Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-28T16:22:36.737Z Has data issue: false hasContentIssue false
  • English
  • Français

High Resolution CO(3-2) and HCO+(4-3) Imaging of the Luminous Infrared Galaxy NGC 6240

Published online by Cambridge University Press:  01 August 2006

D. Iono ,
C. Wilson ,
M. Yun ,
S. Takakuwa ,
A. Peck ,
G. Petitpas ,
P. Ho ,
Z. Wang  and
Y. Pihlstrom
D. Iono
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan; email: d.iono@nao.ac.jp
C. Wilson
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada
M. Yun
Affiliation:
Department of Astronomy, University of Massachusetts, Amherst, MA 01003
S. Takakuwa
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan; email: d.iono@nao.ac.jp
A. Peck
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138
G. Petitpas
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138
P. Ho
Affiliation:
Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 106, Taiwan, R.O.C.
Z. Wang
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138
Y. Pihlstrom
Affiliation:
Department of Physics and Astronomy, University of New Mexico, 800 Yale Boulevard NE, Albuquerque, NM 87131
Rights & Permissions [Opens in a new window]

Extract

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.

We present interferometric CO(3-2), HCO+(4-3) and 870 micron continuum images of the luminous infrared galaxy NGC 6240 obtained at the Submillimeter Array (SMA). Our spatially resolved CO (3–2) and HCO+(4–3) emission peaks between the two nuclear components that are known to both harbor AGNs. The kinematical information provided by the CO (3–2) emission shows a rotating disk centered around the northern AGN and a possible face-on disk around the southern AGN, but the kinematics of gas between the two nuclei is extremely turbulent.

Keywords

galaxies: ISMgalaxies: kinematics and dynamicsgalaxies: individual(NGC 6240)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S235: Galaxy Evolution Across the Hubble Time , August 2006 , pp. 309
Copyright
Copyright © International Astronomical Union 2007