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The cool and warm molecular gas in M82 with Herschel-SPIRE

  • J. Kamenetzky (a1), J. Glenn (a1), N. Rangwala (a1), P. Maloney (a1), M. Bradford (a2), C. D. Wilson (a3), G. J. Bendo (a4), M. Baes (a5), A. Boselli (a6), A. Cooray (a7), K. G. Isaak (a8), V. Lebouteiller (a9), S. Madden (a9), P. Panuzzo (a9), M. R. P. Schirm (a3), L. Spinoglio (a10) and R. Wu (a9)...

Abstract

We present Herschel-SPIRE imaging spectroscopy (194-671 μm) of the bright starburst galaxy M82. We use RADEX and a Bayesian Likelihood Analysis to simultaneously model the temperature, density, column density, and filling factor of both the cool and warm components of molecular gas traced by the entire CO ladder up to J=13-12. The high-J lines observed by SPIRE trace much warmer gas (~500 K) than those observable from the ground. The addition of 13CO (and [C I]) is new and indicates that [C I] may be tracing different gas than 12CO. At such a high temperature, cooling is dominated by molecular hydrogen; we conclude with a discussion on the possible excitation processes in this warm component. Photon-dominated region (PDR) models require significantly higher densities than those indicated by our Bayesian likelihood analysis in order to explain the high-J CO line ratios, though cosmic-ray enhanced PDR models can do a better job reproducing the emission at lower densities. Shocks and turbulent heating are likely required to explain the bright high-J emission.

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References

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Kamenetzky, J., Glenn, J., Rangwala, N., et al. 2012, ApJ 753, 70
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The cool and warm molecular gas in M82 with Herschel-SPIRE

  • J. Kamenetzky (a1), J. Glenn (a1), N. Rangwala (a1), P. Maloney (a1), M. Bradford (a2), C. D. Wilson (a3), G. J. Bendo (a4), M. Baes (a5), A. Boselli (a6), A. Cooray (a7), K. G. Isaak (a8), V. Lebouteiller (a9), S. Madden (a9), P. Panuzzo (a9), M. R. P. Schirm (a3), L. Spinoglio (a10) and R. Wu (a9)...

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