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[CII] emission from the Magellanic Clouds

Published online by Cambridge University Press:  25 November 2011

M. Röllig ,
R. Simon ,
V. Ossenkopf ,
J. Stutzki ,
F.P. Israel  and
P.R. Maloney
F.P. Israel
Affiliation:
Sterrewacht Leiden, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands
P.R. Maloney
Affiliation:
CASA, University of Colorado, Boulder, CO 80303, USA
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Abstract

In the Magellanic Clouds, the [CII]/CO and the [CII]/FIR ratios are much higher than seen in Milky Way star-forming regions. The enhanced relative strength of the [CII] line reflects the physical environment characterised by the low metallicities, dust abundances, and PAH abundances of the LMC, and especially the SMC.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 52: Conditions and Impact of Star Formation , 2011 , pp. 287 - 288
Copyright
© EAS, EDP Sciences 2011

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References

Israel, F.P., et al., 1996, ApJ, 465, 738 CrossRef
Israel, F.P., & Maloney, P.R., 2010, A&A, submitted
Maloney, P.R., & Wolfire, M.G., 1997, in “CO: Twenty-Five Years of Millimeter-Wave Spectroscopy”, IAU Symp. 170, 299
Mochizuki, K., et al., 1994, ApJ, 430, L37 CrossRef
Poglitsch, A., et al., 1995, ApJ, 1995, 454, 293
Rubin, D., et al., 2009, A&A, 494, 647
Sandstrom, K.M., et al., 2010, ApJ, 715, 701CrossRef