Probe of the magnetic field structure in and around the supernova remnant OA 184 (G166.2 + 2.5) using background radio source rotation measures

Details Probe of the magnetic field structure in and around the supernova remnant OA 184 (G166.2 + 2.5) using background radio source rotation measures Probe of the magnetic field structure in and around the supernova remnant OA 184 (G166.2 + 2.5) using background radio source rotation measures

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988aj.....96..704k&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 96, Aug. 1988, p. 704-717. Research supported by the University of Toronto and NSERC

Astronomy and Astrophysics

Astronomy

5

Interstellar Magnetic Fields, Magnetic Field Configurations, Radio Sources (Astronomy), Stellar Magnetic Fields, Supernova Remnants, Data Reduction, Error Analysis, Galactic Radiation, Very Large Array (Vla)

Scientific paper

The authors describe the results of an attempt to probe the magneto-ionic strength of the supernova remnant OA 184 (G 166.2+2.5) by measuring the Faraday rotation measures (RMs) of background radio sources in the field. The sources seen through the SNR have significantly higher RM than nearby background sources. There is tentative evidence for a systematic sign "flip" of the RMs within and/or around the SNR. The background RMs are consistent with an interstellar magnetic irregularity scale of order 100 pc, rather than ≡10 pc; the relatively low "background galactic RM" at the position of OA 184 makes this region better suited than most for probing the magnetic-irregularity scale in the galactic disk. Comparison of the incidence of linear polarization of this (low-latitude) sample with a similar independent VLA polarimetric survey of high-latitude sources near the Coma cluster shows no significant difference. This indicates that there is no significant galactic depolarization for these extragalactic source populations in the outer galactic plane.

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