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We performed observations of NGC1569 for 6 infrared bands (3.2, 4.1, 7, 11,15, and 24 micron) with the Infrared Camera (IRC) onboard AKARI. Near- tomid-infrared (2--13 micron) spectroscopy of a Halpha filament was also carriedout with the IRC.  The extended structure associated with a Halpha filament appears bright at 7micron, suggesting that the filament is bright at the UIR band emission.Follow-up spectroscopic observations with the IRC confirm the presence of 6.2,7.7, and 11.3 micron emission in the filament. The filament spectrum exhibitsstrong 11.3 micron UIR band emission relative to the 7.7 micron band comparedto the galaxy disk observed with the Infrared Spectrograph on Spitzer. Thenear-infrared spectrum also suggests the presence of excess continuum emissionin 2.5--5 micron in the filament.  The Halpha filament is thought to have been formed by the galactic outfloworiginating from the star-formation activity in the disk of NGC1569. Thedestruction timescale of the UIR band carriers in the outflow is estimated tobe much shorter (~ 1.3 x 10^3 yr) than the timescale of the outflow (~ 5.3Myr). Thus it is unlikely that the band carriers survive the outflowenvironment. Alternatively, we suggest that the band carriers in the filamentsmay be produced by the fragmentation of large carbonaceous grains in shocks,which produces the Halpha emission. The NIR excess continuum emission cannot beaccounted for by free-free emission alone and a hot dust contribution may beneeded, although the free-free emission intensity estimated from HIrecombination lines has a large uncertainty.

Detection of unidentified infrared bands in a Halpha filament in the dwarf galaxy NGC1569 with AKARI