Zeta-Payne：用于SDSS-V勘测的Milky Way Mapper程序的全自动频谱分析算法
Zeta-Payne: a fully automated spectrum analysis algorithm for the Milky Way Mapper program of the SDSS-V survey
摘要：
斯隆数字巡天最近启动了其第五代巡天（SDSS-V），重点关注恒星光谱学。特别是，SDSS-V Milky Way Mapper计划将为整个天空中的500多万颗恒星提供多时期的光学和近红外光谱，涵盖恒星质量，表面温度，演化阶段和年龄的大范围。这些光谱中约有10%是OBAF光谱类型的热星，其分析没有建立测量管道。在这里，我们提出了光谱分析算法，Zeta-Payne，专门开发用于从具有这些光谱类型的恒星的SDSS-V光谱中获得恒星标签，并利用机器学习工具。我们提供的算法训练的细节，人工光谱的测试，其验证的两个控制样本的真实恒星。用Zeta-Payne进行的分析在APOGEE的近红外中只产生了适度的内部不确定性（带BOSS的光纤）：Teff为3-10%（1-2%），v*sin（i）为5-30%（5-25%），1.7-6.3 km/s（0.7-2.2 km/s），log（g）的$<0.1$ dex（$<0.05$ dex）和[M/H]的0.4-0.5 dex（0.1 dex）。我们发现一个很好的协议的大气参数的OBAF型恒星推断时，从他们的高分辨率和低分辨率的光谱。对于大多数恒星的标签，APOGEE光谱比这些恒星的BOSS光谱（远）提供的信息少，而log（g），v*sin（i）和[M/H]在大多数情况下对于有意义的天体物理解释来说太不确定了。这使得BOSS的低分辨率光谱更适合于OBAF型恒星的恒星标签，除非后者受到高水平的消光。
英文摘要：
The Sloan Digital Sky Survey has recently initiated its 5th survey generation (SDSS-V), with a central focus on stellar spectroscopy. In particular, SDSS-V Milky Way Mapper program will deliver multi-epoch optical and near-infrared spectra for more than 5 million stars across the entire sky, covering a large range in stellar mass, surface temperature, evolutionary stage, and age. About 10% of those spectra will be of hot stars of OBAF spectral types, for whose analysis no established survey pipelines exist. Here we present the spectral analysis algorithm, Zeta-Payne, developed specifically to obtain stellar labels from SDSS-V spectra of stars with these spectral types and drawing on machine learning tools. We provide details of the algorithm training, its test on artificial spectra, and its validation on two control samples of real stars. Analysis with Zeta-Payne leads to only modest internal uncertainties in the near-IR with APOGEE (optical with BOSS): 3-10% (1-2%) for Teff, 5-30% (5-25%) for v*sin(i), 1.7-6.3 km/s(0.7-2.2 km/s) for RV, $<0.1$ dex ($<0.05$ dex) for log(g), and 0.4-0.5 dex (0.1 dex) for [M/H] of the star, respectively. We find a good agreement between atmospheric parameters of OBAF-type stars when inferred from their high- and low-resolution optical spectra. For most stellar labels the APOGEE spectra are (far) less informative than the BOSS spectra of these stars, while log(g), v*sin(i), and [M/H] are in most cases too uncertain for meaningful astrophysical interpretation. This makes BOSS low-resolution optical spectra better for stellar labels of OBAF-type stars, unless the latter are subject to high levels of extinction.
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