metal-rich star-forming galaxies. In low metallicity dwarf galaxies, where CO(1-0) is not easily detected [e.g. @schruba-2012; @leroy-2011], \[C [ii]{}\] can be as high as 1% of the L$\rm{_{FIR}}$ and often 5 to 10 times brighter relative to CO than in dustier starburst galaxies [e.g. @poglitsch-1995; @madden-1995; @madden-2000; @hunter-2001; @cormier-2010]. The high \[C [ii]{}\]/CO(1-0) ratio in low-metallicity systems may be alerting us to the fact that the morphology of their PDRs and H [ii]{} regions and the relative filling factors of the various phases of dwarf galaxies differ from those of more metal-rich objects [e.g. @madden-2000; @kaufman-2006; @roellig-2006]. Even in the nearest neighboring dwarf galaxies, the picture of star formation – and what controls this star formation – is enigmatic.

However, using \[C [ii]{}\] alone can lead to ambiguous interpretation, particularly on the origin of the C$^+$ emission, which can arise from the ionised as well as neutral phases of the ISM. To employ the \[C [ii]{}\] line as a valuable star formation tracer, it is necessary to model the different phases on galaxy-wide scales. The challenge rests on the unavoidable fact that on the scale of galaxies, aside from the closest dwarf galaxies such as the LMC (50 kpc, 1/2 