Open AccessThe magnetic field structure of SNR G328.4+0.2 from polarimetric observations at 19 GHz
Author(s) -
Johnston Simon,
McClureGriffiths N. M.,
Koribalski Bärbel
Publication year - 2004
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.07526.x
Subject(s) - physics , polarimetry , magnetic field , astronomy , polarization (electrochemistry) , remote sensing , field (mathematics) , astrophysics , computational physics , optics , scattering , chemistry , quantum mechanics , mathematics , pure mathematics , geology
We report on the first polarimetric observations at 19 GHz made with the upgraded Australia Telescope Compact Array. Observations were made of the Galactic supernova remnant (SNR) G328.8+0.2. We find the SNR has circular morphology with a strong central bar, similar to that seen at lower frequencies. The SNR has high linear polarization throughout, with fractional polarization in the bar up to 50 per cent. The orientation of the magnetic field lines follow the filamentary structure of the SNR. The magnetic field at the edge of the SNR is generally toroidal, interspersed with radial fingers, likely caused by Rayleigh–Taylor instabilities. Although the SNR has been identified as Crab‐like, we prefer an interpretation in which the bar is a pulsar‐powered wind nebula with the rest of the SNR consisting of the shell. The proposed pulsar parameters make the SNR/pulsar system more like SNR G11.2–0.3 than the Crab Nebula.