Differences in the dense gas between type 1 and type 2 Seyferts

Details Differences in the dense gas between type 1 and type 2 Seyferts Differences in the dense gas between type 1 and type 2 Seyferts

Jun 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26as..144..271c&link_type=abstract

Astronomy and Astrophysics Supplement, v.144, p.271-284

Astronomy and Astrophysics

Astrophysics

11

Galaxies: Seyfert, Galaxies: Abundances, Galaxies: Structure, Galaxies: Evolution

Scientific paper

We have used observations of the CO J=1->0 transition in a sample of 20 Seyfert galaxies in order to test the result of \cite[Heckman et al. (1989)]{hec89}, who find that type 2 Seyferts have a higher molecular gas content than type 1 Seyferts. From our observational results alone, we possibly find that LCO/LFIR (Sy2)~ L_CO/L_FIR (Sy1) for L_FIR ~ 1011Lsun Seyferts, but LCO/LFIR (Sy2)~3L_CO/L_FIR (Sy1), when we use all of our sample (LFIR ~ 1010-1011Lsun). The results suggest that star-burst activity is most dominant in the (LFIR ~ 1010Lsun) type 2 Seyferts, and the relative contribution of this activity to the FIR flux (compared to the AGN) may decrease with increasing LFIR. Also, in order to test whether the Seyfert classes differ in their molecular gas distributions, we have used a simple model to estimate the inclination of the sub-kpc scale molecular ring, and, upon comparison with the observed spectra, conclude that the ring is generally aligned with the galactic disc, with the largest deviations from this being exhibited by the type 1 Seyferts. With regard to the nucleus, for most of the sample, the pc-scale obscuring torus appears to be approximately (within ~30deg) aligned with the molecular ring for both Seyfert classes. Based on results collected at the European Southern Observatory, La Silla, Chile and Onsala Space Observatory, Sweden.

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