Abstract
We present preliminary results of recently obtained observations of the important cooling line of singly ionized carbon in the Magellanic Clouds. Three LMC and six HII region/CO cloud complexes have been detected and mapped. Comparison shows that the strength and distribution of [CII] regions is well-correlated with those of dust complexes emitting far-infrared radiation, but not with molecular cloud complexes traced by CO emission. The results confirm that photo-dissociation processes are of relatively greater importance in Magellanic Cloud star formation regions than in Galactic regions.
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Israel, F.P., Maloney, P.R. (1993). Ionized carbon [CII] in the Magellanic Clouds. In: Baschek, B., Klare, G., Lequeux, J. (eds) New Aspects of Magellanic Cloud Research. Lecture Notes in Physics, vol 416. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-56432-2_164
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DOI: https://doi.org/10.1007/3-540-56432-2_164
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