We are modeling the spectra of dwarf galaxies from infrared to
submillimeter wavelengths to understand the nature of the various dust
components in low-metallicity environments, which may be comparable to the ISM
of galaxies in their early evolutionary state.
The overall nature of the dust in these environments appears to differ from
those of higher metallicity starbursting systems.
Here, we present a study of one of our sample of dwarf galaxies, NGC 1569,
which is a nearby, well-studied starbursting dwarf.
Using ISOCAM, IRAS, ISOPHOT and SCUBA data with the Désert
et al. (1990)  model, we find consistency with little contribution
from PAHs and Very Small Grains and a relative abundance of bigger colder
grains, which dominate the FIR and submillimeter wavelengths.
We are compelled to use 4 dust components, adding a very cold dust component,
to reproduce the submillimetre excess of our observations.