We use the first release of the SDSS/MaStar stellar library comprising ~9000, high S/N spectra, to calculate integrated spectra of stellar population models. The models extend over the wavelength range 0.36-1.03 micron and share the same spectral resolution (R~1800) and flux calibration as the SDSS-IV/MaNGA galaxy data. The parameter space covered by the stellar spectra collected thus far allows the calculation of models with ages and chemical composition in the range t>200 Myr, -2 0.7 micron absorption spectra. Moreover, a better parameter coverage at low metallicity allows the calculation of models as young as 500 Myr and the full account of the Blue Horizontal Branch phase of old populations. We present models adopting two independent sets of stellar parameters (T_eff, logg, [Z/H]). In a novel approach, their reliability is tested 'on the fly' using the stellar population models themselves. We perform tests with Milky Way and Magellanic Clouds globular clusters, finding that the new models recover their ages and metallicities remarkably well, with systematics as low as a few per cent for homogeneous calibration sets. We also fit a MaNGA galaxy spectrum, finding residuals of the order of a few per cent comparable to the state-of-art models, but now over a wider wavelength range.

中文翻译：

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基于 SDSS-IV MaStar 恒星光谱库的恒星种群模型 – I. 中年/旧模型

我们使用包含 ~9000 高 S/N 光谱的 SDSS/MaStar 恒星库的第一个版本来计算恒星种群模型的综合光谱。这些模型扩展到 0.36-1.03 微米的波长范围，并与 SDSS-IV/MaNGA 星系数据共享相同的光谱分辨率 (R~1800) 和通量校准。迄今为止收集的恒星光谱所涵盖的参数空间允许计算具有 t>200 Myr，-2 0.7 微米吸收光谱范围内的年龄和化学成分的模型。此外，在低金属丰度下更好的参数覆盖允许计算年轻至 500 Myr 的模型，并充分考虑老年种群的蓝色水平分支阶段。我们提出了采用两组独立恒星参数（T_eff、logg、[Z/H]）的模型。在一种新颖的方法中，它们的可靠性得到了测试' 使用恒星种群模型本身“在飞行中”。我们对银河系和麦哲伦星云球状星团进行了测试，发现新模型非常好地恢复了它们的年龄和金属丰度，均匀校准集的系统性低至几个百分点。我们还拟合了 MaNGA 星系光谱，找到了与最先进模型相比的几个百分点的残差，但现在在更宽的波长范围内。