Free access article

A&A 435, 43-64 (2005)
DOI: 10.1051/0004-6361:20042271

A dichotomy in the orientation of dust and radio jets in nearby low-power radio galaxies

G. A. Verdoes Kleijn¹ and P. T. de Zeeuw<sup>2

1</sup>  European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748, Garching bei München, Germany
    e-mail: gverdoes@eso.org
²  Sterrewacht Leiden, Postbus 9513, 2300 RA Leiden, The Netherlands
    e-mail: dezeeuw@strw.leidenuniv.nl

(Received 28 October 2004 / Accepted 28 January 2005 )

Abstract
We examine the properties of central dust in nearby quiescent and active early-type galaxies. The active galaxies are low-power radio galaxies with Fanaroff & Riley type I or I/II radio jets. We focus on (a) the comparison of the dust distributions in the active and quiescent galaxy samples; and (b) the relation between the radio jet and dust orientations. Our main observational conclusions are: (i) in line with previous studies, the dust detection rate is higher in radio-jet galaxies than in non radio-jet galaxies; (ii) radio galaxies contain a higher fraction of regular dust "ellipses" compared to quiescent galaxies which contain more often irregular dust distributions; (iii) the morphology, size and orientation of dust ellipses and lanes in quiescent early-types and active early-types with kpc-scale radio jets is very similar; (iv) dust ellipses are aligned with the major axis of the galaxy, dust lanes do not show a preferred alignment except for large (>kpc) dust lanes which are aligned with the minor axis of the galaxy; and (v) as projected on the sky, jets do not show a preferred orientation relative to the galaxy major axis (and hence dust ellipses), but jets are preferentially perpendicular to dust lanes.

We show that the dust ellipses are consistent with being nearly circular thin disks viewed at random viewing angles. The lanes are likely warped dust structures, which may be in the process of settling down to become regular disks or are being perturbed by a non-gravitational force. We use the observed dust-jet orientations to constrain the three-dimensional angle  between jet and dust. For dust-lane galaxies, the jet is approximately perpendicular to the dust structure, while for dust-ellipse galaxies there is a much wider distribution of  .

We discuss two scenarios that could explain the dust/jet/galaxy orientation dichotomy. If lanes are indeed settling, then the jet orientation apparently is roughly aligned with the angular momentum of the dust before it settles. If lanes are perturbed by a jet-related force, it appears that it causes the dust to move out of its equilibrium plane in the galaxy into a plane which is perpendicular to the jet.

Key words: galaxies: active -- galaxies: elliptical and lenticular, cD -- galaxies: nuclei -- galaxies: jets -- ISM: dust, extinction

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© ESO 2005

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