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Visibility of scattered broad-line emission in Seyfert 2 galaxies

Author

Listed:
  • Charlene A. Heisler

    (The Australian National University)

  • Stuart L. Lumsden

    (Anglo-Australian Observatory)

  • Jeremy A. Bailey

    (Anglo-Australian Observatory)

Abstract

Active galaxies are thought to be powered by the accretion of gas onto a central massive black hole. Seyfert galaxies—the most common examples of nearby active galaxies—are separated into two classes based on their emission line widths1. Seyfert 1 galaxies exhibit broad emission lines that are attributed to ionized gas within 1 pc of the black hole, whereas the spectra of Seyfert 2 galaxies show only narrower emission lines, believed to originate from a much larger region around the core. The 'unified model' for Seyfert galaxies attributes these differences to the presence of a dusty torus of dense molecular gas surrounding the black hole2: the orientation of Seyfert 2 galaxies is such that the broad-line region is obscured. The detection3 in the polarization spectrum of broad emission lines scattered into our line of sight by free electrons in NGC1068 (the prototypical Seyfert 2 galaxy) and other Seyfert 2 galaxies4–8 has strengthened this view, but all of these galaxies were subject to selection biases. Here we report the results of a systematic search for polarized broad emission lines in a well defined sample of Seyfert 2 galaxies. We show that the ability to detect scattered broad emission lines is related to the far-infrared colours, in the manner predicted by the unified model.

Suggested Citation

  • Charlene A. Heisler & Stuart L. Lumsden & Jeremy A. Bailey, 1997. "Visibility of scattered broad-line emission in Seyfert 2 galaxies," Nature, Nature, vol. 385(6618), pages 700-702, February.
    • Handle: RePEc:nat:nature:v:385:y:1997:i:6618:d:10.1038_385700a0
    DOI: 10.1038/385700a0
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