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A correlation between the 24 {\mu}m continuum and the [NII] 205 {\mu}m lineemission may arise if both quantities trace the star formation activity onspatially-resolved scales within a galaxy, yet has so far only been observed inthe nearby edge-on spiral galaxy NGC 891. We therefore assess whether the [NII]205 - 24 {\mu}m emission correlation has some physical origin or is merely anartefact of line-of-sight projection effects in an edge-on disc. We search forthe presence of a correlation in Herschel and Spitzer observations of twonearby face-on galaxies, M51 and M83, and the interacting Antennae galaxies NGC4038 and 4039. We show that not only is this empirical relationship alsoobserved in face-on galaxies, but also that the correlation appears to begoverned by the star formation rate (SFR). Both the nuclear starburst in M83and the merger-induced star formation in NGC 4038/9 exhibit less [NII] emissionper unit SFR surface density than the normal star-forming discs. These regionsof intense star formation exhibit stronger ionization parameters, as traced bythe 70/160 {\mu}m far-infrared colour, that suggest the presence of higherionization lines that may become more important for gas cooling, therebyreducing the observed [NII] 205 {\mu}m line emission in regions with higherstar formation rates. Finally, we present a general relation between the [NII]205 {\mu}m line flux density and SFR density for normal star-forming galaxies,yet note that future studies should extend this analysis by includingobservations with wider spatial coverage for a larger sample of galaxies.

The spatially-resolved correlation between [NII] 205 {\mu}m line emission and the 24 {\mu}m continuum in nearby galaxies