The structure and dynamics of the early-type resonance ring galaxy IC 4214. II. Models

The first paper in this series presented optical (UBVI) and near-infrared ( H) surface photometry and H alpha Fabry-Perot interferometry of IC 4214, an excellent example of a multiringed galaxy with a weak bar. In the present paper, we analyze the nonaxisymmetric gravitational potential of IC 4214, a s defined by the near-infrared data. The gas behavior is modeled with two-d imensional sticky particle simulations that employ a rigidly rotating nonax isymmetric potential. Our goals are to interpret the morphology and velocit y field of IC 4214 and to obtain a model from which the bar pattern speed, halo contribution, and relative bulge and disk masses can be deduced. We al so study the orbital families in the derived IC 4214 model. A fairly good match, in both morphology and kinematics, is obtained for Ome ga(bar) approximate to 40 +/- 5 km s(-1) kpc(-1), placing the bar corotatio n slightly beyond the end of the bar (r(bar)/r(cr) approximate to 0.72 +/- 0.05). The deduced bar amplitude implies that the visible mass of the disk dominates over the unseen halo (M-disk/M-halo > 3-4). Moreover, our model a ccounts quantitatively for the large difference in the orientation of IC 42 14 as derived in our first paper with photometric and kinematic methods.