The Structure and Dynamics of the Early-Type Resonance Ring Galaxy IC 4214. II. Models

Details The Structure and Dynamics of the Early-Type Resonance Ring Galaxy IC 4214. II. Models The Structure and Dynamics of the Early-Type Resonance Ring Galaxy IC 4214. II. Models

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aj....117..792s&link_type=abstract

The Astronomical Journal, Volume 117, Issue 2, pp. 792-810.

Astronomy and Astrophysics

Astronomy

54

Galaxies: Individual: Alphanumeric: Ic 4214, Galaxies: Kinematics And Dynamics, Galaxies: Photometry, Galaxies: Structure

Scientific paper

The first paper in this series presented optical (UBVI) and near-infrared (H) surface photometry and Hα 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, as defined by the near-infrared data. The gas behavior is modeled with two-dimensional sticky particle simulations that employ a rigidly rotating nonaxisymmetric potential. Our goals are to interpret the morphology and velocity 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 also study the orbital families in the derived IC 4214 model. A fairly good match, in both morphology and kinematics, is obtained for Omega_bar~40+/-5 km s^-1 kpc^-1, placing the bar corotation slightly beyond the end of the bar (r_bar/r_cr~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 accounts quantitatively for the large difference in the orientation of IC 4214 as derived in our first paper with photometric and kinematic methods.

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