  A correlation between the 24 {\mu}m continuum and the [NII] 205 {\mu}m line
emission may arise if both quantities trace the star formation activity on
spatially-resolved scales within a galaxy, yet has so far only been observed in
the 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 an
artefact of line-of-sight projection effects in an edge-on disc. We search for
the presence of a correlation in Herschel and Spitzer observations of two
nearby face-on galaxies, M51 and M83, and the interacting Antennae galaxies NGC
4038 and 4039. We show that not only is this empirical relationship also
observed in face-on galaxies, but also that the correlation appears to be
governed by the star formation rate (SFR). Both the nuclear starburst in M83
and the merger-induced star formation in NGC 4038/9 exhibit less [NII] emission
per unit SFR surface density than the normal star-forming discs. These regions
of intense star formation exhibit stronger ionization parameters, as traced by
the 70/160 {\mu}m far-infrared colour, that suggest the presence of higher
ionization lines that may become more important for gas cooling, thereby
reducing the observed [NII] 205 {\mu}m line emission in regions with higher
star 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 including
observations with wider spatial coverage for a larger sample of galaxies.
