EDP Sciences
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Volume 424, Number 2, September III 2004
Page(s) 455 - 464
Section Extragalactic astronomy
DOI http://dx.doi.org/10.1051/0004-6361:20040481

A&A 424, 455-464 (2004)
DOI: 10.1051/0004-6361:20040481

On-axis spectroscopy of the z $\mathsf{=0.144}$ radio-loud quasar HE 1434-1600: an elliptical host with a highly ionized ISM

G. Letawe1, F. Courbin1, P. Magain1, M. Hilker2, P. Jablonka3, K. Jahnke4 and L. Wisotzki4, 5

1  Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août, 17, Bât. B5C, Liège 1, Belgium
    e-mail: gletawe@ulg.ac.be
2  Sternwarte der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
3  GEPI, Observatoire de Paris, Place Jules Janssen, 92915 Meudon Cedex, France
4  Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482, Potsdam, Germany
5  Institut für Physik, Universität Potsdam, Am Neuen Palais 10, 14469 Potsdam, Germany

(Received 19 March 2004 / Accepted 11 May 2004)

VLT on-axis optical spectroscopy of the z=0.144 radio-loud quasar HE 1434-1600 is presented. The spatially resolved spectra of the host galaxy are deconvolved and separated from those of the central quasar in order to study the dynamics of the stars and gas as well as the physical conditions of the ISM. We find that the host of HE 1434-1600 is an elliptical galaxy that resides in a group of at least 5 member galaxies, and that most likely experienced a recent collision with its nearest companion. Compared with other quasar host galaxies, HE 1434-1600 has a highly ionized ISM. The ionization state corresponds to that of typical Seyferts, but the ionized regions are not distributed in a homogeneous way around the QSO, and are located preferentially several kiloparsecs away from it. While the stellar absorption lines do not show any significant velocity field, the gas emission lines do. The observed gas velocity field is hard to reconcile with dynamical models involving rotating disk, modified Hubble laws or power laws, that all require extreme central masses ( $M>10^{9}~M_{\odot}$) to provide only poor fit to the data. Power law models, which best fit the data, provide a total mass of M( <10 kpc)  = 9.2  $\times$ $10^{10}~M_{\odot}$. We conclude that the recent interaction between HE 1434-1600 and its closest companion has strongly affected the gas velocity and ionization state, from the center of the galaxy to its most external parts.

Key words: galaxies: kinematics and dynamics -- galaxies: interactions -- galaxies: quasars: individual: HE 1434-1600 -- techniques: image processing -- techniques: spectroscopic

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