ISO spectroscopy of star formation and active nuclei in the luminous infrared galaxy NGC 6240

Details ISO spectroscopy of star formation and active nuclei in the luminous infrared galaxy NGC 6240 ISO spectroscopy of star formation and active nuclei in the luminous infrared galaxy NGC 6240

2003-07-31

arxiv.org/abs/astro-ph/0307552v1

Astron.Astrophys.409:867-878,2003

Astronomy and Astrophysics

Astrophysics

5 figures. Accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20031165

We present Infrared Space Observatory mid- and far-infrared spectroscopy of the merging galaxy NGC 6240, an object presenting many aspects of importance for the role of star formation and AGN activity in [ultra]luminous infrared galaxies. The mid-infrared spectrum shows starburst indicators in the form of low excitation fine-structure line emission and aromatic `PAH' features. A strong high excitation [OIV] line is observed which most likely originates in the Narrow Line Region of an optically obscured AGN. NGC 6240 shows extremely powerful emission in the pure rotational lines of molecular hydrogen. We argue that this emission is mainly due to shocks in its turbulent central gas component and its starburst superwind. The total shock cooling in infrared emission lines accounts for ~0.6% of the bolometric luminosity, mainly through rotational H_2 emission and the [OI] 63micron line. We analyse several ways of estimating the luminosities of the starburst and the AGN in NGC 6240 and suggest that the contributions to its bolometric luminosity are most likely in the range 50-75% starburst and 25-50% AGN.

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