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We aim to explore whether strong magnetic fields can be effectively generatedin low-mass dwarf galaxies and, if so, whether such fields can be affected bygalactic outflows and spread out into the intergalactic medium (IGM). Weperformed a radio continuum polarimetry study of IC10, the nearest starburstingdwarf galaxy, using a combination of multifrequency interferometric (VLA) andsingle-dish (Effelsberg) observations. VLA observations at 1.43 GHz reveal anextensive and almost spherical radio halo of IC10 in total intensity, extendingtwice more than the infrared-emitting galactic disk. The halo is magnetizedwith a magnetic field strength of 7 microG in the outermost parts. Locally, themagnetic field reaches about 29 microG in HII complexes, becomes more ordered,and weakens to 22 microG in the synchrotron superbubble and to 7-10 microGwithin HI holes. At the higher frequency of 4.86 GHz, we found a large-scalemagnetic field structure of X-shaped morphology, similar to that observed inseveral edge-on spiral galaxies. The X-shaped magnetic structure can be causedby the galactic wind, advecting magnetic fields injected into the interstellarmedium by stellar winds and supernova explosions. The radio continuum scaleheights at 1.43 GHz indicate the bulk speed of cosmic-ray electrons outflowingfrom HII complexes of about 60 km/s, exceeding the escape velocity of 40 km/s.Hence, the magnetized galactic wind in IC10 inflates the extensive radio halovisible at 1.43 GHz and can seed the IGM with both random and ordered magneticfields. These are signatures of intense material feedback onto the IGM,expected to be prevalent in the protogalaxies of the early Universe.

The magnetized galactic wind and synchrotron halo of the starburst dwarf galaxy IC10