arXiv 1703.007202017-03-02astro-ph.SR

银河系中大质量恒星的高精度定量光谱学

Highly accurate quantitative spectroscopy of massive stars in the Galaxy

Maria-Fernanda Nieva, Norbert Przybilla

备注：: 8 pages, 7 figures, conference proceeding (invited talk), IAUS 329: The lives and death-throes of massive stars, J.J. Eldridge, L. McClelland, L. Xiao & J. Bray, eds
DOI：: 10.1017/S1743921317003167

摘要：

在大质量恒星光谱学中，实现恒星参数和化学成分测定的高精度和高精度是具有挑战性的。一方面，无偏样本建立的目标选择由于可能发生在单个对象中的几种类型的特性而变得复杂。另一方面，即使在中高光谱分辨率和典型的信噪比下，复合光谱也往往不能被识别出来，尽管大质量恒星之间的多重性是普遍存在的。特别是，产生大量自动减少数据的调查容易忽略细节，这些细节对于使用适用于单个恒星光谱的一组标准假设而开发的技术进行分析是危险的。因此，由于未认识到所研究物体的真实性质，或如果认识到，用于分析的物体的样本量比最初计划的小得多，可能会产生比预期大得多的系统误差。需要考虑的更多因素是从选择仪器到选择建模代码、输入数据、分析技术和选择待分析的谱线的多个步骤。只有在避免所有可能的陷阱时，才能在基本参数和化学指纹方面实现对恒星的精确和准确的表征，从而为进一步研究恒星结构和演化或银河系的化学演化奠定基础。目前的工作范围是提供更广泛的社会标准，以评估光谱调查的大质量恒星之前，在更广泛的背景下解释他们。讨论是由我们的经验，从最简单的单个对象到多个系统的大质量恒星光谱学的研究十多年。

英文摘要：

Achieving high accuracy and precision in stellar parameter and chemical composition determinations is challenging in massive star spectroscopy. On one hand, the target selection for an unbiased sample build-up is complicated by several types of peculiarities that can occur in individual objects. On the other hand, composite spectra are often not recognized as such even at medium-high spectral resolution and typical signal-to-noise ratios, despite multiplicity among massive stars is widespread. In particular, surveys that produce large amounts of automatically reduced data are prone to oversight of details that turn hazardous for the analysis with techniques that have been developed for a set of standard assumptions applicable to a spectrum of a single star. Much larger systematic errors than anticipated may therefore result because of the unrecognized true nature of the investigated objects, or much smaller sample sizes of objects for the analysis than initially planned, if recognized. More factors to be taken care of are the multiple steps from the choice of instrument over the details of the data reduction chain to the choice of modelling code, input data, analysis technique and the selection of the spectral lines to be analyzed. Only when avoiding all the possible pitfalls, a precise and accurate characterization of the stars in terms of fundamental parameters and chemical fingerprints can be achieved that form the basis for further investigations regarding e.g. stellar structure and evolution or the chemical evolution of the Galaxy. The scope of the present work is to provide the broader community with criteria to evaluate spectroscopic investigations of massive stars before interpreting them in a broader context. The discussion is guided by our experiences made over a decade of studies of massive star spectroscopy ranging from the simplest single objects to multiple systems.

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