Multi-frequency polarimetry of the Galactic radio background around 350 MHz: II. A region in Horologium around l = 137, b = 7

Details Multi-frequency polarimetry of the Galactic radio background around 350 MHz: II. A region in Horologium around l = 137, b = 7 Multi-frequency polarimetry of the Galactic radio background around 350 MHz: II. A region in Horologium around l = 137, b = 7

2003-04-04

arxiv.org/abs/astro-ph/0304087v1

Astron.Astrophys. 404 (2003) 233-248

Astronomy and Astrophysics

Astrophysics

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

Scientific paper

10.1051/0004-6361:20030530

We study a conspicuous ring-like structure with a radius of about 1.4 degrees which was observed with the Westerbork Synthesis Radio Telescope (WSRT) at 5 frequencies around 350 MHz. This ring is very prominent in Stokes Q and U, and less so in polarized intensity P. No corresponding structure is visible in total intensity Stokes I, which indicates that the ring is created by Faraday rotation and depolarization processes. The polarization angle changes regularly from the center of the ring outwards to a radius of more than 1.7 degrees. Thus, the structure in polarization angle is not ring-like but resembles a disk, and it is larger than the ring in P. The rotation measure (RM) decreases almost continuously over the disk, from RM = 0 rad/m2 at the edge, to -8 rad/m2 in the center, while outside the ring the RM is slightly positive. This radial variation of RM yields stringent constraints on the nature of the ring-like structure, because it rules out any spherically symmetrical magnetic field configuration, such as might be expected from supernova remnants or wind-blown bubbles. We discuss several possible connections between the ring and known objects in the ISM, and conclude that the ring is a predominantly magnetic funnel-like structure. This description can explain both the field reversal from outside to inside the ring, and the increase in magnitude of RM towards the center of the ring. The ring-structure in P is most likely caused by a lack of depolarization due to a very uniform RM distribution at that radius. Beyond the ring, the RM gradient increases, depolarizing the polarized emission, so that P decreases. In the SW corner of the field a pattern of narrow filaments of low polarization, aligned with Galactic longitude, is observed, indicative of beam depolarization due to abrupt changes in RM.

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