赫歇尔革命：揭示LMC中高质量恒星形成点N44和N63的形态
The Herschel revolution: unveiling the morphology of the high mass star formation sites N44 and N63 in the LMC
摘要：
我们研究了高质量恒星形成地点周围介质的结构，以确定HII区域与它们形成的环境之间的相互关系。周围环境的密度分布是确定新形成恒星的辐射如何与周围环境相互作用的关键，使其能够用作恒星形成示踪剂。我们提出了新的Herschel/SPIRE 250，350和500妈妈的LHA 120-N44和LHA 120-N63在LMC的数据。我们构建的平均光谱能量分布（SED）为中心的恒星形成网站的红外明亮的一部分的环。环隙覆盖约10-约100 pc。我们使用唯象尘埃模型来拟合这些SED，以获得尘柱密度，入射辐射场和多环芳烃分子的丰度。我们看到辐射场能量密度随N63周围径向距离的变化而减小5倍。N44没有表现出系统性的趋势。我们构造了一个简单的几何模型来推导这两个区域周围的3-D密度分布。Herschel/SPIRE数据已被证明在推导尘埃质量分布方面非常有效。我们发现，在两个源的辐射场的行为非常不同。N63或多或少是球对称的，平均辐射场随距离而下降。N44的辐射强度没有系统性的下降，这可能是由于周围分子物质的不均匀性以及该区域内几个恒星形成星团的复杂分布。
英文摘要：
We study the structure of the medium surrounding sites of high-mass star formation to determine the interrelation between the HII regions and the environment from which they were formed. The density distribution of the surroundings is key in determining how the radiation of the newly formed stars interacts with the surrounds in a way that allows it to be used as a star formation tracer. We present new Herschel/SPIRE 250, 350 and 500 mum data of LHA 120-N44 and LHA 120-N63 in the LMC. We construct average spectral energy distributions (SEDs) for annuli centered on the IR bright part of the star formation sites. The annuli cover ~10-~100 pc. We use a phenomenological dust model to fit these SEDs to derive the dust column densities, characterise the incident radiation field and the abundance of polycyclic aromatic hydrocarbon molecules. We see a factor 5 decrease in the radiation field energy density as a function of radial distance around N63. N44 does not show a systematic trend. We construct a simple geometrical model to derive the 3-D density profile of the surroundings of these two regions. Herschel/SPIRE data have proven very efficient in deriving the dust mass distribution. We find that the radiation field in the two sources behaves very differently. N63 is more or less spherically symmetric and the average radiation field drops with distance. N44 shows no systematic decrease of the radiation intensity which is probably due to the inhomogeneity of the surrounding molecular material and to the complex distribution of several star forming clusters in the region.
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