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Long-Slit Spectroscopy of IC 5135 and NGC 4388

Published online by Cambridge University Press:  07 August 2017

Joseph C. Shields  and
Alexei V. Filippenko
Joseph C. Shields
Affiliation:
Department of Astronomy, University of California, Berkeley, CA 94720 U.S.A.
Alexei V. Filippenko
Affiliation:
Department of Astronomy, University of California, Berkeley, CA 94720 U.S.A.

Extract

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The nucleus of the peculiar Sa galaxy IC 5135 has strong emission lines whose relative intensities resemble those of Seyfert 2 galaxies (Phillips, Charles, and Baldwin 1983). However, the galaxy exhibits relative line intensities such as [O III] λ5007/Hβ = 6.5 and He II λ4686/Hβ = 0.17 that are considerably smaller than typical Seyfert 2 values of 11 and 0.3, respectively (Koski 1978). New, high-resolution spectra (FWHM ≈ 2Å) obtained at Las Campanas Observatory reveal that the Hβ emission-line profile actually consists of a relatively strong, narrow component (FWHM ≈ 250 km s−1) superposed on a much weaker, broad base (FWHM ≈ 1000 km s−1; Fig. 1). A similar two-component profile is evident in [O I] λ6300, whose narrow core probably comes from circumnuclear H II regions that produce little [O III] and He II emission. The strong, high-order Balmer absorption lines are consistent with the presence of a young stellar population in the nucleus.

Type
Part 8: Relationships of Nucleus, Galaxy and Environment
Information
Symposium - International Astronomical Union , Volume 134: Active Galactic Nuclei , 1989 , pp. 480 - 481
Copyright
Copyright © Kluwer 1989 

References

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