2008ApJ...683...70H

We have mapped the central region of the Seyfert 1 galaxy NGC 1097 in ^ 12^CO J=2-1 with the Submillieter Array (SMA). The ^ 12^CO J=2-1 map shows a central concentration and a surrounding ring coinciding, respectively, with the Seyfert nucleus and a starburst ring. The line intensity peaks at the nucleus, whereas in a previously published ^ 12 ^CO J=1-0 map the intensity peaks at the starburst ring. The azimuthally averaged ^ 12 ^CO J=1-0 intensity ratio R₂₁ of the ring is about unity, which is similar to those in nearby active star-forming galaxies, suggesting that most of the molecular gas in the ring is involved in fueling the starburst. The ratio of molecular gas to dynamical mass in the starburst ring shows a somewhat lower value than that found in nearby star-forming galaxies, suggesting that the high R₂₁ of unity may be caused by additional effects, such as shocks induced by gas infall along the bar. The molecular gas can last for about 1.2x10⁸ yr without further replenishment, assuming a constant star formation rate. The central gas is rotating with the molecular ring in the same direction, while its velocity gradient is steeper than that of the ring, and similar to what usually observed in Seyfert 2 galaxies. To view the Seyfert nucleus without obscuration, the central gas can be a low-inclined disk or torus but not too low to be less massive than the mass of the host galaxy, or be a highly inclined thin disk or clumpy and thick torus, inner part of the galactic disk is also possible. The R₂₁ of ∼1.9 of the central gas is significantly higher than that of the ring, indicates that the activity of the Seyfert nucleus may significant influence the central gas.