Mass distribution and kinematics of the barred galaxy NGC 2336

For the intermediate-type barred galaxy NGC 2336 stationary models are cons tructed which reproduce in a consistent manner the observed distribution of the luminous matter and the observed gas kinematics in those regions affec ted by the bar. We present 2D fits to the observed NIR-band luminosity dist ribution that consist of three components: a bulge, a bar, and a disk. The brightness distribution of each component is converted into an underlying m ass distribution by means of a suitable M/L-conversion. The resulting coadd ed potential of NGC 2336 is implemented into a numerical code for the compu tation of closed orbits for gas clouds (HII-gas). Using the resulting track s, the phase space accessible to the models is examined with regard to the main orbit families. For different orbit energies complete sets of closed o rbits are computed. By projection to the reference frame of the galaxy, art ificial 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 NGC 2336-models are optimi zed by computing and evaluating a large number of parameters. The result is a final model that reproduces the morphological structure of NGC 2336 as w ell as the observed kinematics of the HII-gas. The parameter values from th e morphological decomposition and those needed to fit the HII-rotation curv es best are in excellent agreement. The effects of changing single paramete r values and possible error sources are discussed in detail. It turns out t hat the kinematics of the warm HII-gas of NGC 2336 can be explained without considering hydrodynamic effects, even in the central regions.