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This study explores the link between the [OIII]88mu emission, a well-knowntracer of HII regions, and 24mu continuum, often used to trace warm dust in theionized phases of galaxies. We investigate the local conditions driving therelation between those tracers in the Magellanic Clouds, comparing observationswith Cloudy models consisting of an HII region plus a photodissociation region(PDR) component, varying the stellar age, the initial density (at theilluminated edge of the cloud), and the ionization parameter. We introduce anew parameter, cPDR, to quantify the proportion of emission arising from PDRsand that with an origin in HII regions along each line of sight. We use theratio ([CII]+[OI])/[OIII] as a proxy for the ratio of PDR versus HII regionemission, and compare it to [OIII]/24mu. The use of [OIII]/24mu and [OIII]/70mutogether allows us to constrain the models most efficiently. We find acorrelation over at least 3 orders of magnitude in [OIII]88mu and 24mucontinuum in spatially resolved maps of the Magellanic Cloud regions as well asunresolved galaxy-wide low metallicity galaxies of the Dwarf Galaxy Survey.Most of the regions have low proportions of PDRs along the lines of sight (<12%), while a limited area of some of the mapped regions can reach 30 to 50%.For most lines of sight within the star-forming regions we have studied in theMagellanic Clouds, HII regions are the dominant phase. We propose the use ofthe correlation between the [OIII]88mu and 24mu continuum as a new predictivetool to estimate, for example, the [OIII]88mu emission when the 24mu continuumis available or inversely. This can be useful to prepare for ALMA observationsof [OIII]88mu in high-z galaxies. This simple and novel method may also providea way to disentangle different phases along the line of sight, when other 3Dinformation is not available.

Disentangling emission from star-forming regions in the Magellanic Clouds: Linking [OIII]88 micron and 24 micron