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Holmberg II - a dwarf galaxy in the nearby M81 group - is a very informativesource of distribution of gas and dust in the interstellar discs.High-resolution observations in the infrared (IR) allows us to distinguishisolated star-forming regions, photodissociation (PDR) and HII regions,remnants of supernovae (SNe) explosions and, as such, can provide informationabout more relevant physical processes. In this paper we analyse dust emissionin the wavelength range 4.5 to 160 micron using the data from IR spaceobservatories at 27 different locations across the galaxy. We observe that thederived spectra can be represented by multiple dust populations with differenttemperatures, which are found to be independent of their locations in thegalaxy. By comparing the dust temperatures with the far ultraviolet (FUV)intensities observed by the UVIT instrument onboard AstroSat, we find that forlocations showing a 100 micron peak, the temperature of cold (20 to 30 K) dustgrains show a dependence on the FUV intensities, while such dependence is notobserved for the other locations. We believe that the approach described herecan be a good tool in revealing different dust populations in other nearbygalaxies with available high spatial resolution data.

Unravelling multi-temperature dust populations in the dwarf galaxy Holmberg II