麦哲伦星云II的C+辐射。[CII]恒星形成区LMC-N 11、SMC-N 66和其他几个恒星形成区的地图
C+ Emission from the Magellanic Clouds II. [CII] maps of star-forming regions LMC-N 11, SMC-N 66, and several others
摘要：
我们研究了来自恒星形成区域的158微米[CII]精细结构线发射与金属丰度的函数关系。我们用Kuiper机载天文台的FIFI仪器对LMC中非常明亮的HII区复合体N11和SMC中的N66以及SMC HII区N25、N27、N83/N84和N88的[CII]发射进行了测量和绘图。在LMC和SMC中，[CII]线与CO线和远红外连续辐射的比率比几乎任何其他地方都要高得多，包括银河系恒星形成区域和整个星系。在低金属丰度、低尘埃丰度的LMC和SMC环境中，UV平均自由程长度远大于高金属丰度的银河系。增加的光电加热效率导致显著更大的相对[CII]线发射强度。与此同时，PAH丰度的类似减少具有相反的效果，通过减少光电加热速率。因此，在低金属丰度环境中，相对[CII]强度很高，但对实际金属丰度的依赖性很小。相对[CII]强度略高于在LMC比SMC，其中既有较低的灰尘和较低的PAH丰度。
英文摘要：
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.
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