The Open Cluster Chemical Abundances and Mapping Survey. IV. Abundances for 128 Open Clusters Using SDSS/APOGEE DR16
The Open Cluster Chemical Abundances and Mapping Survey. IV. Abundances for 128 Open Clusters Using SDSS/APOGEE DR16
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DOI：
10.3847/1538-3881/ab77bc
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发表时间：
2020-02
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通讯作者：
J. Donor;P. Frinchaboy;K. Cunha;J. O’Connell;C. Prieto;Andr'es Almeida;F. Anders;R. Beaton
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文献类型：
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作者：
J. Donor;P. Frinchaboy;K. Cunha;J. O’Connell;C. Prieto;Andr'es Almeida;F. Anders;R. Beaton
疏散星团化学丰度和绘图（OCCAM）调查旨在通过构建数百个疏散星团的大型，全面，统一，基于红外的光谱数据集来限制关键的银河系动力学和化学演化参数。这是OCCAM巡天的第四个贡献，介绍了使用Sloan Digital Sky Survey/APOGEE DR 16对128个疏散星团样本的分析，其中71个我们根据它们的颜色-星等图的外观指定为“高质量”。我们发现APOGEE DR 16衍生的[Fe/H]丰度与以前的高分辨率光谱疏散星团丰度的研究是很好的协议。使用高质量的样品，我们测量了银河系中16种元素的丰度梯度，并发现了一些[X/Fe]梯度随年龄的变化。我们发现在6 < RGC < 13.9 kpc的范围内，银河系[Fe/H]与RGC的整体梯度为−0.068 ± 0.001 dex kpc−1;然而，我们注意到这个结果对所使用的距离表很敏感，变化高达15%。我们正式推导出一个突破的位置在[Fe/H]丰度梯度作为一个自由参数的梯度拟合的第一次。我们还测量了O，Mg，S，Ca，Mn，Cr，Cu，Na，Al和K的显着银河系梯度，其中一些是第一次测量。我们的大样本使我们能够检查四个人口稠密的年龄箱，以探索大量元素的梯度的时间演化，并评论可能对银河系化学演化和径向迁移的影响。
The Open Cluster Chemical Abundances and Mapping (OCCAM) survey aims to constrain key Galactic dynamical and chemical evolution parameters by the construction of a large, comprehensive, uniform, infrared-based spectroscopic data set of hundreds of open clusters. This fourth contribution from the OCCAM survey presents analysis using Sloan Digital Sky Survey/APOGEE DR16 of a sample of 128 open clusters, 71 of which we designate to be “high quality” based on the appearance of their color–magnitude diagram. We find the APOGEE DR16 derived [Fe/H] abundances to be in good agreement with previous high-resolution spectroscopic open cluster abundance studies. Using the high-quality sample, we measure Galactic abundance gradients in 16 elements, and find evolution of some of the [X/Fe] gradients as a function of age. We find an overall Galactic [Fe/H] versus RGC gradient of −0.068 ± 0.001 dex kpc−1 over the range of 6 < RGC < 13.9 kpc; however, we note that this result is sensitive to the distance catalog used, varying as much as 15%. We formally derive the location of a break in the [Fe/H] abundance gradient as a free parameter in the gradient fit for the first time. We also measure significant Galactic gradients in O, Mg, S, Ca, Mn, Cr, Cu, Na, Al, and K, some of which are measured for the first time. Our large sample allows us to examine four well-populated age bins in order to explore the time evolution of gradients for a large number of elements and comment on possible implications for Galactic chemical evolution and radial migration.