Spectral energy distribution modelling of southern candidate massive protostars using the Bayesian inference method
Spectral energy distribution modelling of southern candidate massive protostars using the Bayesian inference method
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使用贝叶斯推理方法对南部候选大质量原恒星进行光谱能量分布建模
DOI：
10.1111/j.1365-2966.2008.14103.x
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发表时间：
2008
影响因子：
4.8
通讯作者：
M. Cunningham
中科院分区：
文献类型：
--
作者：
T. Hill;C. Pinte;V. Minier;M. Burton;M. Cunningham
将毫米波段的数据与红外波段的数据相结合，我们对Hill等人提出的405毫米波段连续谱源中的227个进行了光谱能量分布（SED）建模，这些连续谱源被认为在其形成的最早阶段含有年轻的大质量恒星。从拟合中提取三个主要参数：温度、质量和光度。所采用的方法是贝叶斯推断，它允许为每个原恒星候选者绘制每个参数的统计上可能的合适值范围。这是该方法首次应用于大质量星星的形成。
在这项工作中的SED建模参数的累积分布图表明，集体，没有甲醇脉泽和/或无线电连续协会（MM-唯一的核心）的来源显示类似的特性，高质量的星星形成区域。归因于MM只有核心和高质量的星星形成样本之间的边缘区别的意义，我们得出的假设的MM只有核心的性质，包括人口本身包括不同类型的源的可能性，并讨论他们的作用，在大规模的星星形成的形成方案。此外，我们还讨论了SED建模及其应用领域的有用性和局限性。从这项工作中，很明显，在有效的参数范围内，利用目前的远红外数据的SED不能用于确定大质量原恒星或大质量年轻恒星物体的演化。
Concatenating data from the millimetre regime to the infrared, we have performed spectral energy distribution (SED) modelling for 227 of the 405 millimetre continuum sources of Hill et al. which are thought to contain young massive stars in the earliest stages of their formation. Three main parameters are extracted from the fits: temperature, mass and luminosity. The method employed was the Bayesian inference, which allows a statistically probable range of suitable values for each parameter to be drawn for each individual protostellar candidate. This is the first application of this method to massive star formation.
The cumulative distribution plots of the SED modelled parameters in this work indicate that collectively, the sources without methanol maser and/or radio continuum associations (MM-only cores) display similar characteristics to those of high-mass star formation regions. Attributing significance to the marginal distinctions between the MM-only cores and the high-mass star formation sample, we draw hypotheses regarding the nature of the MM-only cores, including the possibility that the population itself comprises different types of source, and discuss their role in the formation scenarios of massive star formation. In addition, we discuss the usefulness and limitations of SED modelling and its application to the field. From this work, it is clear that within the valid parameter ranges, SEDs utilising current far-infrared data cannot be used to determine the evolution of massive protostars or massive young stellar objects.
影响因子：
3.2
作者：
V. Mannings;A. Boss;S. Russell
通讯作者：
V. Mannings;A. Boss;S. Russell