1.5 $μ$ m光谱区原子谱线参数的经验测定
Empirical determination of atomic line parameters of the 1.5 $μ$m spectral region
摘要：
由于望远镜及其仪器的改进，天体物理学数据的质量和数量随着时间的推移不断提高。这就需要相应地改进用于获得和分析结果数据的技术。在1.56 $μ$ m处的红外光谱范围通常由位于GREGOR太阳望远镜的GREGOR红外光谱仪（GRIS）观测到，其宽度约为30 $Å$，并且包括至少15条谱线。通常情况下，只有少数谱线（最多五条）用于使用GRIS的研究，因为缺乏其他的原子参数。包括更多的谱线可以减轻太阳大气参数之间的一些已知的模糊性。我们使用反演技术来推断太阳大气模型和原子参数的谱线，在当地的热力学平衡（LTE）近似下，重现光谱偏振观测。我们提出了精确的原子参数的光谱范围内的15个谱线从15644 $Å$到15674 $Å$。这个光谱范围通常用于太阳研究，因为它可以研究低光球层。此外，红外谱线是比光学更好的磁场示踪剂。
英文摘要：
Both the quality and amount of astrophysical data are steadily increasing over time owing to the improvement of telescopes and their instruments. This requires corresponding evolution of the techniques used for obtaining and analyzing the resulting data. The infrared spectral range at 1.56 $μ$m usually observed by the GRegor Infrared Spectrograph (GRIS) at the GREGOR solar telescope has a width of around 30 $Å$ and includes at least 15 spectral lines. Normally, only a handful of spectral lines (five at most) are used in studies using GRIS because of the lack of atomic parameters for the others. Including more spectral lines may alleviate some of the known ambiguities between solar atmospheric parameters. We used inversion techniques to infer both solar atmospheric models and the atomic parameters of spectral lines which, under the local thermodynamic equilibrium (LTE) approximation, reproduce spectropolarimetric observations. We present accurate atomic parameters for 15 spectral lines within the spectral range from 15644 $Å$ to 15674 $Å$. This spectral range is commonly used in solar studies because it enables the study of the low photosphere. Moreover, the infrared spectral lines are better tracers of the magnetic fields than the optical ones.
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