Computer Science
Scientific paper
Feb 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981phdt........94a&link_type=abstract
PhD thesis (in German) to obtain the degree of a doctor in natural sciences (Dr.rer.nat.), Ruhr-Universitaet Bochum, Germany, xi
Computer Science
2
Radio Galaxies, Spectral Index Distribution, Polarization, Multifrequency Radio Mapping, Tailed Radio Sources
Scientific paper
Radio continuum maps of three tailed radio galaxies (3C 40, HB 13 and PKS 2247+11) were made with the 100-m radio telescope of the MPIfR Bonn at 2.7, 4.9 and 10.7 GHz with angular resolutions between 4.4 and 1.2 arcmin. A triple-feed system at 10.7 GHz allowed to map their extended outer regions for the first time at such frequencies and permitted to construct spectral index maps between 5 and 10 GHz at 2.7 arcmin resolution, as well as spectral comparisons between four or five frequencies at 4.4 arcmin resolution. Variations in spectral index were found to be a strong function of wavelength and angular resolution, due to appreciable spectral curvature (positive and negative). A concave radio spectrum is observed in the inner parts of the sources (<~250 kpc from the nucleus) which cannot be explained by the presence of a flat spectrum core alone. Either a superposition within the beam of compact flat spectrum jets and diffuse steep spectrum emission regions around these jets, or the presence of self-absorbed knots has to be invoked. Except for one of the outermost regions of 3C 40 there is no evidence for a spectral break due to synchrotron ageing of radiating electrons. Either a continuous injection of fresh particles or leakage of the aged particles from the emission region (or both) is required to explain the lack of appreciable convex spectral curvature. Polarization maps at 10.7 GHz show that the magnetic field is parallel to the boundaries of the radio tails and follows the bends of the tails at their leading edges. This supports the idea of a highly tangled magnetic field within the tails, which has been ordered by compression and shear at the interface with the intergalactic medium.
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