高质量原恒星物体的Spitzer-IRAC II
Spitzer-IRAC GLIMPSE of high mass protostellar objects II - SED modelling of a bonafide sample
摘要：
我们的目标是估计和分析的HMPO的红外对应物的物理性质，通过比较它们的光谱能量分布（SED）与那些预测的辐射转移吸积模型的YSO。利用2 MASS、GLIMPSE 2.0版星表、MSX、IRAS和一些单碟（和干涉）（亚）毫米数据，将68个IRCs的SED从GLIMPSE测光扩展到可能的极限，从近红外到毫米波段。利用一个在线的SED拟合工具，使用二维辐射转移吸积模型的YSO拟合观测到的SED，以获得各种物理参数。IRC的SED由质量在5-42 Msun之间、年龄在10^3 ~ 10^6年之间的大质量原恒星模型拟合。其质量和年龄的中位数分别为10 Msun和10^4 yr。包层很大，平均大小约为0.2-0.3 pc，其分布与论文I中讨论的8微米星云的大小分布非常相似。估计的包层吸积速率很高，平均值为10^（-3）Msun/yr，并显示出指数为2的幂律质量依赖性，表明在这些尺度下的球形吸积。在大多数的源中发现了平均质量为10^（-1.4+-0.7）Msun的中微子。用YSO吸积模型成功地解释了观测到的HMPO红外对应物的红外-毫米波SED。模拟的源主要代表原B星，尽管其中一些可能在未来成为O星。我们证明，这些结果中的许多可能代表了一个现实的图片大质量恒星形成，尽管一些结果可能是模型内的假设的影响。
英文摘要：
We aim to estimate and analyse the physical properties of the infrared counterparts of HMPOs by comparing their spectral energy distributions (SED) with those predicted by radiative transfer accretion models of YSOs. The SED of 68 IRCs are extended beyond the GLIMPSE photometry to the possible limits, from the near-infrared to the millimetre wavelengths by using the 2MASS, GLIMPSE version 2.0 catalogs, MSX, IRAS and some single dish (and interferometric) (sub)mm data. An online SED fitting tool that uses 2D radiative transfer accretion models of YSOs is employed to fit the observed SED to obtain various physical parameters. The SED of IRCs were fitted by models of massive protostars with a range of masses between 5-42 Msun and ages between 10^3 and 10^6 years. The median mass and age are 10 Msun and 10^4 yrs. The envelopes are large with a mean size of ~ 0.2-0.3 pc and show a distribution that is very similar to the distribution of the sizes of 8 micron nebulae discussed in Paper I. The estimated envelope accretion rates are high with a mean value of 10^(-3) Msun/yr and show a power law dependence to mass with an exponent of 2, suggesting spherical accretion at those scales. Disks are found to exist in most of the sources with a mean mass of 10^(-1.4+-0.7) Msun. The observed infrared-millimetre SED of the infrared counterparts of HMPOs are successfully explained with an YSO accretion model. The modelled sources mostly represent proto-B stars although some of them could become O stars in future. We demonstrate that many of these results may represent a realistic picture of massive star formation, despite some of the results which may be an effect of the assumptions within the models.
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