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We have mapped the central region of the Seyfert 1 galaxy NGC 1097 in12CO(J=2-1) with the Submillieter Array (SMA). The 12CO(J=2-1) map shows acentral concentration and a surrounding ring, which coincide respectively withthe Seyfert nucleus and a starburst ring. The line intensity peaks at thenucleus, whereas in a previously published 12CO(J=1-0) map the intensity peaksat the starburst ring. The molecular ring has an azimuthally averaged12CO(J=2-1)/(J=1-0) intensity ratio (R21) of about unity, which is similar tothose in nearby active star forming galaxies, suggesting that most of themolecular mass in the ring is involved in fueling the starburst. The moleculargas can last for only about 1.2\times10^8 years without further replenishmentassuming a constant star formation rate and a perfect conversion of gas tostars. The velocity map shows that the central molecular gas is rotating withthe molecular ring in the same direction, while its velocity gradient is muchsteeper than that of the ring. This velocity gradient of the central gas issimilar to what is usually observed in some Seyfert 2 galaxies. To view theactive nucleus directly in the optical, the central molecular gas structure caneither be a low-inclined disk or torus but not too low to be less massive thanthe mass of the host galaxy itself, be a highly-inclined thin disk or clumpyand thick torus, or be an inner part of the galactic disk. The R21 value of~1.9 of the central molecular gas component, which is significantly higher thanthe value found at the molecular gas ring, indicates that the activity of theSeyfert nucleus may have a significant influence on the conditions of themolecular gas in the central component.

Interferometric 12CO(J=2-1) image of the Nuclear Region of Seyfert 1 Galaxy NGC 1097