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More complete knowledge of galaxy evolution requires understanding theprocess of star formation and interaction between the interstellar radiationfield and the interstellar medium in galactic environments traversing a widerange of physical parameter space. Here we focus on the impact of massive starformation on the surrounding low metallicity ISM in 30 Doradus in the LargeMagellanic Cloud. A low metal abundance, as is the case of some galaxies of theearly universe, results in less ultra-violet shielding for the formation of themolecular gas necessary for star formation to proceed. The half-solarmetallicity gas in this region is strongly irradiated by the super star clusterR136, making it an ideal laboratory to study the structure of the ISM in anextreme environment. Our spatially resolved study investigates the gas heatingand cooling mechanisms, particularly in the photo-dissociation regions wherethe chemistry and thermal balance are regulated by far-ultraviolet photons (6eV< h\nu <13.6 eV).  We present Herschel observations of far-infrared fine-structure linesobtained with PACS and SPIRE/FTS. We have combined atomic fine-structure linesfrom Herschel and Spitzer observations with ground-based CO data to providediagnostics on the properties and the structure of the gas by modeling it withthe Meudon PDR code. We derive the spatial distribution of the radiation field,the pressure, the size, and the filling factor of the photodissociated gas andmolecular clouds. We find a range of pressure of ~ 10^5 - 1.7x10^6 cm^{-3} Kand a range of incident radiation field G_UV ~ 10^2 - 2.5x10^4 through PDRmodeling. Assuming a plane-parallel geometry and a uniform medium, we find atotal extinction of 1-3 mag , which correspond to a PDR cloud size of 0.2 to3pc, with small CO depth scale of 0.06 to 0.5pc. We also determine the threedimensional structure of the gas. (Abridged)

A milestone toward understanding PDR properties in the extreme environment of LMC-30Dor