Characterization of dense Planck clumps observed with Herschel and SCUBA-2
Characterization of dense Planck clumps observed with Herschel and SCUBA-2
复制标题
用 Herschel 和 SCUBA-2 观察到的致密普朗克团块的表征
DOI：
10.1051/0004-6361/202037791
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发表时间：
2021
影响因子：
6.5
通讯作者：
Lee C. W.
中科院分区：
文献类型：
--
作者：
Mannfors E.;Juvela M.;Bronfman L.;Eden D. J.;He J.;Kim G.;Kim K.-T.;Kirppu H.;Liu T.;Montillaud J.;Parsons H.;Sanhueza P.;Shang H.;Soam A.;Tatematsu K.;Traficante A.;Vaisala M. S.;Lee C. W.
背景虽然恒星形成的基本过程是已知的，但对恒星形成的多尺度、多环境还需要更多的研究。Planckall-sky调查提供了一大批银河系冷云和团块，这些冷云和团块一直是几次后续调查的目标。目的我们的目标是描述银河系内各种密集的、潜在的恒星形成核心、团块和云的尘埃发射和SF活动。方法我们研究了JCMT Scuba-2连续调查范围内观察到的53个场，并用Herschel绘制了它们的图。我们用修正的黑体函数对Herschel观测进行了拟合，估计了尘埃的性质，研究了尘埃温度与尘埃不透明度光谱指数β之间的关系，并估计了尘埃柱密度。我们使用Fellwalker算法从Scuba-2850μm图中提取团块，并检查它们的质量和大小。星团与几个星表中发现的年轻恒星物体有关。我们用维里分析估计了团块的引力稳定性。结果共发现5 2 9个致密团块，柱子密度一般在(0.3~4.8)×10 2 2 cm−2之间，平均为(1.5±0.0 4)×10 2 2 cm−2，低温(T∼ 10~2 0K)，估计亚毫米β=1.7±0.1。我们发现向毫米波段的不透明光谱指数略有增加。源的质量从0.04M⊙到4259M⊙不等。质量、线大小和温度与距离相关。此外，估计的引力稳定性依赖于距离，距离越远的团块看起来就越像病毒一样束缚着。最后，我们给出了团块的属性目录。结论我们的来源提供了大量的SF区域，从高纬度附近的扩散云到银河系中心附近的大型SF复合体。随着分子谱线数据的增加，对这些区域的分析将继续进行，这将使我们能够更详细地研究团块中最密集的区域。
ContextAlthough the basic processes of star formation (SF) are known, more research is needed on SF across multiple scales and environments. ThePlanckall-sky survey provided a large catalog of Galactic cold clouds and clumps that have been the target of several follow-up surveys.AimsWe aim to characterize a diverse selection of dense, potentially star-forming cores, clumps, and clouds within the Milky Way in terms of their dust emission and SF activity.MethodsWe studied 53 fields that have been observed in the JCMT SCUBA-2 continuum survey SCOPE and have been mapped withHerschel. We estimated dust properties by fittingHerschelobservations with modified blackbody functions, studied the relationship between dust temperature and dust opacity spectral indexβ, and estimated column densities. We extracted clumps from the SCUBA-2 850 μm maps with the FellWalker algorithm and examined their masses and sizes. Clumps are associated with young stellar objects found in several catalogs. We estimated the gravitational stability of the clumps with virial analysis. The clumps are categorized as unbound starless, prestellar, or protostellar.ResultsWe find 529 dense clumps, typically with high column densities from (0.3–4.8) × 1022cm−2, with a mean of (1.5 ± 0.04) ×1022cm−2, low temperatures (T∼ 10–20 K), and estimated submillimeterβ= 1.7 ± 0.1. We detect a slight increase in opacity spectral index toward millimeter wavelengths. Masses of the sources range from 0.04M⊙to 4259M⊙. Mass, linear size, and temperature are correlated with distance. Furthermore, the estimated gravitational stability is dependent on distance, and more distant clumps appear more virially bound. Finally, we present a catalog of properties of the clumps.ConclusionsOur sources present a large array of SF regions, from high-latitude, nearby diffuse clouds to large SF complexes near the Galactic center. Analysis of these regions will continue with the addition of molecular line data, which will allow us to study the densest regions of the clumps in more detail.