Dense molecular gas in Seyfert galaxies

Free access article

Issue		Astron. Astrophys. Suppl. Ser. Volume 141, Number 2, January II 2000


Page(s)		193 - 209
DOI		http://dx.doi.org/10.1051/aas:2000119

DOI: 10.1051/aas:2000119

Astron. Astrophys. Suppl. Ser. 141, 193-209

S.J. Curran - S. Aalto - R.S. Booth

Send offprint request: S. Curran

1 - Onsala Space Observatory, Chalmers University of Technology, S-439 92 Onsala, Sweden
e-mail: sjc@oso.chalmers.se

Received March 2; accepted October 22, 1999

Abstract:

We have used the 20 m Onsala and 15 m SEST telescopes to observe the CO $J=1\rightarrow0$ (simultaneously with CO $J=2\rightarrow1$ at SEST) and HCN $J=1\rightarrow0$ (simultaneously with CS $J=3\rightarrow2$ at SEST) transitions in 20 Seyfert galaxies. The sample consists of the 18 galaxies detected in CO $J=1\rightarrow0$ by [Heckman et al. (1989)] plus 2 which were not detected in their survey. We have successfully detected all of the galaxies in the CO transition and 13 in HCN of which NGCs 1667, 2273, 5033, 5135, 6814 and Mrk 273 are new detections. For the galaxies in which the beam-width exceeds $\approx10$ kpc we find that $\frac{L_{\rm HCN}}{L_{\rm CO}}\approx1/6$ , i.e. a global ratio similar to that of ultra-luminous infrared galaxies and over 10 times the ratio for normal spiral galaxies. This implies that $\frac{L_{\rm FIR}}{L_{\rm CO}}~(L_{\rm FIR}\sim10^{11}~L_{\odot}~{\rm Seyferts})\approx10\frac{L_{\rm FIR}}{L_{\rm CO}}~({\rm normal ~spirals})$ and we believe that the far infrared fluxes in our sample arise from star-burst activity, although we cannot rule out the possibility of a contribution from active galactic nuclei.

Key words: galaxies: Seyfert-galaxies: abundances -- galaxies: ISM

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