Molecular gas structure around an AGN with nuclear starburst: 3-D Non-LTE calculations of CO lines

Details Molecular gas structure around an AGN with nuclear starburst: 3-D Non-LTE calculations of CO lines Molecular gas structure around an AGN with nuclear starburst: 3-D Non-LTE calculations of CO lines

2004-10-11

arxiv.org/abs/astro-ph/0410254v1

Astrophys.J. 619 (2005) 93-104

Astronomy and Astrophysics

Astrophysics

11 pages, 10 figures. ApJ 20 Jan., 2005, in press

Scientific paper

10.1086/426377

We have performed three-dimensional, non-LTE radiative transfer calculations for 12CO and 13CO lines, applying them to our high-resolution hydrodynamic models of the `torus' around a SMBH in an active galactic nucleus. The hydrodynamic simulations reveal inhomogeneous and turbulent gas structure on a sub-pc scale in a circum-nuclear starburst region. Thick disks interlaced with filaments, clumps and holes are naturally formed due to the interplay among energy feedback from supernovae, self-gravity of the gas, galactic rotation, and radiative cooling. The intensity maps of the molecular lines for the circum-nuclear disks show a clumpy structure reflecting the intrinsic inhomogeneity and turbulent motion of the gas disk. The fine structure of the `torus' could be resolved in the nearby active galaxies using ALMA. We also found that the X-factor is not uniformly distributed in the central 100 pc region. The X-factor derived for 12CO(J=1-0) intensity depends strongly on the intensity, whereas the X for 12CO(3-2) is nearly constant over two orders of magnitude of the intensity. The suggested conversion factor for the molecular gas mass is X_CO (3-2) ~ 0.27 x 10^{20} cm^{-2} (K km s^{-1})^{-1}.

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