FROM GAS TO STARS IN ENERGETIC ENVIRONMENTS: DENSE GAS CLUMPS IN THE 30 DORADUS REGION WITHIN THE LARGE MAGELLANIC CLOUD
FROM GAS TO STARS IN ENERGETIC ENVIRONMENTS: DENSE GAS CLUMPS IN THE 30 DORADUS REGION WITHIN THE LARGE MAGELLANIC CLOUD
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从气体到高能环境中的恒星：大麦哲伦星云内 30 DORADUS 区域的致密气体团块
DOI：
10.1088/0004-637x/793/1/37
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发表时间：
2012
期刊：
影响因子：
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通讯作者：
J. Seale
中科院分区：
文献类型：
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作者：
C. Anderson;D. Meier;J. Ott;A. Hughes;T. Wong;C. Henkel;R. Chen;R. Indebetouw;L. Looney;E. Muller;J. Pineda;J. Seale
我们提出了秒差距尺度的HCN（1-0）和HCO+（1-0）从恒星形成区30剑鱼座，获得使用澳大利亚望远镜紧凑阵列的致密气体排放的干涉图。这个位于大麦哲伦星云（LMC）的极端恒星形成区域的特征是非常强烈的紫外线电离辐射场和太阳下的金属丰度，预计这两者都会影响分子云结构。我们在剑鱼座30 -10巨型分子云中探测到13个明亮、密集的团块。一些团块沿着具有特征间距的沉积结构排列，该特征间距与通过静脉曲张流体不稳定性形成的一致。我们的分析表明，暗条引力不稳定，坍缩形成恒星。暗条中的HCO+发射与最近的星星形成活动（包括H2O脉泽和年轻恒星天体（YSO））的特征之间有很好的相关性。YSO似乎继续沿着沿着同一方向的暗条朝着西南方向的大质量致密星星星团R136移动。我们详细比较了30 Dor-10与大麦哲伦星云其他星星形成区（N159、N113、N105和N44）的团块性质（质量、线宽和大小）。我们的分析表明，30 Dor-1 - 0团块具有类似的质量，但更宽的线宽和类似的HCN/HCO+（1-0）线比在其他LMC恒星形成区检测到的团块。我们的研究结果表明，致密的分子气体团在30 Dor-10的内部被很好地屏蔽了强烈的电离场，这是在30 Doradus地区。
We present parsec-scale interferometric maps of HCN(1–0) and HCO+(1–0) emission from dense gas in the star-forming region 30 Doradus, obtained using the Australia Telescope Compact Array. This extreme star-forming region, located in the Large Magellanic Cloud (LMC), is characterized by a very intense ultraviolet ionizing radiation field and sub-solar metallicity, both of which are expected to impact molecular cloud structure. We detect 13 bright, dense clumps within the 30 Doradus-10 giant molecular cloud. Some of the clumps are aligned along a filamentary structure with a characteristic spacing that is consistent with formation via varicose fluid instability. Our analysis shows that the filament is gravitationally unstable and collapsing to form stars. There is a good correlation between HCO+ emission in the filament and signatures of recent star formation activity including H2O masers and young stellar objects (YSOs). YSOs seem to continue along the same direction of the filament toward the massive compact star cluster R136 in the southwest. We present detailed comparisons of clump properties (masses, linewidths, and sizes) in 30Dor-10 to those in other star forming regions of the LMC (N159, N113, N105, and N44). Our analysis shows that the 30Dor-10 clumps have similar masses but wider linewidths and similar HCN/HCO+ (1–0) line ratios as clumps detected in other LMC star-forming regions. Our results suggest that the dense molecular gas clumps in the interior of 30Dor-10 are well shielded against the intense ionizing field that is present in the 30Doradus region.