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arXiv 2403.08067astro-ph.GAastro-ph.SR
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使用 APOGEE 进行化学制图：来自第17次数据发布的288,789颗恒星的双过程参数与残余丰度

Chemical Cartography with APOGEE: Two-process Parameters and Residual Abundances for 288,789 Stars from Data Release 17

Tawny Sit, David H. Weinberg, Adam Wheeler, Christian R. Hayes, Sten Hasselquist, Thomas Masseron, Jennifer Sobeck

备注：
Updated to ApJ accepted version. 35 pages, 18 figures, 5 tables. Catalog available at https://doi.org/10.5281/zenodo.10659205
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AI总结：

本研究校准APOGEE中288,789颗恒星的17种元素丰度，用核心坍缩与Ia型超新星双过程模型提取振幅和残余丰度，并揭示星团与矮星系的化学特征。

摘要：

恒星丰度测量会受到系统误差影响，这些误差会在元素丰度模式中引入额外离散和人为相关性。我们推导了经验校准偏移，以消除 SDSS APOGEE 巡天中288,789颗演化恒星的17种元素丰度随表面重力 $\log(g)$ 变化的系统趋势。我们将这些经校正的丰度拟合为追踪核心坍缩超新星的快速过程与追踪Ia型超新星的延迟过程之和，从而把每颗恒星的测量值重新表示为振幅 $A_{\text{cc}}$ 和 $A_{\text{Ia}}$，以及由该双参数拟合得到的逐元素残余量。作为该星表的首个应用——其规模比以往采用受限 $\log(g)$ 范围的分析大8倍——我们考察了14个疏散星团、9个球状星团和4个矮卫星星系的中位残余丰度。相对于银河系场盘星，年龄小于2 Gyr的疏散星团显示出中子俘获元素Ce约 $0.1-0.2$ dex 的增强，而两个年龄小于0.5 Gyr的星团还显示出C+N、Na、S和Cu水平升高。球状星团显示C+N、Na、Al和Ce的中位丰度升高，并且相关丰度残余遵循此前已知的趋势。四个矮卫星星系尽管具有不同的恒星形成历史，却显示出相似的残余丰度模式：C+N、Na和Al贫化约 $0.2-0.3$ dex，Ni、V、Mn和Co贫化约 $0.1$ dex。我们提供了包含经校正的APOGEE丰度、双过程振幅和残余丰度的星表，这将有助于未来研究不同恒星族群中的丰度模式，以及影响星系化学演化的其他增丰过程。

英文摘要：

Stellar abundance measurements are subject to systematic errors that induce extra scatter and artificial correlations in elemental abundance patterns. We derive empirical calibration offsets to remove systematic trends with surface gravity $\log(g)$ in 17 elemental abundances of 288,789 evolved stars from the SDSS APOGEE survey. We fit these corrected abundances as the sum of a prompt process tracing core-collapse supernovae and a delayed process tracing Type Ia supernovae, thus recasting each star's measurements into the amplitudes $A_{\text{cc}}$ and $A_{\text{Ia}}$ and the element-by-element residuals from this two-parameter fit. As a first application of this catalog, which is $8\times$ larger than that of previous analyses that used a restricted $\log(g)$ range, we examine the median residual abundances of 14 open clusters, nine globular clusters, and four dwarf satellite galaxies. Relative to field Milky Way disk stars, the open clusters younger than 2 Gyr show $\approx 0.1-0.2$ dex enhancements of the neutron-capture element Ce, and the two clusters younger than 0.5 Gyr also show elevated levels of C+N, Na, S, and Cu. Globular clusters show elevated median abundances of C+N, Na, Al, and Ce, and correlated abundance residuals that follow previously known trends. The four dwarf satellites show similar residual abundance patterns despite their different star formation histories, with $\approx 0.2-0.3$ dex depletions in C+N, Na, and Al and $\approx 0.1$ dex depletions in Ni, V, Mn, and Co. We provide our catalog of corrected APOGEE abundances, two-process amplitudes, and residual abundances, which will be valuable for future studies of abundance patterns in different stellar populations and of additional enrichment processes that affect galactic chemical evolution.

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