Abstract
The central 2° × 2° area of the Small Magellanic Cloud (SMC) has been fully surveyed in the J = 1 → 0 rotational transition of 12 CO at an angular resolution of 8.8'. Most of the emission arises from two large complexes, located in the southwest and northeast regions of the Bar, closely associated with the most intense H I emission from the SMC. Five individual molecular clouds are identified; their peak antenna temperatures are very weak, ∼ 0.035 K. It is suggested that for the SMC, the conversion factor to derive the column density of molecular hydrogen from the velocity-integrated CO line emission is 6 × 10 21 (K km cm 2 ) -1 s, which is about 20 times higher than the value adopted for our Galaxy.
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