Stellar Population Models Based on the Milky Way Interstellar Medium-Corrected MaStar Stellar Library

This file contains simple stellar population (SSP) model spectra constructed from a version of the SDSS-IV MaNGA Stellar Library (MaStar; Yan et al. 2019, Abdurro'uf et al. 2022) that has been corrected for the effects of absorption in the CaII 3934, 3969 and NaI D 5891, 5897 transitions arising in the Milky Way's interstellar medium (ISM). These corrections are described in full in Rubin et al. (2025), and our approach to constructing these SSP models is described in Maraston et al. (2020) and Rubin et al. (2025). In brief, our models are calculated with the evolutionary population synthesis code of Maraston (2005), which is based on the fuel consumption theorem for the evaluation of the energetics of post-Main Sequence phases. We use the calibrated median values of the stellar parameters calculated for the MaStar sample to generate representative stellar spectra as functions of effective temperature, surface gravity, and chemical composition. These representative spectra are then used as input for the stellar population models. The stellar parameter estimates are described in R. Yan et al. (2025, in preparation) and at https://www.sdss4.org/dr17/mastar/mastar-stellar-parameters/. We calculate SSPs using stars in metallicity bins centered at [Z/H] = -1.35, -0.33, 0.0, and +0.35 with an approximate bin width of 0.1 dex assuming a Salpeter IMF. The SSP ages span 3 Myr to 15 Gyr and are calculated at 51 gridpoints. For comparison, we also calculate the equivalent SSPs using the uncorrected MaStar spectra. The datamodel is described below. HDU1: 51 x 4 x 1 x 3 matrix describing the parameters of each SSP spectrum. Each gridpoint (i,j,k) contains a 3-element array listing the age (in Gyr), metallicity, and IMF slope (in linear mass units) HDU2: 2 x 4563 array containing the vacuum wavelength and spectral resolution (R) grids for models constructed from the uncorrected (original) stellar library. The wavelength sampling is logarithmic and the wavelengths have units of Angstroms. R = wave / (FWHM dwave) HDU3: 51 x 4 x 1 x 4563 matrix containing the SSPs constructed from the uncorrected (original) stellar library in units of erg/s/Ang/Msun HDU4: 2 x 4542 array containing the vacuum wavelength and spectral resolution (R) grids for models constructed from the corrected (cleaned) stellar library. The wavelength sampling is logarithmic and the wavelengths have units of Angstroms. R = wave / (FWHM dwave) HDU5: 51 x 4 x 1 x 4542 matrix containing the SSPs constructed from the corrected (cleaned) stellar library in units of erg/s/Ang/Msun本数据集包含基于修正版斯隆数字巡天-IV（SDSS-IV）MaNGA恒星库（MaStar; Yan et al. 2019, Abdurro'uf et al. 2022）构建的简单恒星种群（SSP, Simple Stellar Population）模型光谱，该修正版本针对银河系星际介质（ISM, Interstellar Medium）中产生的CaII 3934、3969与NaI D 5891、5897谱线的吸收效应完成了校正。相关校正的完整细节披露于Rubin等人（2025）的研究中，而本团队构建此类SSP模型的方法则详见Maraston等人（2020）与Rubin等人（2025）的工作。简言之，本模型基于Maraston（2005）提出的演化种群合成代码构建，该代码依托燃料消耗定理评估主序后演化阶段的能量学特征。我们采用针对MaStar样本校准得到的恒星参数中位数，生成作为有效温度、表面重力与化学组成函数的代表性恒星光谱，并将这些光谱作为恒星种群模型的输入。关于恒星参数估算方法的细节，可参见R. Yan等人（2025，待刊）以及公开网址https://www.sdss4.org/dr17/mastar/mastar-stellar-parameters/。 我们以萨尔皮特初始质量函数（IMF, Initial Mass Function）为基础，在以[Z/H] = -1.35、-0.33、0.0与+0.35为中心的金属丰度区间内构建SSP模型，各区间近似宽度为0.1 dex。SSP的年龄覆盖范围为3 Myr至15 Gyr，共设置51个网格点完成计算。为便于对比，我们同时使用未经校正的原始MaStar光谱构建了等效的SSP模型。数据模型说明如下： HDU1：为51×4×1×3的矩阵，用于描述每条SSP光谱的参数。每个网格点(i,j,k)对应一个三元数组，依次列出年龄（单位：Gyr）、金属丰度与初始质量函数斜率（以线性质量单位计）。 HDU2：为2×4563的数组，包含基于未经校正（原始）恒星库构建的模型的真空波长与光谱分辨率（R）网格。波长采样采用对数形式，单位为埃（Å），光谱分辨率定义为R = λ / (FWHM·Δλ)。 HDU3：为51×4×1×4563的矩阵，存储基于未经校正（原始）恒星库构建的SSP模型光谱，单位为erg/s/Å/M☉。 HDU4：为2×4542的数组，包含基于经校正（清洁化）恒星库构建的模型的真空波长与光谱分辨率（R）网格。波长采样采用对数形式，单位为埃（Å），光谱分辨率定义为R = λ / (FWHM·Δλ)。 HDU5：为51×4×1×4542的矩阵，存储基于经校正（清洁化）恒星库构建的SSP模型光谱，单位为erg/s/Å/M☉。