Abstract
2.4″ resolution interferometric observations of the CO emission in the merger galaxy NGC 7252 are reported. The molecular gas concentration around the nucleus of this galaxy is well resolved and shows solid body rotation in a direction opposite to the motion of the ionized gas in the outer parts of the galaxy. The CO surface brightness distribution is complex, yet the kinematics of the molecular gas bears striking resemblance to that of the inner ionized gas disk. The CO can be traced farther into the galactic center than the Hα emission, but a small central hole (∼300 pc radius) apparently free of gas remains
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