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5 GHz EVN Polarization of 3C286

Published online by Cambridge University Press:  25 May 2016

D. Dallacasa ,
R.T. Schilizzi ,
H.S. Sanghera ,
D.R. Jiang ,
E. Lüdke  and
W.D. Cotton
D. Dallacasa
Affiliation:
Joint Institute for VLBI in Europe, Dwingeloo, NL Shanghai Observatory, Chinese Academy of Sciences, China Universidade Federal de Santa Maria, Santa Maria, Brazil National Radio Astronomy Observatory, Charlottesville, USA
R.T. Schilizzi
Affiliation:
Joint Institute for VLBI in Europe, Dwingeloo, NL Shanghai Observatory, Chinese Academy of Sciences, China Universidade Federal de Santa Maria, Santa Maria, Brazil National Radio Astronomy Observatory, Charlottesville, USA
H.S. Sanghera
Affiliation:
Joint Institute for VLBI in Europe, Dwingeloo, NL Shanghai Observatory, Chinese Academy of Sciences, China Universidade Federal de Santa Maria, Santa Maria, Brazil National Radio Astronomy Observatory, Charlottesville, USA
D.R. Jiang
Affiliation:
Joint Institute for VLBI in Europe, Dwingeloo, NL Shanghai Observatory, Chinese Academy of Sciences, China Universidade Federal de Santa Maria, Santa Maria, Brazil National Radio Astronomy Observatory, Charlottesville, USA
E. Lüdke
Affiliation:
Joint Institute for VLBI in Europe, Dwingeloo, NL Shanghai Observatory, Chinese Academy of Sciences, China Universidade Federal de Santa Maria, Santa Maria, Brazil National Radio Astronomy Observatory, Charlottesville, USA
W.D. Cotton
Affiliation:
Joint Institute for VLBI in Europe, Dwingeloo, NL Shanghai Observatory, Chinese Academy of Sciences, China Universidade Federal de Santa Maria, Santa Maria, Brazil National Radio Astronomy Observatory, Charlottesville, USA

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3C286 (1328+307) is a powerful radio source identified with a quasar at z=0.849. There is a foreground galaxy responsible for an H I absorption line system at z=0.6922 (Brown & Roberts 1973), centered approximately 2.″5 to the southeast of 3C286. The radio source has a steep spectrum (α = −0.61, Sv ∝ vα between 1.4 and 15 GHz) which turns over at about 100 MHz. Subarcsecond resolution radio images show a misaligned triple structure, dominated by the central component (Spencer et al. 1989) which accounts for at least 95% of the total flux density at all frequencies. 3C286 is one of the strongest extragalactic sources in polarized emission (0.84 Jy at 5 GHz and 1.41 Jy at 1.4 GHz) and with a rotation measure close to 0 rad m–2 (Rudnick and Jones 1983). Hence the observed orientation of the electric field vector is essentially independent of frequency.

Type
Properties of Radio Sources
Information
Symposium - International Astronomical Union , Volume 175: Extragalactic Radio Sources , 1996 , pp. 85 - 87
Copyright
Copyright © Kluwer 1996 

References

Brown, R.L., Roberts, M.S., 1973, ApJ , 184, 7.Google Scholar
Cawthorne, T.V., et al., 1993, ApJ , 416, 519.Google Scholar
Dallacasa, D., et al. 1995, A&A , 299, 671.Google Scholar
Fernini, I., et al., 1993, AJ , 105, 1690.Google Scholar
Laing, R., 1988, in Hot Spots in Extragalactic Radio Sources, Meisenheimer, K. and Roser, H.J. eds., p.27.Google Scholar
Meisenheimer, K., et al. 1989, A&A , 219, 63.Google Scholar
Phillips, R.B., Shaffer, D.B., ApJ , 271, 32.CrossRefGoogle Scholar
Rudnick, L., Jones, T.W., 1983, AJ , 88, 518.Google Scholar
Spencer, R.E., et al. 1989, MNRAS , 240, 657.Google Scholar
Spencer, R.E., et al. 1991, MNRAS , 250, 225.Google Scholar
Zhang, F.J., et al., 1994, A&A , 281, 649.Google Scholar