The geometry of the Seyfert nucleus in NGC 4151 revisited. I - Cloudy structure from the /O III/ line profile analysis

Details The geometry of the Seyfert nucleus in NGC 4151 revisited. I - Cloudy structure from the /O III/ line profile analysis The geometry of the Seyfert nucleus in NGC 4151 revisited. I - Cloudy structure from the /O III/ line profile analysis

Jan 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...105..335p&link_type=abstract

Astronomy and Astrophysics, vol. 105, no. 2, Jan. 1982, p. 335-341.

Astronomy and Astrophysics

Astrophysics

31

Emission Spectra, Galactic Nuclei, Galactic Structure, Oxygen Ions, Seyfert Galaxies, Spectral Line Width, Astronomical Spectroscopy, Iron, Kinetic Energy, Plasma Clouds, Spectral Resolution, Spectrum Analysis

Scientific paper

A detailed analysis of the [O III] 500.68 nm emission line in NGC 4151 is discussed in this paper. The increased resolution (0.025 nm) of the present data allows a quantitative decomposition which leads to the following results.
- The cloud system in NGC 4151 involves about 6 components representing a mass of ionized gas of the order of 1O3 Msun, an internal macroscopic turbulent energy of 1050 erg and a kinetic energy of 1050 erg: in other words, as far as energetics is concerned, this phenomenon does not seem to play a major role in this nucleus.
- A broad (FWHM of 1750 km s-1) component is revealed by the [O III] 500.68 line profile analysis: it represents 45% of the total line flux and shows an emission velocity blue-shifted by 130 km s-1, with respect to the systemic velocity of the galaxy. This effect, already found by us in NGC 1068 and NGC 3783, is of extreme importance for understanding the geometry and dynamics of the forbidden line region in Seyfert nuclei.

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