Journal Article

Multifrequency VLA observations of the FR I radio galaxy 3C 31: morphology, spectrum and magnetic field

R. A. Laing, A. H. Bridle, P. Parma, L. Feretti, G. Giovannini, M. Murgia and R. A. Perley

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 386, issue 2, pages 657-672
Published in print May 2008 | ISSN: 0035-8711
Published online April 2008 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2008.13091.x
Multifrequency VLA observations of the FR I radio galaxy 3C 31: morphology, spectrum and magnetic field

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We present high-quality Very Large Array (VLA) images of the Fanaroff–Riley Class I (FR I) radio galaxy 3C 31 in the frequency range 1365–8440 MHz with angular resolutions from 0.25 to 40 arcsec. Our new images reveal complex, well resolved filamentary substructure in the radio jets and tails. We also use these images to explore the spectral structure of 3C 31 on large and small scales.

We infer the apparent magnetic field structure by correcting for Faraday rotation. Some of the intensity substructure in the jets is clearly related to structure in their apparent magnetic field: there are arcs of emission where the degree of linear polarization increases, with the apparent magnetic field parallel to the ridges of the arcs.

The spectra of the jets between 1365 and 8440 MHz are consistent with power laws within 60 arcsec of the nucleus. The spectral indices, α (flux density ∝ν−α) are significantly steeper (α= 0.62) within ≈7 arcsec of the nucleus than between 7 and 50 arcsec (α= 0.52–0.57). The spectra of the arcs and of the jet edges are also slightly flatter than the average for their surroundings. At larger distances, the jets are clearly delimited from surrounding larger scale emission both by their flatter radio spectra and by sharp brightness gradients.

The spectral index of 0.62 in the first 7 arcsec of 3C 31's jets is very close to that found in other FR I galaxies where their jets first brighten in the radio and where X-ray synchrotron emission is most prominent. Farther from the nucleus, where the spectra flatten, X-ray emission is fainter relative to the radio. The brightest X-ray emission from FR I jets is therefore not associated with the flattest radio spectra, but with a particle acceleration process whose characteristic energy index is 2α+ 1 = 2.24. The spectral flattening with distance from the nucleus occurs where our relativistic jet models require deceleration, and the flatter spectra at the jet edges may be associated with transverse velocity shear.

Keywords: acceleration of particles; magnetic fields; MHD; polarization; galaxies: jets; radio continuum: galaxies

Journal Article.  8606 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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