Model of Molecular Abundance in an AGN disk of NGC 1068

Details Model of Molecular Abundance in an AGN disk of NGC 1068 Model of Molecular Abundance in an AGN disk of NGC 1068

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.192h&link_type=abstract

The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole

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Scientific paper

We model the spatial dependence of molecular abundances in the accretion disk of NGC 1068, a typical AGN-dominant galaxy. A number of different possible disk structures are used, and X-rays, cosmic-rays, and UV-photons are included in the model. The effects of these parameters on molecular abundances are examined for the well-observed species CO, CN, HCN, and HCO+ and also for the recently observed carbon-chain species C2H, c-C3H2 and HC3N. Although the effects of X-rays can enhance CN and HCN abundances, our results show that a high-temperature effect in the inner portion of disks can explain the different peak locations for the CN/HCN and CN/CO ratios. Photon-dominated regions are not likely to be the dominant in the very inner disk. Sulfur-containing species can be probes of the gas-phase elemental abundance of sulfur, especially CS and SO. We briefly discuss the comparison with other types of galaxies such as (Ultra-) Luminous Infrared Galaxies and starburst galaxies.

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