论文标题
索非亚大规模（SOMA）星星形成调查。 iii。从中间到高质量原始恒星
The SOFIA Massive (SOMA) Star Formation Survey. III. From Intermediate- to High-Mass Protostars
论文作者
论文摘要
我们介绍$ \ sim10-40 \，μ$ m m sofia forcast图像，是14个中间质量原始候选者，作为Sofia Massive（SOMA）星星形成调查的一部分。我们构建了光谱能量分布（SED），还利用档案Spitzer，Herschel和IRAS数据。然后，我们以基于湍流核心积聚理论的Zhang＆Tan（2018）的辐射转移（RT）模型拟合SED，以估计关键的Protostellar特性。添加了这些中间质量的来源，Soma Protostars从$ \ sim10^{2} -10^{6} \：l _ {\ odot} $，当前的protostellar质量，$ \ sim0.5-30 \：m _ { $ 0.1-3 \：{\ rm {g \：cm}^{ - 2}} $。还探测了各个质恒星和原始环境的各种进化状态。我们还考虑了大约50个在红外乌云中鉴定出的原始恒星，并预计将处于进化的最早阶段。使用该全球样品，探测了高质量和中等质量原恒星的大多数进化阶段。从最佳拟合模型来看，没有证据表明需要形成最高$ \ sim25 \：m_ \ odot $的原始块状质量表面密度的阈值。但是，要形成更大的质恒星，有暂定的证据表明$σ_ {\ rm {cl}} $需要为$ \ gtrsim1 \：{\ rm {g \，cm}}}}^{ - 2} $。我们讨论这与核心积聚模型的期望是如何一致的，核心积聚模型包括来自形成大量恒星的内部反馈。
We present $\sim10-40\,μ$m SOFIA-FORCAST images of 14 intermediate-mass protostar candidates as part of the SOFIA Massive (SOMA) Star Formation Survey. We build spectral energy distributions (SEDs), also utilizing archival Spitzer, Herschel and IRAS data. We then fit the SEDs with radiative transfer (RT) models of Zhang & Tan (2018), based on Turbulent Core Accretion theory, to estimate key protostellar properties. With the addition of these intermediate-mass sources, SOMA protostars span luminosities from $\sim10^{2}-10^{6}\:L_{\odot}$, current protostellar masses from $\sim0.5-30\:M_{\odot}$ and ambient clump mass surface densities, $Σ_{\rm cl}$ from $0.1-3\:{\rm{g\:cm}^{-2}}$. A wide range of evolutionary states of the individual protostars and of the protocluster environments are also probed. We have also considered about 50 protostars identified in Infrared Dark Clouds and expected to be at the earliest stages of their evolution. With this global sample, most of the evolutionary stages of high- and intermediate-mass protostars are probed. From the best fitting models, there is no evidence of a threshold value of protocluster clump mass surface density being needed to form protostars up to $\sim25\:M_\odot$. However, to form more massive protostars, there is tentative evidence that $Σ_{\rm{cl}}$ needs to be $\gtrsim1\:{\rm{g\,cm}}^{-2}$. We discuss how this is consistent with expectations from core accretion models that include internal feedback from the forming massive star.
