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We present a model for the interstellar medium of NGC4214 with the objectiveto probe the physical conditions in the two main star-forming regions and theirconnection with the star formation activity of the galaxy. We used the spectralsynthesis code Cloudy to model an HII region and the associatedphotodissociation region (PDR) to reproduce the emission of mid- andfar-infrared fine-structure cooling lines from the Spitzer and Herschel spacetelescopes for these two regions. Input parameters of the model, such aselemental abundances and star formation history, are guided by earlier studiesof the galaxy, and we investigated the effect of the mode in which starformation takes place (bursty or continuous) on the line emission. Furthermore,we tested the effect of adding pressure support with magnetic fields andturbulence on the line predictions. We find that this model can satisfactorilypredict (within a factor of ~2) all observed lines that originate from theionized medium ([SIV] 10.5um, [NeIII] 15.6um, [SIII] 18.7um, [SIII] 33.5um, and[OIII] 88um), with the exception of [NeII] 12.8um and [NII] 122um, which mayarise from a lower ionization medium. In the PDR, the [OI] 63um, [OI] 145um,and [CII] 157um lines are matched within a factor of ~5 and work better whenweak pressure support is added to the thermal pressure or when the PDR cloudsare placed farther away from the HII regions and have covering factors lowerthan unity. Our models of the HII region agree with different evolutionarystages found in previous studies, with a more evolved, diffuse central region,and a younger, more compact southern region. However, the local PDR conditionsare averaged out on the 175 pc scales that we probe and do not reflectdifferences observed in the star formation properties of the two regions.

Modeling the physical properties in the ISM of the low-metallicity galaxy NGC4214