  We have carried out a detailed modeling of the dust Spectral Energy
Distribution (SED) of the nearby, starbursting dwarf galaxy NGC 4214. A key
point of our modeling is that we distinguish the emission from (i) HII regions
and their associated photodissociation regions (PDRs) and (ii) diffuse dust.
For both components we apply templates from the literature calculated with a
realistic geometry and including radiation transfer. The large amount of
existing data from the ultraviolet (UV) to the radio allows the direct
measurement of most of the input parameters of the models. We achieve a good
fit for the total dust SED of NGC 4214. In the present contribution we describe
the available data, the data reduction and the determination of the model
parameters, whereas a description of the general outline of our work is
presented in the contribution of Lisenfeld et al. in this volume.
