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arXiv 1910.10554astro-ph.SRastro-ph.GA
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高分辨红外光谱中疏散星团的化学丰度。II。NGC 752

Chemical Abundances Of Open Clusters From High-Resolution Infrared Spectra. II. NGC 752

G. Böcek Topcu, M. Afsar, C. Sneden, C. A. Pilachowski, P. A. Denissenkov, D. A. VandenBerg, D. Wright, G. N. Mace, D. T. Jaffe, E. Strickland, H. Kim, K. R. Sokal

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16 pages, 11 figures
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摘要：

我们提出了一个详细的近红外化学丰度分析银河系疏散星团NGC 752的10个红巨星成员。高分辨率（R $\simeq$ 45000）近红外光谱数据是用浸没光栅红外光谱仪（IGRINS）收集的，可同时覆盖整个H和K波段。计算了氢燃烧元素（C，N，O）、$α$（Mg，Si，S，Ca）、轻奇Z元素（Na，Al，P，K）、铁族元素（Sc，Ti，Cr，Fe，Co，Ni）和中子俘获元素（Ce，Nd，Yb）的丰度。本文首次报道了NGC752中S、P、K、Ce和Yb的丰度。我们的分析产生了太阳的金属丰度和太阳丰度比几乎所有的元素都比NGC 752中的CNO组重。O和N丰度的测量从一些OH和CN的功能在$H$带，和C丰度主要是由CO分子线的K带。高激发\ion{C}{i}线存在于近红外和光学光谱中也包括在C丰度测定。碳同位素比值来自23440 ℃附近的第一泛音（2 - 0）和（3 $-$ 1）$^{12}$ CO和（2 - 0）$^{13}$ CO线以及23730 ℃附近的（3 - 1）$^{13}$ CO线的R分支带头。CNO丰度和$^{12}$ C/$^{13}$ C比值均与我们的巨人已完成CN-环产物的"首次挖掘"包络混合一致。我们独立评估了盖亚天体测量的NGC 752恒星成员资格，从而为这个星团绘制了一个新的颜色星等图。应用维多利亚等时线和MESA模型，这些数据产生更新的NGC 752星团年龄（1.52 Gyr）和演化阶段的指示程序的明星。光度学证据和光谱学的轻元素丰度都表明，大多数，也许是所有的程序星都是这个星团中燃烧氦的红色团块的成员。

英文摘要：

We present a detailed near-infrared chemical abundance analysis of 10 red giant members of the Galactic open cluster NGC 752. High-resolution (R$\simeq$45000) near-infrared spectral data were gathered with the Immersion Grating Infrared Spectrograph (IGRINS), providing simultaneous coverage of the complete H and K bands. We derived the abundances of H-burning (C, N, O), $α$ (Mg, Si, S, Ca), light odd-Z (Na, Al, P, K), Fe-group (Sc, Ti, Cr, Fe, Co, Ni) and neutron-capture (Ce, Nd, Yb) elements. We report the abundances of S, P, K, Ce, and Yb in NGC 752 for the first time. Our analysis yields solar metallicity and solar abundance ratios for almost all of the elements heavier than the CNO group in NGC 752. O and N abundances were measured from a number of OH and CN features in the $H$ band, and C abundances were determined mainly from CO molecular lines in the K band. High excitation \ion{C}{i} lines present in both near-infrared and optical spectra were also included in the C abundance determinations. Carbon isotopic ratios were derived from the R-branch band heads of first overtone (2-0) and (3$-$1) $^{12}$CO and (2-0) $^{13}$CO lines near 23440 Åand (3-1) $^{13}$CO lines at about 23730 Å. The CNO abundances and $^{12}$C/$^{13}$C ratios are all consistent with our giants having completed "first dredge-up" envelope mixing of CN-cyle products. We independently assessed NGC 752 stellar membership from Gaia astrometry, leading to a new color-magnitude diagram for this cluster. Applications of Victoria isochrones and MESA models to these data yield an updated NGC 752 cluster age (1.52 Gyr) and evolutionary stage indications for the program stars. The photometric evidence and spectroscopic light element abundances all suggest that the most, perhaps all of the program stars are members of the helium-burning red clump in this cluster.

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