The SOFIA Massive (SOMA) Star Formation Survey. III. From Intermediate- to High-mass Protostars
The SOFIA Massive (SOMA) Star Formation Survey. III. From Intermediate- to High-mass Protostars
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DOI：
10.3847/1538-4357/abbefb
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发表时间：
2020-06
期刊：
影响因子：
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通讯作者：
Mengyao Liu;J. Tan;J. D. De Buizer;Yichen Zhang;E. Moser;M. Beltrán;J. Staff;Kei E. I. Tanaka;B. Whitney;V. Rosero;Yao-lun Yang;R. Fedriani
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作者：
Mengyao Liu;J. Tan;J. D. De Buizer;Yichen Zhang;E. Moser;M. Beltrán;J. Staff;Kei E. I. Tanaka;B. Whitney;V. Rosero;Yao-lun Yang;R. Fedriani
作为SOFIA大质量（索马）星星形成调查的一部分，我们提供了14个中等质量原星星候选者的SOFIA-FORCAST图像。我们建立光谱能量分布，也使用档案斯皮策，赫歇尔和红外天文台的数据。然后，我们拟合的光谱能量分布与辐射传输模型的张和谭，湍流核心吸积理论的基础上，估计关键的原恒星的属性。随着这些中等质量的来源，根据平均性能来自SED拟合，索马原恒星跨度光度，目前的原恒星质量，和周围的团块质量表面密度，。还探讨了各种各样的个体原恒星和原星团环境的演化状态。我们还考虑了大约50颗在红外暗云中发现的原恒星，这些原恒星预计处于演化的最早阶段。有了这个全球性的样本，大多数高质量和中等质量的原恒星的演化阶段进行了探测。最佳拟合模型显示，没有证据表明，一个阈值的原星团质量表面密度是需要形成原恒星。然而，为了形成更大质量的原恒星，有初步的证据表明需要。我们讨论了这是如何与核心吸积模型，包括从形成大质量星星的内部反馈的预期一致。
We present SOFIA–FORCAST images of 14 intermediate-mass protostar candidates as part of the SOFIA Massive (SOMA) Star Formation Survey. We build spectral energy distributions, also using archival Spitzer, Herschel, and IRAS data. We then fit the spectral energy distributions with radiative transfer models of Zhang & Tan, based on turbulent core accretion theory, to estimate key protostellar properties. With the addition of these intermediate-mass sources, based on average properties derived from SED fitting, SOMA protostars span luminosities from , current protostellar masses from , and ambient clump mass surface densities, , from . A wide range of evolutionary states of the individual protostars and of the protocluster environments is also probed. We have also considered about 50 protostars identified in infrared dark clouds that are 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. The best-fitting models show no evidence that a threshold value of the protocluster clump mass surface density is required to form protostars up to . However, to form more massive protostars, there is tentative evidence that needs to be . We discuss how this is consistent with expectations from core accretion models that include internal feedback from the forming massive star.