Zeta-Payne: A Fully Automated Spectrum Analysis Algorithm for the Milky Way Mapper Program of the SDSS-V Survey-猫眼课题宝

DOI：

10.3847/1538-3881/ac5f49

发表时间：

2022-03

期刊：

The Astronomical Journal

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通讯作者：

中科院分区：

其他

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作者：

I. Straumit;A. Tkachenko;S. Gebruers;J. Audenaert;M. Xiang;E. Zari;C. Aerts;Jennifer Johnson;J. Kollmeier;H. Rix;R. Beaton;J. Saders;J. Teske;A. Roman-Lopes;Y. Ting;Carlos G. Rom'an-Z'uniga

斯隆数字巡天（SDSS）最近启动了其第五代巡天（SDSS-V），重点是恒星光谱学。特别是，SDSS-V的银河系测绘仪计划将为整个天空中超过5 × 106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，专门开发的SDSS-V光谱的恒星与这些光谱类型和机器学习工具的绘图获得恒星标签。我们提供的算法训练的细节，人工光谱测试，其验证的两个控制样本的真实的明星。使用ZETA-PAYNE进行的分析在使用APOGEE进行的近红外分析中仅产生了适度的内部不确定性（带BOSS的光纤）：3%-10%（1%-2%）T eff，5%-30%（5%-25%）vsini，1.7-6.3 km s−1（0.7-2.2 km s−1），logg <0.1 dex（<0.05 dex），星星的[M/H]为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光谱的信息量（远）小于这些恒星的BOSS光谱，而logg，vsini和[M/H]在大多数情况下都太不确定，无法进行有意义的天体物理解释。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。

The Sloan Digital Sky Survey (SDSS) has recently initiated its fifth survey generation (SDSS-V), with a central focus on stellar spectroscopy. In particular, SDSS-V's Milky Way Mapper program will deliver multiepoch optical and near-infrared spectra for more than 5 × 106 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 T eff, 5%–30% (5%–25%) for vsini , 1.7–6.3 km s−1 (0.7–2.2 km s−1) for radial velocity, <0.1 dex (<0.05 dex) for logg , 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 logg , vsini , 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.

Zeta-Payne: A Fully Automated Spectrum Analysis Algorithm for the Milky Way Mapper Program of the SDSS-V Survey

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