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Title:
The supernova remnant W50 at 5 GHz
Authors:
Downes, A. J. B.; Pauls, T.; Salter, C. J.
Affiliation:
AA(Mullard Radio Astronomy Observatory, Cambridge, England), AB(Koeln, Universitaet, Cologne, West Germany), AC(National Radio Astronomy Observatory, Tucson, AZ)
Publication:
Royal Astronomical Society, Monthly Notices (ISSN 0035-8711), vol. 218, Feb. 1, 1986, p. 393-407. SERC-supported research. (MNRAS Homepage)
Publication Date:
02/1986
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
RADIO SOURCES (ASTRONOMY), STELLAR SPECTROPHOTOMETRY, SUPERNOVA REMNANTS, ASTRONOMICAL MAPS, INTERSTELLAR MAGNETIC FIELDS, LINEAR POLARIZATION, RADIANT FLUX DENSITY, SPECTRAL ENERGY DISTRIBUTION, STELLAR ENVELOPES, STELLAR LUMINOSITY
Bibliographic Code:
1986MNRAS.218..393D

Abstract

Observations of the supernova remnant W50, which contains SS 433, have been made at 5 GHz with the Effelsberg 100-m telescope. These are combined with previous results at 1.7 and 2.7 GHz to investigate the intrinsic linear polarization and the variation of spectral index across the source. The spectrum of W50 is typical for old shell remnants and shows no evidence for the injection of flat spectrum fast particles from SS 433. If such injection occurs, it must either be modest or be of particles with a steep energy spectrum. The northern boundary of the remnant is bright and has a slightly flatter spectrum (alpha of about 0.4). The polarization there is strong (up to 50 percent of the total intensity). The magnetic field direction, where it can be deduced, is tangential to the shell. The bright northern edge appears to be a typical example of compression of a large-scale interstellar magnetic field. The shell of W50 has bright regions which coincide with the position angles of the precession cone of the jets from SS 433, seen in projection.

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