EDP Sciences
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Volume 408, Number 1, September II 2003
Page(s) 101 - 109
Section Galactic structure and dynamics
DOI http://dx.doi.org/10.1051/0004-6361:20030893

A&A 408, 101-109 (2003)
DOI: 10.1051/0004-6361:20030893

The narrow line region of Ark 564

M. Contini1, 2, A. Rodríguez-Ardila3 and S. M. Viegas1

1  Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Rua do Matão 1226, CEP 05508-900, São Paulo, SP, Brazil
    e-mail: viegas@astro.iag.usp.br
2  School of Physics and Astronomy, Tel-Aviv University, Ramat-Avit, Tel-Aviv 69978, Israel
3  Laboratório Nacional de Astrofísica, Rua dos Estados Unidos 154, Bairro das Nações, CEP 37500-000, Itajubá, MG, Brazil
    e-mail: aardila@lna.br

(Received 14 February 2003 / Accepted 5 June 2003)

The continuum and emission-line spectrum of the narrow-line Seyfert 1 galaxy Ark 564 is used to investigate, for the first time, the physical conditions and structure of its narrow line region (NLR). For this purpose, composite models, accounting for the coupled effect of photoionization and shocks, are employed. The emission-line spectrum of Ark 564, which ranges from the ultraviolet to the near-infrared, shows a rich forbidden line spectrum. Strong emphasis is given to the study of the coronal line region. The diversity of physical conditions deduced from the observations requires multi-cloud models to reproduce the observed lines and continuum. We find that a combination of high velocity ( $V_{\rm s} = 1500$  $\rm km\, s^{-1}$) shock-dominated clouds as well as low velocity ( $V_{\rm s} = 150$  $\rm km\, s^{-1}$) radiation-dominated clouds explains the coronal lines, while the optical low-ionization lines are mainly explained by shock-dominated clouds. The results for Ark 564 are compared with those obtained for other Seyfert galaxies previously analyzed such as NGC 5252, Circinus, NGC 4051 and NGC 4151. The model results for the ultraviolet and optical permitted lines suggest that the broad line region may contribute up to 80%, depending on the emission-line, being of about 30% for H $\beta$. The consistency of the multi-cloud model is checked by comparing the predicted and observed continuum, from radio to X-ray, and indicate that the dust-to-gas ratio in the clouds varies from 10 -15 to 10 -12.

Key words: galaxies: Seyfert -- galaxies: individual: Ark 564 -- infrared: galaxies -- line: formation

Offprint request: M. Contini, marcel@wise1.tau.ac.il

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