APOGEE Chemical Abundance Patterns of the Massive Milky Way Satellites
APOGEE Chemical Abundance Patterns of the Massive Milky Way Satellites
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DOI：
10.3847/1538-4357/ac25f9
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发表时间：
2021-09
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通讯作者：
S. Hasselquist;C. Hayes;J. Lian;D. Weinberg;G. Zasowski;D. Horta;Rachael Beaton;D. Feuillet;E. R. Garro;C. Gallart;V. Smith;J. Holtzman;D. Minniti;I. Lacerna;M. Shetrone;H. Jönsson;M. Cioni;S. Fillingham;K. Cunha;R. O’Connell;J. G. Fern'andez-Trincado;R. Muñoz;R. Schiavon;Andr'es Almeida;B. Anguiano;T. Beers;D. Bizyaev;J. Brownstein;R. Cohen;P. Frinchaboy;D. A. Garc'ia-Hern'andez;D. Geisler;R. Lane;S. Majewski;D. Nidever;C. Nitschelm;Joshua Povick;A. Price-Whelan;A. Roman-Lopes;M. Rosado;J. Sobeck;G. Stringfellow;O. Valenzuela;S. Villanova;F. Vincenzo
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作者：
S. Hasselquist;C. Hayes;J. Lian;D. Weinberg;G. Zasowski;D. Horta;Rachael Beaton;D. Feuillet;E. R. Garro;C. Gallart;V. Smith;J. Holtzman;D. Minniti;I. Lacerna;M. Shetrone;H. Jönsson;M. Cioni;S. Fillingham;K. Cunha;R. O’Connell;J. G. Fern'andez-Trincado;R. Muñoz;R. Schiavon;Andr'es Almeida;B. Anguiano;T. Beers;D. Bizyaev;J. Brownstein;R. Cohen;P. Frinchaboy;D. A. Garc'ia-Hern'andez;D. Geisler;R. Lane;S. Majewski;D. Nidever;C. Nitschelm;Joshua Povick;A. Price-Whelan;A. Roman-Lopes;M. Rosado;J. Sobeck;G. Stringfellow;O. Valenzuela;S. Villanova;F. Vincenzo
SDSS-IV阿帕奇点天文台星系演化实验(APOEE)探测获得了分布在银河系(MW)大质量卫星星系(MW)中的数千颗红巨星的高分辨率光谱，这些星系包括大小麦哲伦星云(LMC/SMC)、人马座矮星系(SGR)、火神座(FNX)和现已完全解体的盖亚香肠/土卫二(GSE)系统。我们给出并分析了每个星系的远地点化学丰度模式，通过量化多元素(C、N、O、Mg、Al、Si、Ca、Fe、Ni和Ce)的相对丰度趋势，以及通过将化学演化模型拟合到每个星系的[α/Fe]-[Fe/H]丰度平面，从而得出关于其恒星形成历史的可靠结论。结果表明，Nidever等人观测到的麦哲伦星云(MCs)中恒星暴增的化学特征。在α中，元素丰度延伸到C+N、Al和Ni，其中SMC的主要爆发发生在LMC爆发之前约3-4Gyr。我们发现SGR和Fnx也表现出暗示二次星形成时期的化学丰度模式，但这些事件比在MC中观察到的事件更弱和更早(∼5-7Gyr前)。没有化学证据表明在GSE中发生了第二次恒星爆发，但与其他四个星系相比，这个星系显示出最强的初始恒星形成。所有矮小星系中AGB星对其富集度的相对贡献都大于MW。对比这些化学模式，突出了银河系环境对其化学演化的重要性。
The SDSS-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey has obtained high-resolution spectra for thousands of red giant stars distributed among the massive satellite galaxies of the Milky Way (MW): the Large and Small Magellanic Clouds (LMC/SMC), the Sagittarius Dwarf Galaxy (Sgr), Fornax (Fnx), and the now fully disrupted Gaia Sausage/Enceladus (GSE) system. We present and analyze the APOGEE chemical abundance patterns of each galaxy to draw robust conclusions about their star formation histories, by quantifying the relative abundance trends of multiple elements (C, N, O, Mg, Al, Si, Ca, Fe, Ni, and Ce), as well as by fitting chemical evolution models to the [α/Fe]–[Fe/H] abundance plane for each galaxy. Results show that the chemical signatures of the starburst in the Magellanic Clouds (MCs) observed by Nidever et al. in the α-element abundances extend to C+N, Al, and Ni, with the major burst in the SMC occurring some 3–4 Gyr before the burst in the LMC. We find that Sgr and Fnx also exhibit chemical abundance patterns suggestive of secondary star formation epochs, but these events were weaker and earlier (∼5–7 Gyr ago) than those observed in the MCs. There is no chemical evidence of a second starburst in GSE, but this galaxy shows the strongest initial star formation as compared to the other four galaxies. All dwarf galaxies had greater relative contributions of AGB stars to their enrichment than the MW. Comparing and contrasting these chemical patterns highlight the importance of galaxy environment on its chemical evolution.