Multi-frequency polarimetry of the Galactic radio background around 350 MHz: I. A region in Auriga around l = 161, b = 16

Details Multi-frequency polarimetry of the Galactic radio background around 350 MHz: I. A region in Auriga around l = 161, b = 16 Multi-frequency polarimetry of the Galactic radio background around 350 MHz: I. A region in Auriga around l = 161, b = 16

2003-03-26

arxiv.org/abs/astro-ph/0303575v1

Astron.Astrophys.403:1031-1044,2003

Astronomy and Astrophysics

Astrophysics

15 pages, 14 figures, to be published in A&A

Scientific paper

10.1051/0004-6361:20030432

With the Westerbork Synthesis Radio Telescope (WSRT), multi-frequency polarimetric images were taken of the diffuse radio synchrotron background in a region centered on (l,b) = (161,16). The observations were done simultaneously in 5 frequency bands from 341 MHz to 375 MHz, with 5 arcmin resolution. Ubiquitous structure on arcminute and degree scales in the polarized intensity and polarization angle, combined with no observed structure in total intensity, indicates that the structure in the polarized radiation must be due to Faraday rotation and depolarization mostly in the warm nearby Galactic interstellar medium (ISM). Beam depolarization most likely creates "depolarization canals" of one beam wide, while depth depolarization is responsible for creating most of the structure on scales larger than a beam width. Rotation measures RM are in the range -17 < RM < 10 rad/m2 with a non-zero average of about -3.4 rad/m2. The gradient and average RM are consistent with a regular magnetic field of about 1 uG which has a pitch angle of p = -14 degrees. 13 Extragalactic sources in the field have |RM| < 13 rad/m2, with an estimated intrinsic source contribution of 3.6 rad/m2. The RMs of the extragalactic sources show a gradient (with a sign reversal) that is about 3 times larger than the gradient in the RMs of the diffuse emission, and that is approximately in Galactic latitude. This difference is ascribed to a vastly different effective length of the line of sight. The observations are interpreted in terms of a single-cell-size model of the warm ISM which contains gas and magnetic fields, with a polarized background.

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