The state of the molecular gas in a luminous starburst Seyfert 2 galaxy: NGC 1068 revisited

We present fully sampled (CO)-C-12, (CO)-C-13 J =2-1, 3-2 maps of the inner similar to 1' x 1' region of NGC 1068. We combine these measurements with an existing interferometric map of (CO)-C-12 J=1-0 that includes single dis h data and thus contains all the flux present. This allows a reliable estim ate of the (CO)-C-12 (J =-3-2)/(J =1-0) ratio at the highest angular resolu tion currently possible and the use of this sensitive line ratio to probe t he physical condition of the molecular gas. We also present, two measuremen ts of the faint (CO)-O-18 J =2-1 emission that confirm earlier measurements of a high (CO)-O-18/(CO)-C-13 intensity ratio in this galaxy. The ratios o f the (CO)-C-12,(CO)-C-13 isotopes can only be reproduced for small to mode rate optical depths of (CO)-C-12 J = 1-0 (tau similar to 1-2), which is inc ompatible with the high (CO)-O-18/(CO)-C-13 ratios observed. A simple two-p hase model for the gas can account for all the observed line ratios if the (CO)-O-18 emission and part of the (CO)-C-13 emission arise in a dense spat ially concentrated component, where (CO)-O-18 J = 1-0 has optical depths of tau greater than or similar to 1. The (CO)-C-12 emission originates from a warmer, diffuse gas phase with tau similar to 1-2 for J =1-0. The dense ga s phase contains the bulk of the molecular gas mass, whereas the diffuse ph ase may not be virialized, leading to an overestimate of molecular gas mass when deduced from the luminosity of the (CO)-C-12 J = 1-0 line and a stand ard galactic conversion factor. This suggests that, since type 2 Seyferts h arbor a central starburst more often than type 1, the higher average (CO)-C -12 J=1-0 luminosity of type 2 hinted by earlier studies-may simply reflect a difference in molecular gas excitation rather than in gas mass.