标题： 盖亚-ESO调查的原子数据 显示英文标题

标题： Atomic data for the Gaia-ESO Survey

摘要： 我们描述了在盖亚-ESO调查中用于FGK型恒星丰度分析的原子和分子数据。 我们提出了一项前所未有的努力，以创建一个均匀的谱线列表，该列表被多个丰度分析小组用于计算合成光谱和等值宽度。 原子数据附有质量指标和详细的来源参考。 原子和分子数据以电子形式公开提供。 一般来说，优先使用实验过渡概率，但也使用了理论值。 由于这种程序的模型依赖性，避免使用天体物理gf值。 对于其谱线显著受超精细结构或同位素分裂影响的元素，已做出协调努力，收集各个谱线成分的必要数据。 我们还对碰撞引起的谱线展宽的可用数据进行了详细研究，这些碰撞是与中性氢原子发生的。 计算了太阳和大角星的合成光谱，以评估谱线的重叠特性。 在35种元素的波长范围从475纳米到685纳米以及从850纳米到895纳米的超过1300条谱线中，我们识别出约200条谱线，属于24种物质，这些谱线具有准确的gf值，并且在太阳和大角星的光谱中没有重叠。 对于与中性氢原子碰撞引起的展宽，建议使用Anstee-Barklem-O'Mara理论的数据，如果可用的话，否则应避免中性物种的谱线。 R.L. Kurucz的理论展宽数据应用于Sc II、Ti II和Y II谱线。 对于电离的稀土元素，可以使用Unsöld近似，并将线宽增强因子设为1.5。 指出了若干物质的原子数据的改进需求，包括Al I、S I、Cr II、Na I、Si I、Ca II和Ni I。 显示英文摘要

摘要： We describe the atomic and molecular data that were used for the abundance analyses of FGK-type stars carried out within the Gaia-ESO Survey. We present an unprecedented effort to create a homogeneous line list, which was used by several abundance analysis groups to calculate synthetic spectra and equivalent widths. The atomic data are accompanied by quality indicators and detailed references to the sources. The atomic and molecular data are made publicly available in electronic form. In general experimental transition probabilities were preferred but theoretical values were also used. Astrophysical gf-values were avoided due to the model-dependence of such a procedure. For elements whose lines are significantly affected by hyperfine structure or isotopic splitting a concerted effort has been made to collate the necessary data for the individual line components. We also performed a detailed investigation of available data for line broadening due to collisions with neutral hydrogen atoms. Synthetic spectra calculated for the Sun and Arcturus were used to assess the blending properties of the lines. Among a subset of over 1300 lines of 35 elements in the wavelength ranges from 475 nm to 685 nm and from 850 nm to 895 nm we identified about 200 lines of 24 species which have accurate gf-values and are free of blends in the spectra of the Sun and Arcturus. For the broadening due to collisions with neutral hydrogen we recommend data based on Anstee-Barklem-O'Mara theory, where available, and to avoid lines of neutral species otherwise. Theoretical broadening data by R.L. Kurucz should be used for Sc II, Ti II, and Y II lines. For ionised rare-earth species the Uns\"old approximation with an enhancement factor of 1.5 for the line width can be used. Desirable improvements in atomic data were identified for a number of species, including Al I, S I, Cr II, Na I, Si I, Ca II, and Ni I.