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We discuss the interpretation of the dust SED from the mid-infrared to themillimeter range of NGC 1569. The model developed by D\'esert et al. (1990)including three dust components (Polyaromatic Hydrocarbons, Very Small Grainsand big grains) can explain the data using a realistic interstellar radiationfield and adopting an enhanced abundance of VSGs. A simple three-temperaturemodel is also able to reproduce the data but requires a very low dusttemperature which is considered to be unlikely in this low-metallicitystarburst galaxy. The high abundance of Very Small Grains might be due to largegrain destruction in supernova shocks. This possibility is supported by ISOdata showing that the emission at 14.3 $\mu$m, tracing VSGs, is enhanced withrespect to the emission at 6.7 $\mu$m and 850 $\mu$m in regions of high starformation.Comment: 4 pages, conference proceedings paper, "The Spectral Energy  Distribution of Gas-Rich Galaxies: Confronting Models with Data", Heidelberg,  4-8 Oct. 2004, eds. C.C. Popescu & R.J. Tuffs, AIP Conf. Ser., in pres

The dust SED in the dwarf galaxy NGC 1569: Indications for an altered dust composition?