2000ApJ...535..663R

We present interferometric observations of CO J=1-0 emission in the central regions of the edge-on galaxy NGC 4631, known for its extended gaseous halo and its tidal interactions. Previous single-dish observations revealed that almost all of the CO emission arises from a central ring or barlike structure of length ∼4 kpc. We confirm this structure at higher resolution and find that it is bent at the center, reflecting the overall bend in this galaxy apparent from optical images. The kinematic evidence favors a rigidly rotating ring over a bar. The gaseous halo emission in several tracers is concentrated above and below this molecular structure. To the north of an emission peak at the eastern end of the structure is an extraplanar feature showing filamentary and shell-like properties we interpret as an energetic molecular outflow. The energies involved are difficult to estimate but are probably of order 10⁵⁴ ergs or more. The CO concentration in the disk below this structure coincides with a bright H II region complex, a peak of radio emission, and the brightest X-ray feature in the inner disk of the galaxy seen in a ROSAT HRI map, all suggesting intense star formation. A filament of radio continuum emission may also have a footprint in this region of the disk. The origin of the outflow is unclear.