%0 Generic %1 Israel2011 %A Israel, F. P. %A Maloney, P. R. %D 2011 %K HIIregion [CII] %T C+ Emission from the Magellanic Clouds II. CII maps of star-forming regions LMC-N 11, SMC-N 66, and several others %U http://arxiv.org/abs/1104.2047 %X We study the 158 micron CII fine-structure line emission from star-forming regions 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 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. In both the LMC and SMC, the ratio of the CII line to the 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. 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 the 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.

@misc{Israel2011, abstract = { We study the 158 micron [CII] fine-structure line emission from star-forming regions 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 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. In both the LMC and SMC, the ratio of the [CII] line to the 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. 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 the 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. }, added-at = {2011-04-13T07:49:49.000+0200}, author = {Israel, F. P. and Maloney, P. R.}, biburl = {https://www.bibsonomy.org/bibtex/21605a7ed5bb9a44c8b18366def68b2a2/miki}, description = {[1104.2047] C+ Emission from the Magellanic Clouds II. [CII] maps of star-forming regions LMC-N 11, SMC-N 66, and several others}, interhash = {50be1d04022c40ff0a4176d07609a8c0}, intrahash = {1605a7ed5bb9a44c8b18366def68b2a2}, keywords = {HIIregion [CII]}, note = {cite arxiv:1104.2047 Comment: To appear in Astronomy & Astrophysics}, timestamp = {2011-04-13T07:49:49.000+0200}, title = {C+ Emission from the Magellanic Clouds II. [CII] maps of star-forming regions LMC-N 11, SMC-N 66, and several others}, url = {http://arxiv.org/abs/1104.2047}, year = 2011 }