Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/28638
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Hill, A. S. | en_US |
dc.contributor.author | Landecker, T. L. | en_US |
dc.contributor.author | CARRETTI, ETTORE | en_US |
dc.contributor.author | Douglas, K. | en_US |
dc.contributor.author | Sun, X. H. | en_US |
dc.contributor.author | Gaensler, B. M. | en_US |
dc.contributor.author | Mao, S. A. | en_US |
dc.contributor.author | McClure-Griffiths, N. M. | en_US |
dc.contributor.author | Reich, W. | en_US |
dc.contributor.author | Wolleben, M. | en_US |
dc.contributor.author | Dickey, J. M. | en_US |
dc.contributor.author | Gray, A. D. | en_US |
dc.contributor.author | Haverkorn, M. | en_US |
dc.contributor.author | Leahy, J. P. | en_US |
dc.contributor.author | Schnitzeler, D. H. F. M. | en_US |
dc.date.accessioned | 2020-12-03T11:00:18Z | - |
dc.date.available | 2020-12-03T11:00:18Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28638 | - |
dc.description.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. | en_US |
dc.language.iso | eng | en_US |
dc.title | The Fan Region at 1.5 GHz - I. Polarized synchrotron emission extending beyond the Perseus Arm | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stx389 | en_US |
dc.identifier.scopus | 2-s2.0-85032673901 | en_US |
dc.identifier.isi | 000398421100064 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/467/4/4631/2998726 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 467 | en_US |
dc.relation.issue | 4 | en_US |
dc.relation.firstpage | 4631 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017MNRAS.467.4631H | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.orcid | 0000-0002-3973-8403 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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stx389.pdf | Pdf editoriale | 10.97 MB | Adobe PDF | View/Open |
28638-stx389_P01.pdf | Miur | 6.27 MB | Adobe PDF | |
28638-stx389_P02.pdf | Miur | 4.78 MB | Adobe PDF |
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