论文标题
部分可观测时空混沌系统的无模型预测
New Generation Stellar Spectral Libraries in the Optical and Near-Infrared I: The Recalibrated UVES-POP Library for Stellar Population Synthesis
论文作者
论文摘要
我们提出了从波长范围320-1025 nm的uves-pop恒星库中重新处理的406颗恒星的通量校准光谱，可用于恒星种群合成。这些光谱在具有光谱解析功率r = 20,000和r = 80,000的两个版本中提供。使用我们开发的一些其他算法，使用了最新版本的uves数据减少管道来重新降低ESO数据存档的原始光谱。 The most significant improvements in comparison with the original UVES-POP release are: (i) an updated Echelle order merging, which eliminates "ripples" present in the published spectra, (ii) a full telluric correction, (iii) merging of non-overlapping UVES spectral setups taking into account the global continuum shape, (iv) a spectrophotometric correction and absolute flux calibration, and (v) estimates of星际灭绝。对于样本中的364星，我们计算了大气参数$ t_ \ mathrm {eff} $，表面重力log $ g $，金属性[Fe/h]和$α$ - 元素增强[$α$/fe]，通过使用基于合成stellar seltellar sellgor and a Greamsizizizizizion的全光谱拟合技术，通过使用全光谱拟合技术。我们还提供投影的旋转速度$ v \ sin i $和径向速度$ v_ {rad} $估计。重新处理的数据集中的总体绝对通量不确定性大于2％，而大约一半的恒星的准确性低于％。重新校准的乌维式流程与其他光谱文库的比较表明，在通量中的一致性非常好。同时，$ gaia $ dr3 bp/rp光谱通常与我们的数据相差，我们将其归因于$ gaia $ dr3的分光光度计校准问题。
We present re-processed flux calibrated spectra of 406 stars from the UVES-POP stellar library in the wavelength range 320-1025 nm, which can be used for stellar population synthesis. The spectra are provided in the two versions having spectral resolving power R=20,000 and R=80,000. Raw spectra from the ESO data archive were re-reduced using the latest version of the UVES data reduction pipeline with some additional algorithms that we developed. The most significant improvements in comparison with the original UVES-POP release are: (i) an updated Echelle order merging, which eliminates "ripples" present in the published spectra, (ii) a full telluric correction, (iii) merging of non-overlapping UVES spectral setups taking into account the global continuum shape, (iv) a spectrophotometric correction and absolute flux calibration, and (v) estimates of the interstellar extinction. For 364 stars from our sample, we computed atmospheric parameters $T_\mathrm{eff}$, surface gravity log $g$, metallicity [Fe/H], and $α$-element enhancement [$α$/Fe] by using a full spectrum fitting technique based on a grid of synthetic stellar atmospheres and a novel minimization algorithm. We also provide projected rotational velocity $v\sin i$ and radial velocity $v_{rad}$ estimates. The overall absolute flux uncertainty in the re-processed dataset is better than 2% with sub-% accuracy for about half of the stars. A comparison of the recalibrated UVES-POP spectra with other spectral libraries shows a very good agreement in flux; at the same time, $Gaia$ DR3 BP/RP spectra are often discrepant with our data, which we attribute to spectrophotometric calibration issues in $Gaia$ DR3.
