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|Title:||The Fan Region at 1.5 GHz - I. Polarized synchrotron emission extending beyond the Perseus Arm||Authors:||Hill, A. S.
Landecker, T. L.
Sun, X. H.
Gaensler, B. M.
Mao, S. A.
McClure-Griffiths, N. M.
Dickey, J. M.
Gray, A. D.
Leahy, J. P.
Schnitzeler, D. H. F. M.
|Issue Date:||2017||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||467||Issue:||4||First Page:||4631||Abstract:||The Fan Region is one of the dominant features in the polarized radio sky, long thought to be a local (distance ≲500 pc) synchrotron feature. We present 1.3-1.8 GHz polarized radio continuum observations of the region from the Global Magneto-Ionic Medium Survey and compare them to maps of Hα and polarized radio continuum intensity from 0.408 to 353 GHz. The high-frequency (>1 GHz) and low-frequency (≲600 MHz) emissions have different morphologies, suggesting a different physical origin. Portions of the 1.5 GHz Fan Region emission are depolarized by ≈30 per cent by ionized gas structures in the Perseus Arm, indicating that this fraction of the emission originates ≳2 kpc away. We argue for the same conclusion based on the high polarization fraction at 1.5 GHz (≈40 per cent). The Fan Region is offset with respect to the Galactic plane, covering -5° ≲ b ≲ +10°; we attribute this offset to the warp in the outer Galaxy. We discuss origins of the polarized emission, including the spiral Galactic magnetic field. This idea is a plausible contributing factor although no model to date readily reproduces all of the observations. We conclude that models of the Galactic magnetic field should account for the ≳1 GHz emission from the Fan Region as a Galactic scale, not purely local, feature.||URI:||http://hdl.handle.net/20.500.12386/28638||URL:||https://academic.oup.com/mnras/article/467/4/4631/2998726||ISSN:||0035-8711||DOI:||10.1093/mnras/stx389||Bibcode ADS:||2017MNRAS.467.4631H||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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checked on Jun 19, 2021
checked on Jun 19, 2021
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