基于SLAM的恒星光谱工厂（SSF）
The Stellar Spectra Factory (SSF) Based On SLAM
AI总结：
本文提出基于SLAM的恒星光谱工厂（SSF），通过四个子模型从任意恒星大气参数生成经验光谱，验证显示与已知光谱库及观测的差异小于5%。
摘要：
在这项工作中，我们介绍了恒星光谱工厂（SSF），这是一个能够从任意恒星大气参数生成基于经验数据的恒星光谱的工具。给定任意有效温度、表面重力加速度和金属丰度，SSF可以预测相对流量定标的经验光谱。SSF基于SLAM构建插值方法，并使用ATLAS-A库作为训练数据集。SSF由4个数据驱动的子模型组成，用于预测经验恒星光谱。SSF-N可以生成从A型到K型以及部分M型巨星的光谱，覆盖3700 < Teff < 8700 K，0 < logg < 6 dex，以及-1.5 < [M/H] < 0.5 dex的范围。SSF-gM主要用于预测M型巨星光谱，其参数范围为3520 < Teff < 4000K和-1.5 < [M/H] < 0.4 dex。SSF-dM用于生成M型矮星光谱，参数范围为3295 < Teff < 4040K，-1.0 < [M/H] < 0.1 dex。而SSF-B可以预测B型恒星光谱，参数范围为9000 < Teff < 24000K和-5.2 < MG < 1.5 mag。通过将预测光谱的流量与从已知光谱库MILES和MaStar中选择的具有相同恒星参数的恒星的光谱进行比较，验证了预测光谱的准确性。预测光谱与MILES和MaStar中相应光谱在光学波长上的平均流量差异小于5%。进一步验证是在预测光谱积分计算出的星等与PS1和APASS波段中具有相同恒星参数的观测值之间进行的。在预测光谱与光度观测之间未发现显著的系统性差异。与从PS1中选择的具有相同恒星参数的恒星相比，SSF-gM在r波段的误差为0.08mag。而与从APASS中选择的具有相同恒星参数的恒星相比，SSF-dM在i波段的误差为0.31mag。
英文摘要：
In this work, we present Stellar Spectra Factory (SSF), a tool to generate empirical-based stellar spectra from arbitrary stellar atmospheric parameters. The relative flux-calibrated empirical spectra can be predicted by SSF given arbitrary effective temperature, surface gravity, and metallicity. SSF constructs the interpolation approach based on the SLAM, using ATLAS-A library as the training dataset. SSF is composed of 4 data-driven sub-models to predict empirical stellar spectra. SSF-N can generate spectra from A to K type and some M giant stars, covering 3700 < Teff < 8700 K, 0 < logg < 6 dex, and -1.5 < [M/H] < 0.5 dex. SSF-gM is mainly used to predict M giant spectra with 3520 < Teff < 4000K and -1.5 < [M/H] < 0.4 dex. SSF-dM is for generating M dwarf spectra with 3295 < Teff < 4040K, -1.0 < [M/H] < 0.1 dex. And SSF-B can predict B-type spectra with 9000 < Teff < 24000K and -5.2< MG < 1.5 mag. The accuracy of the predicted spectra is validated by comparing the flux of predicted spectra to those with same stellar parameters selected from the known spectral libraries, MILES and MaStar. The averaged difference of flux over optical wavelength between the predicted spectra and the corresponding ones in MILES and MaStar is less than 5%. More verification is conducted between the magnitudes calculated from the integration of the predicted spectra and the observations in PS1 and APASS bands with the same stellar parameters. No significant systematic difference is found between the predicted spectra and the photomatric observations. The uncertainty is 0.08mag in r band for SSF-gM when comparing with the stars with the same stellar parameters selected from PS1. And the uncertainty becomes 0.31mag in i band for SSF-dM when comparing with the stars with the same stellar parameters selected from APASS.
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