Dense and Warm Molecular Gas between Double Nuclei of the Luminous Infrared Galaxy NGC 6240

Details Dense and Warm Molecular Gas between Double Nuclei of the Luminous Infrared Galaxy NGC 6240 Dense and Warm Molecular Gas between Double Nuclei of the Luminous Infrared Galaxy NGC 6240

2005-07-07

arxiv.org/abs/astro-ph/0507163v1

Astronomy and Astrophysics

Astrophysics

25 pages, 8 figures, To be appeared in PASJ 57, No.4 (August 25, 2005) issue

Scientific paper

High spatial resolution observations of the 12CO(1-0), HCN(1-0), HCO+(1-0), and 13CO(1-0) molecular lines toward the luminous infrared merger NGC 6240 have been performed using the Nobeyama Millimeter Array and the RAINBOW Interferometer. All of the observed molecular emission lines are concentrated in the region between the double nuclei of the galaxy. However, the distributions of both HCN and HCO+ emissions are more compact compared with that of 12CO, and they are not coincident with the star-forming regions. The HCN/12CO line intensity ratio is 0.25; this suggests that most of the molecular gas between the double nuclei is dense. A comparison of the observed high HCN/13CO intensity ratio, 5.9, with large velocity gradient calculations suggests that the molecular gas is dense [n(H_2)=10^{4-6} cm^-3] and warm (T_kin>50 K). The observed structure in NGC 6240 may be explained by time evolution of the molecular gas and star formation, which was induced by an almost head-on collision or very close encounter of the two galactic nuclei accompanied with the dense gas and star-forming regions.

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