Infrared fluorescence of H2 in NGC 6240: A starburst origin for the H2 luminosity

Masuo Tanaka, Tetsuo Hasegawa, Ian Gatley

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24 Scopus citations

Abstract

The highly luminous galaxy-merger system NGC 6240 exhibits strong emission lines of vibrationally excited molecular hydrogen in the near-infrared. In disagreement with previous analyses, which have attributed these H2 lines to shock excitation or X-ray irradiation, we show here that the published line ratios imply ultraviolet excitation followed by infrared fluorescence. We apply the method of analysis developed for galactic sources to the central ∼2 kpc of NGC 6240 and show that the line ratios are well reproduced as a mixture of fluorescent and thermal components. Although the fluorescent component contributes only 30% to the υ = 1-0 S(1) intensity, fluorescent lines from higher vibrational levels makes up a large luminosity which overwhelms the thermal component; the total H2 luminosity amounts to 3 × 109 L, of which 70% is due to fluorescence. This luminous fluorescent H2 emission is excited by ultraviolet (λ ∼ 1000 Å) photons most probably radiated by many (∼1 × 108) early B stars. The abundance of early B stars and the well-known deficit of O stars indicate a sharp upper mass cutoff at ∼20 M in the present-day mass spectrum in the central region of NGC 6240. We present a starburst model in which the present-day stellar population and other observed features can be reproduced if (1) the central region of NGC 6240 experienced a cataclysmic starburst which stopped suddenly a few times 107 yr ago and if (2) the initial mass function there had a lower mass cutoff at ∼5 M. The high mass edge of the present-day mass spectrum can be explained as a result of evolution of massive stars; no artificial high mass cutoff in the initial mass function is necessary, although we do not exclude a possibility of its presence. An important parameter in the present starburst model is the efficiency to convert ultraviolet photons to H2 infrared fluorescence. The above explanation for NGC 6240 requires the efficiency as high as that in Galactic reflection nebulae (e.g., NGC 2023), while other luminous starburst galaxies may be less efficient by an order of magnitude.

Original languageEnglish (US)
Pages (from-to)516-521
Number of pages6
JournalAstrophysical Journal
Volume374
Issue number2
DOIs
StatePublished - Jun 20 1991
Externally publishedYes

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Galaxies: individual (NGC 6240)
  • Galaxies: interactions
  • Infrared: spectra
  • Interstellar : molecules
  • Molecular processes
  • Radiation mechanisms

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