinematics of the HII-gas. The
parameter values from the morphological decomposition and those needed to fit
the HII-rotation curves best are in exellent agreement. The effects of changing
single parameter values and possible error sources are discussed in detail. It
turns out that the kinematics of the warm HII-gas of NGC2336 can be explained
without considering hydrodynamic effects, even in the central regions.
