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Astron. Astrophys. 327, 513-521


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The high-frequency compact radio structure
of the peculiar quasar 4C 39.25

A. Alberdi1,2, T.P. Krichbaum3, D.A. Graham3, A. Greve4, M. Grewing4, J.M. Marcaide5, A. Witzel3, R.S. Booth6, and
L.B. Bååth6, and F. Colomer6,7, and S. Doeleman8, and A.P. Marscher9, and A.E.E. Rogers8, and C.J. Schalinski4,10, and K. Standke3

1Laboratorio de Astrofísica Espacial y Física Fundamental, Apdo. 50727, E-28080 Madrid, Spain
2Instituto de Astrofísica de Andalucía, CSIC, Apdo. 3004, Granada, Spain
3Max Planck Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany
4IRAM, Domaine Universitaire, Grenoble, France
5Departamento de Astronomía, Universitat de València, E-46100 Burjassot, Spain
6Onsala Space Observatory, Onsala, Sweden
7Observatorio de Yebes, Apdo. 148, Guadalajara, Spain
8NEROC, Haystack Observatory, Westford, Massachusetts, USA
9Boston University, Boston, MA, USA
10now at Institut für Weltraumsensorik (DLR), Rudower Chaussee 5, D-12489 Berlin, Germany

Received 24 February 1997 / Accepted 2 April 1997

Abstract

We present new high angular resolution images of the compact non-thermal radio source 4C 39.25 obtained from VLBI observations at FORMULA1.3 cm, FORMULA7 mm, and FORMULA3 mm wavelengths. These maps and Gaussian modelfits show that the milli-arcsecond to sub-milliarcsecond structure of 4C 39.25 consists of a complex bent core-jet structure with embedded moving and stationary VLBI components. Facilitated by the small observing beams and high angular resolutions obtained at mm-wavelengths, we measured the relative positions of the jet components with an accuracy of a few hundred micro-arcseconds. This allows the detailed followup of the ongoing merging process of a westward superluminally moving component (b) with a stationary component a, located at FORMULA2.9 mas east of the putative core d. In contrast to the other components of the structure with steeper spectra, the westernmost component d exhibits an inverted spectrum peaking between FORMULA7 mm and FORMULA3 mm, thus further supporting its identification as the VLBI core, self-absorbed at longer wavelengths.

From two VLBI maps obtained nearly simultaneously at FORMULA7 mm and FORMULA1.3 cm, we made the first spectral index map of 4C 39.25 in this wavelength regime. The main characteristics of the spectral index distribution of the jet are pronounced changes of the spectral index between orientations parallel and transverse to the jet axis. Near the merging components a and b the spectral index steepens with increasing separation from d. However, in the bridge of emission c, which connects d with a and b, the spectral index gradient has a direction transverse to the jet axis, suggesting a frequency dependent jet curvature and edge-brightening. A brief discussion of this behaviour within current jet models is presented.

Key words: galaxies: jets - quasars: 4C 39.25 - techniques: interferometric - radio continuum: general

Send offprint requests to: A. Alberdi


© European Southern Observatory (ESO) 1997

Online publication: October 14, 1997
Last change: April 6, 1998
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