WSRT Faraday tomography of the Galactic ISM at λ\sim 0.86 m

Abstract

We investigate the distribution and properties of Faraday rotating and synchrotron emitting regions in the Galactic ISM in the direction of the Galactic anti-centre. We apply Faraday tomography to a radio polarization dataset that we obtained with the WSRT. We developed a new method to calculate a linear fit to periodic data, which we use to determine rotation measures from our polarization angle data. From simulations of a Faraday screen + noise we could determine how compatible the data are with Faraday screens. An unexpectedly large fraction of 14% of the lines-of-sight in our dataset show an unresolved main component in the Faraday depth spectrum. For lines-of-sight with a single unresolved component we demonstrate that a Faraday screen in front of a synchrotron emitting region that contains a turbulent magnetic field component can explain the data.

5 pages, 5 figures. Accepted for publication as a Letter to the Editor in A&A

References in corpus (2)

• Magnetic Field Structure from Synchrotron Polarization
• The WENSS and Dwingeloo surveys and the Galactic magnetic field

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