Volume 415, Number 3, March I 2004
|Page(s)||905 - 913|
|Published online||13 February 2004|
The inner kiloparsec of the jet in 3C 264
Dpto. Física Teórica y del Cosmos, Universidad de Granada, Avda. Fuentenueva s/n, 18071 Granada, Spain
2 Instituto de Astrofísica de Andalucía (CSIC), Apdo. 3004, 18080 Granada, Spain
3 Istituto di Radioastronomia (CNR), via P. Gobetti 101, 40129 Bologna, Italy
4 Dipartimento di Astronomia, Universitá di Bologna, via Ranzani 1, 40127 Bologna, Italy
5 National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA
Corresponding author: L. Lara, firstname.lastname@example.org
Accepted: 3 November 2003
We present new multi-frequency EVN, MERLIN and VLA observations of the radio source 3C 264, sensitive to linear scales ranging from parsec to several kiloparsecs. The observations confirm the existence of regions with different properties in the first kiloparsec of the jet. The most remarkable feature is the transition between a well collimated narrow jet at distances from the core below 80 pc, to a conical-shaped wide jet, with an opening angle of . Another change of properties, consisting of an apparent deflection of the jet ridge line and a diminution of the surface brightness, occurs at a distance of ~300 pc from the core, coincident with the radius of a ring observed at optical wavelengths. Our observations add new pieces of information on the spectrum of the radio-optical jet of 3C 264, with results consistent with a synchrotron emission mechanism and a spectrum break frequency in the infrared. Brightness profiles taken perpendicularly to the jet of 3C 264 are consistent with a spine brightened jet at distances below 100 pc from the core, and an edge-brightened jet beyond, which can be interpreted as evidence of a transverse jet velocity structure. Our observations do not allow us to distinguish between the presence of a face-on dust and gas disk at the center of the host galaxy of 3C 264, or rather an evacuated bubble. However, the properties of the jet structure, the changes in the polarization angle, and the plausible jet orientation can be naturally brought into agreement in the bubble scenario.
Key words: galaxies: individual: 3C 264 / galaxies: individual: NGC 3862 / galaxies: active / galaxies: nuclei / galaxies: jets / radio continuum: galaxies
© ESO, 2004
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