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We study the 158 micron [CII] fine-structure line emission from star-formingregions as a function of metallicity. We have measured and mapped the [CII]emission from the very bright HII region complexes N 11 in the LMC and N 66 inthe SMC, as well as the SMC HII regions N 25, N 27, N 83/N 84, and N 88, withthe FIFI instrument on the Kuiper Airborne Observatory. In both the LMC andSMC, the ratio of the [CII] line to the CO line and to the far-infraredcontinuum emission is much higher than seen almost anywhere else, includingMilky Way star-forming regions and whole galaxies. In the low metallicity, lowdust-abundance environment of the LMC and the SMC, UV mean free path lengthsare much greater than those in the higher-metallicity Milky Way. The increasedphotoelectric heating efficiencies cause significantly greater relative [CII]line emission strengths. At the same time, similar decreases in PAH abundanceshave the opposite effect, by diminishing photoelectric heating rates.Consequently, in low-metallicity environments the relative [CII] strengths arehigh but exhibit little further dependence on actual metallicity. Relative[CII] strengths are slightly higher in the LMC than in the SMC, which has bothlower dust and lower PAH abundances.

C+ Emission from the Magellanic Clouds II. [CII] maps of star-forming regions LMC-N 11, SMC-N 66, and several others