论文标题
使用条件丰度评估的银河系磁盘的化学富集
The chemical enrichment of the Milky Way disk evaluated using conditional abundances
论文作者
论文摘要
银河系磁盘中恒星的化学丰度是其丰富历史的经验示踪剂。但是，他们捕获了对拆卸有价值的联合信息。在这项工作中，我们试图量化固定的超新星贡献（[fe/h]，[mg/fe]）的各个磁盘的整个半径如何演变。我们使用18,135个Apogee DR17红色团星和7,943 Galah DR3主序列星，分别在$ 3-13 $ kpc和$ 6.5-9.5 $ kpc上比较（[Fe/H]，[mg/h]，[mg/h]，[mg/fe]）的丰度分布。我们总共检查了15个要素：C，N，Al，K（Light），O，Si，S，Ca，（$α$），MN，NI，CR，CU，（Iron-Peak）CE，BA（S-Process）和EU（R-Process）。我们发现，条件中子捕获和光元素在磁盘的富集历史中最显着痕迹变化，具有绝对条件径向梯度$ \ leq 0.03 $ dex/kpc。所研究的其他元素具有绝对条件梯度$ \ Lessim 0.01 $ dex/kpc。我们发现了低$α$的[Fe/H]的结构化条件丰度变化，而不是高$α$序列。在不同半径处的平均条件丰度之间的平均散射为$σ_\ text {intinsic} \大约$ 0.02 dex（带有ce，eu，ba $σ_\ text {intinsic}> $ 0.05 dex）。这些结果是对不同元素一旦考虑到信托超新星相关性的痕量径向径向富集历史的量度的量度。此外，我们在条件丰度分布的所有时刻中发现了细微的系统变化，这可能会限制银河系的化学演化模型。
Chemical abundances of stars in the Milky Way disk are empirical tracers of its enrichment history. However, they capture joint-information that is valuable to disentangle. In this work, we seek to quantify how individual abundances evolve across the present-day radius of the disk, at fixed supernovae contribution ([Fe/H], [Mg/Fe]). We use 18,135 APOGEE DR17 red clump stars and 7,943 GALAH DR3 main sequence stars to compare the abundance distributions conditioned on ([Fe/H], [Mg/Fe]) across $3-13$ kpc and $6.5-9.5$ kpc, respectively. In total we examine 15 elements: C, N, Al, K (light), O, Si, S, Ca, ($α$), Mn, Ni, Cr, Cu, (iron-peak) Ce, Ba (s-process) and Eu (r-process). We find that the conditional neutron capture and light elements most significantly trace variations in the disk's enrichment history, with absolute conditional radial gradients $\leq 0.03$ dex/kpc. The other elements studied have absolute conditional gradients $\lesssim 0.01$ dex/kpc. We uncover structured conditional abundance variations as a function of [Fe/H] for the low-$α$, but not the high-$α$ sequence. The average scatter between the mean conditional abundances at different radii is $σ_\text{intrinsic} \approx$ 0.02 dex (with Ce, Eu, Ba $σ_\text{intrinsic} >$ 0.05 dex). These results serve as a measure of the magnitude via which different elements trace Galactic radial enrichment history once fiducial supernovae correlations are accounted for. Furthermore, we uncover subtle systematic variations in all moments of the conditional abundance distributions that will presumably constrain chemical evolution models of the Galaxy.
