1999AJ....118.2184H

We present high-resolution interferometric data of the inner 30' of the H I gas of the irregular galaxy NGC 4449. In addition to the previously known two counter-rotating gas systems, the H I exhibits an unusual ring morphology and high velocity dispersions in the outer part of the optical galaxy. In addition the position angle and inclination of the outer gas are moderately different from those of the optical galaxy. The position angle and inclination of the inner gas system are approximately similar to those of the inner optical galaxy only if strong deviations from ordered motion in the center are ignored. The H I interstellar medium appears to be fragmented into clouds, which are similar to clouds observed in other galaxies. There is very little correlation between the H I surface density and Hα surface brightness. The optical isophotes of the galaxy define three different and distinct position angles and inclinations. The inner structure is similar in properties to a bar structure that includes a large fraction of the optical galaxy. The nature of the middle structure is unclear. Exterior to these bars are unusual faint filamentary structures. The V- and J-band surface photometry are well fit by an exponential disk to low surface brightness levels, including the bar structures. However, the central surface brightness is unusually bright. The star formation activity compared over three different time scales as a function of radius is fairly consistent. In the optical there are also unusual extensions at low light levels in the outskirts of the galaxy. Many characteristics of the gas and stars are consistent with a picture in which NGC 4449 has been disturbed by an external perturber, and the gas has not yet returned to equilibrium.