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• W3104396985 abstract "Context. We study the λ 158 μm [CII] fine-structure line emission from star-forming regions as a function of metallicity. Aims. We have measured and mapped the [CII] emission from the very bright HII region complexes N 11 in the LMC and N 66 in the SMC; as well as the SMC HII regions N 25, N 27, N 83/N 84, and N 88 with the FIFI instrument on the Kuiper Airborne Observatory. Methods. In both LMC and SMC, the ratio of [CII] line to CO line and to the far-infrared continuum emission is much higher than seen almost anywhere else, including Milky Way star-forming regions, and whole galaxies. Results. In the low metallicity, low dust-abundance environment of the LMC and the SMC UV mean free path lengths are much greater than those in the higher-metallicity Milky Way. The increased photoelectric heating efficiencies cause significantly greater relative [CII] line emission strengths. At the same time, similar decreases in PAH abundances have the opposite effect by diminishing photoelectric heating rates. Consequently, in low-metallicity environments relative [CII] strengths are high but exhibit little further dependence on actual metallicity. Relative [CII] strengths are slightly higher in the LMC than in the SMC which has both lower dust and lower PAH abundances." @default.
• W3104396985 created "2020-11-23" @default.
• W3104396985 creator A5000008228 @default.
• W3104396985 creator A5080484613 @default.
• W3104396985 date "2011-07-01" @default.
• W3104396985 modified "2023-09-23" @default.
• W3104396985 title "C + emission from the Magellanic Clouds. II. [C II] maps of star-forming regions LMC-N 11, SMC-N 66, and several others" @default.
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• W3104396985 hasPublicationYear "2011" @default.
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