SPECIES Ⅰ：恒星的光谱参数和atmosphEric ChemIstriEs
SPECIES I: Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars
摘要：
对系外行星的探测和随后的定性与其宿主恒星的特征密切相关。因此，有必要详细研究这颗恒星，以了解其伴星的形成历史和特征。我们的目标是开发一个社区工具，允许自动计算恒星参数的大量恒星，使用高分辨率中阶梯光谱和最小的光度星等，并介绍了这项工作的第一个结果。我们测量了几条铁谱线的等效宽度，并将其用于求解假设局部热力学平衡的辐射转移方程，以获得大气参数（$T_{\text{eff}}$，[Fe/H]，logg和$ξ_t$）。我们用这些值来推导恒星光球中11种化学元素（Na，Mg，Al，Si，Ca，Ti，Cr，Mn，Ni，Cu和Zn）的丰度。旋转和宏观湍流速度，得到使用温度校准器和合成线配置文件，以匹配所观察到的光谱的五个吸收线。最后，通过插值网格的MIST等时线，我们推导出的质量，半径和年龄使用贝叶斯方法。SPECIES获得的批量参数与不同现有目录中的测量值非常一致，包括使用不同方法导出的参数。我们发现很好的协议与以前的作品，使用类似的方法。我们发现一些元素的化学丰度与其他作品的差异，这可能是由于$T_{\text{eff}}$的差异，或者是用于推导它们的线列表或原子线数据的差异。我们还获得了描述不同参数之间相关性的解析关系，并实施了新方法来更好地处理这些相关性，从而更好地描述了与测量相关的不确定性。
英文摘要：
The detection and subsequent characterisation of exoplanets are intimately linked to the characteristics of their host star. Therefore, it is necessary to study the star in detail in order to understand the formation history and characteristics of their companion(s). Our aims were to develop a community tool that allows the automated calculation of stellar parameters for a large number of stars, using high resolution echelle spectra and minimal photometric magnitudes, and introduce the first results in this work. We measured the equivalent widths of several iron lines and used them to solve the radiative transfer equation assuming local thermodynamic equilibrium to obtain the atmospheric parameters ($T_{\text{eff}}$, [Fe/H], logg and $ξ_t$). We used these values to derive the abundance of 11 chemical elements in the stellar photosphere (Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Ni, Cu and Zn). Rotation and macroturbulent velocity were obtained using temperature calibrators and synthetic line profiles to match the observed spectra of five absorption lines. Finally, by interpolating in a grid of MIST isochrones, we derived the mass, radius and age using a Bayesian approach. SPECIES obtains bulk parameters that are in good agreement with measured values from different existing catalogues, including when different methods are used to derive them. We find excellent agreement with previous works that used similar methodologies. We find discrepancies in the chemical abundances for some elements with respect to other works, which could be produced by differences in $T_{\text{eff}}$, or in the line list or the atomic line data used to derive them. We also obtained analytic relations to describe the correlations between different parameters, and we implemented new methods to better handle these correlations, which provides a better description of the uncertainties associated with the measurements.
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