Hostname: page-component-78c5997874-m6dg7 Total loading time: 0 Render date: 2024-11-13T06:40:19.188Z Has data issue: false hasContentIssue false
  • English
  • Français

12CO observations on narrow-line Seyfert 1 galaxies

Published online by Cambridge University Press:  01 July 2007

Toshihiro Kawaguchi ,
K. Nakanishi ,
K. Kohno ,
K. Ohta  and
K. Aoki
Toshihiro Kawaguchi
Affiliation:
Department of Physics, Aoyama Gakuin University, Sagamihara, Kanagawa 229-8558, Japan email: kawaguti@phys.aoyama.ac.jp
K. Nakanishi
Affiliation:
Nobeyama Radio Observatory, Minamimaki, Minamisaku, Nagano 384-1305, Japan
K. Kohno
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan
K. Ohta
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan
K. Aoki
Affiliation:
Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI 96720, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In order to investigate how the growth of galactic bulges is accompanied with the growth of central black holes (BHs), we observed molecular gas (fuel for the coming star formation) in possibly young active galaxies, narrow-line Seyfert 1 galaxies (NLS1s). We present the results of pilot observations of 12CO (1→0) line using the Nobeyama Millimeter Array for two FIR-bright NLS1s, ending in the first detection of their CO emission. Corresponding molecular-gas masses M(H2) of (1−3)×109M⊙ are the 2nd and 4th largest ones among NLS1s. Together with CO data for other NLS1s (including our sub-kpc observations) and for broad-line Seyfert 1 galaxies (BLS1s), we found that NLS1s and BLS1s contain a similar amount of molecular–gas. We do not see a significant difference in M(H2)/MBH ratios and in M(H2)/Mbulge ratios between NLS1s and BLS1s. The lack of a clear difference in M(H2) between them indicates either that bulge and BH growth phases are not overlapped or that the duration of star formation is much longer than that of active galaxies.

Keywords

galaxies: activegalaxies: evolutiongalaxies: ISMradio lines: ISMISM: molecules
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S245: Formation and Evolution of Galaxy Bulges , July 2007 , pp. 249 - 250
Copyright
Copyright © International Astronomical Union 2008

References

Brandt, W. N. & Boller, T. 1998, American Institute of Physics Conference Series 431, 191Google Scholar
Ferrarese, L. & Merritt, D. 2000, ApJ (Letters) 539, L9CrossRefGoogle Scholar
Gebhardt, K. et al. 2000, ApJ (Letters) 539, L13Google Scholar
Mineshige, S., Kawaguchi, T., Takeuchi, M., & Hayashida, K. 2000, PASJ, 52, 499Google Scholar
Nelson, C. H. 2000, ApJ (Letters), 544, L91Google Scholar
Pogge, R. W. 2000, New Astronomy Reviews 44, 381Google Scholar