ATHOS：基于光谱通量比的FGK恒星的飞行中恒星参数确定
ATHOS: On-the-fly stellar parameter determination of FGK stars based on flux ratios from optical spectra
摘要：
光谱测定基本恒星参数的工具不仅应包括针对某一特定调查或仪器的定制解决方案，而且，为了使跨调查具有可比性，它们还应能够处理来自各种摄谱仪、分辨率和波长覆盖范围的光谱。为了满足这些雄心勃勃的规格，我们开发了ATHOS（均匀化恒星参数的工具），这是一种全新的分析工具，它采用计算成本低廉的分析关系，将光谱中指定波长区域的通量比（FR）与恒星参数有效温度（$T_\mathrm{eff}$）、铁丰度（[Fe/H]）和表面重力（$\log{g}$）联系起来。我们的$T_\mathrm{eff}$估计器是基于来自巴耳末线H $β$和H $α$周围的九对波长范围的FR，而对于[Fe/H]和$\log{g}$，我们提供4800 nm和6500 nm之间的31和11个FR。采用这些FR的分析关系在基准样品的124个真实光谱上进行训练，该基准样品覆盖$T_{\rm eff}\approx$ 4000至6500 K、[Fe/H] $\approx$-4.5至0.3 dex和$\log{g}\approx$ 1至5 dex的大参数空间，这也反映了ATHOS的适用范围。该方法的精度仅受训练样本参数的有限不确定性的限制，而其内部精度可以提高70%。我们在六个独立的大型调查中测试了ATHOS，其中包括Gaia-ESO和SDSS/SEGUE调查。异常低的执行时间（<30 ms/光谱）以及与文献参数的比较表明，ATHOS可以成功地实现其主要目标，即快速恒星参数化，具有交叉调查的有效性，高精度和高精度。这些是使未来调查（如4MOST或WEAVE）的输出均匀化的关键。[删节]
英文摘要：
Tools for the spectroscopic determination of fundamental stellar parameters should not only comprise customized solutions for one particular survey or instrument, but, in order to enable cross-survey comparability, they should also be capable of dealing with spectra from a variety of spectrographs, resolutions, and wavelength coverages. To meet these ambitious specifications, we developed ATHOS (A Tool for HOmogenizing Stellar parameters), a fundamentally new analysis tool that adopts computationally inexpensive analytical relations tying flux ratios (FRs) of designated wavelength regions in optical spectra to the stellar parameters effective temperature ($T_\mathrm{eff}$), iron abundance ([Fe/H]), and surface gravity ($\log{g}$). Our $T_\mathrm{eff}$ estimator is based on FRs from nine pairs of wavelength ranges around the Balmer lines H$β$ and H$α$, while for [Fe/H] and $\log{g}$ we provide 31 and 11 FRs between 4800 Å and 6500 Å. The analytical relations employing these FRs were trained on 124 real spectra of a benchmark sample that covers a large parameter space of $T_{\rm eff}\approx$ 4000 to 6500 K, [Fe/H] $\approx$ -4.5 to 0.3 dex, and $\log{g}\approx$ 1 to 5 dex, which also reflects ATHOS' range of applicability. The method's accuracies are merely bounded by finite uncertainties in the training sample parameters, while its internal precisions can be better by up to 70%. We tested ATHOS on six independent large surveys, amongst which are the Gaia-ESO and the SDSS/SEGUE surveys. The exceptionally low execution time (<30 ms/spectrum) together with a comparison to the literature parameters showed that ATHOS can successfully achieve its main objectives, i.e. fast stellar parameterization with cross-survey validity, high accuracy, and high precision. These are key to homogenize the output from future surveys, such as 4MOST or WEAVE. [abridged]
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
