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Carbon chain abundance in the diffuse interstellar medium.

L J Allamandola1, D M Hudgins, C W Bauschlicher

  • 1NASA Ames Research Center, Moffett Field, CA 94034-1000, USA. lallamandola@mail.arc.nasa.gov

Astronomy and Astrophysics
|September 7, 2001
PubMed
Summary
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Infrared spectroscopy reveals carbon chains in the diffuse interstellar medium. These molecules, including cyanopolyynes and hydrogenated chains, have abundances consistent with dense clouds, contributing to diffuse interstellar bands.

Area of Science:

  • Astronomy and Astrophysics
  • Astrochemistry
  • Spectroscopy

Background:

  • The diffuse interstellar medium (ISM) is a reservoir of gas and dust.
  • Infrared spectroscopy offers a unique window into molecular composition.
  • Previous studies suggested the presence of specific carbon anions in the ISM.

Purpose of the Study:

  • To search for infrared signatures of various carbon chain molecules in the diffuse ISM.
  • To analyze the Infrared Space Observatory (ISO) and Infrared Telescope (IRTS) spectrometer data.
  • To determine the abundance and contribution of carbon chains to interstellar features.

Main Methods:

  • Analysis of mid-infrared spectra from the IRTS.
  • Theoretical calculations of infrared band frequencies and intensities for carbon chain species.

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  • Comparison of observed spectral features with theoretical predictions.

    • Main Results:

    • Identified infrared signatures consistent with various carbon chain species (cyanopolyynes, linear carbon molecules, hydrogenated carbon chains).
    • Estimated abundances of these carbon chains in the diffuse ISM to be around 10^-10 relative to hydrogen.
    • Calculated that carbon chains constitute a small fraction of cosmic carbon and contribute to diffuse interstellar bands.

    Conclusions:

    • Carbon chain molecules are present in the diffuse interstellar medium.
    • Their abundances are comparable to those found in dense molecular clouds.
    • These species play a role in the observed diffuse interstellar bands.