论文标题
GAIA-ESO调查的原子数据
Atomic data for the Gaia-ESO Survey
论文作者
论文摘要
我们描述了用于在GAIA-ESO调查中进行的FGK型星的丰度分析的原子数据和分子数据。我们提出了创建均匀的线列表的前所未有的努力，该列表被几个丰度分析组用于计算合成光谱和等效宽度。原子数据伴随着质量指标和对来源的详细引用。原子数据和分子数据以电子形式公开提供。总的来说，首选实验过渡概率，但还使用了理论值。由于这种程序的模型依赖性，避免了天体物理GF值。对于线条结构或同位素分裂的显着影响的元素，已经采取了共同的努力来整理单个线组件的必要数据。由于与中性氢原子的碰撞，我们还对可用数据进行了详细研究。用于太阳和arcturus计算的合成光谱用于评估线条的混合特性。在波长范围为475 nm至685 nm的1300多种35个元素的子集中，从850 nm到895 nm，我们鉴定了约200条24种，具有准确的GF值，并且在太阳和Arcturus的光谱中没有混合物。对于由于与中性氢的碰撞而引起的扩展，我们建议基于Anstee-Barklem-o'mara理论的数据，并避免避免中性物种的线。 R.L. Kurucz的理论扩展数据应用于SC II，Ti II和Y II线。对于离子稀土物种，可以使用线条宽度为1.5的Unsöld近似值。确定了许多物种的原子数据的理想改进，包括Al I，S I，Cr II，Na I，Si I，Ca II和Ni I.
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 Unsöld 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.
