Z$_{\odot}$), SMC (60 kpc, 1/5 Z$_{\odot}$), NGC6822 (500 kpc, 1/4 Z$_{\odot}$), or IC10 (800 kpc, 1/3 Z$_{\odot}$), the phases of the ISM are mixed together in single telescope beams. When using a limited number of diagnostic lines, only a single galactic component can be modeled and average conditions derived, which is otherwise an ensemble of individual PDRs, ionised regions, etc. This requires modeling a comprehensive suit of tracers covering a range of critical densities and excitation potentials to characterise the dense H [ii]{} regions, the diffuse H [ii]{} regions, PDRs, etc. self-consistently. This approach allow us to grapple with degeneracies and ambiguities in the interpretation of these tracers. In this way, valuable observational diagnostics can be turned into a more accurate description of the multi-phase configuration of a full galaxy.

The [*Herschel*]{} Space Observatory [@pilbratt-2010] has brought the opportunity to obtain a wide range of valuable FIR fine-structure diagnostics never observed before in dwarf galaxies. The Dwarf Galaxy Survey (DGS; P.I. Madden) is surveying the dust and gas of a wide range of low metallicity galaxies in the local universe [@cormier-2010; @galametz-2010; @o'halloran-2010; @madden-2012b; @remy-2012] using PACS [@poglitsch-2010] and SPIRE [@griffin-2010]. The brightest low-metallicity galaxy of the DGS observed with 