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The J = 3-2 CO line is detected for the first time in an external galaxy, in the nearby spiral IC 342. It is shown that in contrast to the J = 1-0 CO line, which favors optically thick and cool gas, the J = 3-2 CO line can be used to study a hot component in extragalactic nuclear environment. Limited mapping results suggest that the J = 3-2 CO emission arises from the same regions as the J = 1-0 CO emission. It is therefore likely that hot gas and strong star-formation activities are closely associated with the central molecular gas bar.
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Ho et al. (1987) studied this question.
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