JINAbase—A Database for Chemical Abundances of Metal-poor Stars
JINAbase—A Database for Chemical Abundances of Metal-poor Stars
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DOI：
10.3847/1538-4365/aadfe9
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发表时间：
2017-11
期刊：
影响因子：
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通讯作者：
Abdu Abohalima;A. Frebel
中科院分区：
文献类型：
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作者：
Abdu Abohalima;A. Frebel
重建银河系的化学演化对于理解整个宇宙时间内恒星、行星和星系的形成至关重要。关于早期宇宙中元素的产生以及元素是如何融入气体和恒星的不同研究是必要的，以拼凑出元素是如何演化的。这些措施包括建立贫金属星设定的化学丰度趋势，将核合成产额预测与恒星丰度数据进行比较，以及化学演化的理论模型。为了帮助这些研究，我们从文献中收集了极贫金属星的化学丰度测量和其他信息，如恒星参数、坐标、星等和径向速度。该数据库名为JINABASE，包含1,659颗独特的恒星，其中60%具有[Fe/H]≤−2.5。这些信息与用户友好的可查询Web应用程序(http://jinabase.pythonanywhere.com).)一起存储在一个Sql数据库中具有独特化学元素特征的对象(例如，r过程星、S过程星和CEMP星)被标记为或可以被分类为这样。我们发现，使用[Fe/H]≤−2.0时，高达19%的贫金属星会出现不同的中子俘获元素特征，当考虑碳增强时，会出现32%的中子俘获元素特征。该Web应用程序允许从文献中快速选择定制的比较样本，以进行上述研究和其他更多研究。使用三颗研究最充分的贫金属星的多个条目，我们评估了不同研究之间化学丰度测量的系统不确定度。我们为希望了解贫金属星和化学丰度测量细节的非光谱学家提供了一个用于模型比较的化学元素选择的简要指南。
Reconstructing the chemical evolution of the Milky Way is crucial for understanding the formation of stars, planets, and galaxies throughout cosmic time. Different studies associated with element production in the early universe and how elements are incorporated into gas and stars are necessary to piece together how the elements evolved. These include establishing chemical abundance trends, as set by metal-poor stars, comparing nucleosynthesis yield predictions with stellar abundance data, and theoretical modeling of chemical evolution. To aid these studies, we have collected chemical abundance measurements and other information, such as stellar parameters, coordinates, magnitudes, and radial velocities, for extremely metal-poor stars from the literature. The database, JINAbase, contains 1659 unique stars, 60% of which have [Fe/H] ≤ −2.5. This information is stored in an SQL database, together with a user-friendly queryable web application (http://jinabase.pythonanywhere.com). Objects with unique chemical element signatures (e.g., r-process stars, s-process and CEMP stars) are labeled or can be classified as such. We find that the various neutron-capture element signatures occur in up to 19% of metal-poor stars with [Fe/H] ≤ −2.0, and 32% when also considering carbon enhancement. The web application enables fast selection of customized comparison samples from the literature for the aforementioned studies and many more. Using multiple entries for three of the most well-studied metal-poor stars, we evaluate systematic uncertainties of chemical abundance measurements between the different studies. We provide a brief guide to the selection of chemical elements for model comparisons for non-spectroscopists who wish to learn about metal-poor stars and the details of chemical abundance measurements.