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The magnetized galactic wind and synchrotron halo of the starburst dwarf galaxy IC 10

The magnetized galactic wind and synchrotron halo ...

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dc.contributor.author Chyży, Krzysztof [SAP11011785] pl
dc.contributor.author Drzazga, Robert [USOS29124] pl
dc.contributor.author Beck, Rainer pl
dc.contributor.author Urbanik, Marek [SAP11005004] pl
dc.contributor.author Heesen, Volker pl
dc.contributor.author Bomans, Dominik J. pl
dc.date.accessioned 2016-06-29T11:22:14Z
dc.date.available 2016-06-29T11:22:14Z
dc.date.issued 2016 pl
dc.identifier.issn 0004-637X pl
dc.identifier.uri http://ruj.uj.edu.pl/xmlui/handle/item/28463
dc.language eng pl
dc.rights Dodaję tylko opis bibliograficzny *
dc.rights.uri *
dc.title The magnetized galactic wind and synchrotron halo of the starburst dwarf galaxy IC 10 pl
dc.type JournalArticle pl
dc.abstract.en We aim to explore whether strong magnetic fields can be effectively generated in low-mass dwarf galaxies and, if so, whether such fields can be affected by galactic outflows and spread out into the intergalactic medium (IGM). We performed a radio continuum polarimetry study of IC 10, the nearest starbursting dwarf galaxy, using a combination of multifrequency interferometric (VLA) and single-dish (Effelsberg) observations. VLA observations at 1.43 GHz reveal an extensive and almost spherical radio halo of IC 10 in total intensity, extending twice more than the infrared-emitting galactic disk. The halo is magnetized with a magnetic field strength of 7 \muG in the outermost parts. Locally, the magnetic field reaches about 29 \mu {{G}} in H ii complexes, becomes more ordered, and weakens to 22 \mu {{G}} in the synchrotron superbubble and to 7–10 \muG within H i holes. At the higher frequency of 4.86 GHz, we found a large-scale magnetic field structure of X-shaped morphology, similar to that observed in several edge-on spiral galaxies. The X-shaped magnetic structure can be caused by the galactic wind, advecting magnetic fields injected into the interstellar medium by stellar winds and supernova explosions. The radio continuum scale heights at 1.43 GHz indicate the bulk speed of cosmic-ray electrons outflowing from H ii complexes of about 60 km s^{-1}, exceeding the escape velocity of 40 km s^{-1}. Hence, the magnetized galactic wind in IC 10 inflates the extensive radio halo visible at 1.43 GHz and can seed the IGM with both random and ordered magnetic fields. These are signatures of intense material feedback onto the IGM, expected to be prevalent in the protogalaxies of the early universe. pl
dc.subject.en galaxies: dwarf pl
dc.subject.en galaxies: evolution pl
dc.subject.en galaxies: irregular pl
dc.subject.en galaxies: magnetic fields pl
dc.subject.en Local Group pl
dc.subject.en radio continuum: galaxies pl
dc.description.volume 819 pl
dc.description.number 1 pl
dc.identifier.doi 10.3847/0004-637X/819/1/39 pl
dc.identifier.eissn 1538-4357 pl
dc.title.journal The Astrophysical Journal pl
dc.language.container eng pl
dc.affiliation Wydział Fizyki, Astronomii i Informatyki Stosowanej : Instytut – Obserwatorium Astronomiczne pl
dc.subtype Article pl
dc.identifier.articleid 39 pl
dc.rights.original OTHER; inne; ostateczna wersja wydawcy; po opublikowaniu; 12 pl
dc.identifier.project 2011/03/B/ST9/01859 pl
dc.identifier.project 2012/07/B/ST9/04404 pl
dc.identifier.project ST/J001600/1 pl
.pointsMNiSW [2016 A]: 40


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