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The motion of an emission-line region near the center of the galaxy NGC 4151

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Abstract

Possible orbits for the motion of a region in the gravitational field of the central body of the galaxy NGC 4151 are presented. The region is manifest through its line emission, observed in the red wing of the Hα, Pβ, and other broad lines. We carried out a computer selection of all Keplerian orbits for which the measured radial velocities of the emission-line region could be observed. We used radial-velocity data obtained by us at the Fesenkov Astrophysical Institute, as well as data from the literature. The computation results can be used to determine the mass range for the central body of NGC 4151 that provides the best agreement with the observational data: (61–65)× 106 M ⊙. Suitably designed monitoring of active galactic nuclei can be used to verify these results, and to carry out similar analyses for other Seyfert galaxies.

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Authors and Affiliations

  1. Fesenkov Astrophysics Institute, Almaty, Kazakhstan

    E. K. Denissyuk, R. R. Valiullin & V. N. Gaisina

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  1. E. K. Denissyuk
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  2. R. R. Valiullin
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  3. V. N. Gaisina
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Correspondence to E. K. Denissyuk.

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Original Russian Text © E.K. Denissyuk, R.R. Valiullin, V.N. Gaisina, 2011, published in Astronomicheskii Zhurnal, 2011, Vol. 88, No. 9, pp. 828–836.

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Denissyuk, E.K., Valiullin, R.R. & Gaisina, V.N. The motion of an emission-line region near the center of the galaxy NGC 4151. Astron. Rep. 55, 761–769 (2011). https://doi.org/10.1134/S1063772911090034

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  • DOI: https://doi.org/10.1134/S1063772911090034

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