Radio Polarization from the Galactic Plane in Cygnus

Details Radio Polarization from the Galactic Plane in Cygnus Radio Polarization from the Galactic Plane in Cygnus

2002-11-19

arxiv.org/abs/astro-ph/0211436v1

Astrophys.J. 585 (2003) 785-800

Astronomy and Astrophysics

Astrophysics

31 pages, 13 jpg figures, Accepted for publication in The Astrophysical Journal

Scientific paper

10.1086/346234

We present 1420 MHz (lambda=21cm) observations of polarized emission from an area of 117 degree square in the Galactic plane in Cygnus, covering 82 < l < 95, -3.5 < b < +5.5, a complex region where the line of sight is directed nearly along the Local spiral arm. The angular resolution is ~ 1', and structures as large as 45' are fully represented in the images. Polarization features bear little resemblance to features detected in total power: while the polarized signal arises in diffuse Galactic synchrotron emission regions, the appearance of the polarized sky is dominated by Faraday rotation occurring in small-scale structure in the intervening Warm Ionized Medium. There is no concentration of polarization structure towards the Galactic plane, indicating that both the emission and Faraday rotation occur nearby. We develop a conceptual framework for interpretation of the observations. We can detect only that polarized emission which has its origin closer than the polarization horizon, at a distance d_ph; more distant polarized emission is undetectable because of depth depolarization (differential Faraday rotation) and/or beam depolarization (due to internal and external Faraday dispersion). d_ph depends on the instrument used (frequency and beamwidth) as well as the direction being studied. In our data we find that d_ph ~ 2 kpc, consistent with the polarization features originating in the Local arm.

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