The Fornax 3D project: Globular clusters tracing kinematics and metallicities
The Fornax 3D project: Globular clusters tracing kinematics and metallicities
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DOI：
10.1051/0004-6361/202037685
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发表时间：
2020-03
影响因子：
6.5
通讯作者：
K. Fahrion;M. Lyubenova;M. Hilker;G. Ven;J. Falc'on-Barroso;Robert Leaman;I. Mart'in-Navarro;A. Bittner;L. Coccato;E. Corsini;D. Gadotti;E. Iodice;R. McDermid;F. Pinna;M. Sarzi;S. Viaene;P. Zeeuw;L. Zhu
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作者：
K. Fahrion;M. Lyubenova;M. Hilker;G. Ven;J. Falc'on-Barroso;Robert Leaman;I. Mart'in-Navarro;A. Bittner;L. Coccato;E. Corsini;D. Gadotti;E. Iodice;R. McDermid;F. Pinna;M. Sarzi;S. Viaene;P. Zeeuw;L. Zhu
球状星团(GCs)普遍存在于大质量星系中，由于其年代久远，被认为是星系演化的化石记录。对GC系统的光谱研究通常局限于星系的外围，在那里GC在星系背景下脱颖而出，是星系组装的明亮示踪物。在这项工作中，我们利用多单元探测器光谱仪(MUSE)的能力提取了福尔纳克斯星系团中32个星系内部区域(≲3Reff)的722个GC的光谱样本。这些星系是作为Fornax 3D项目的一部分被观测到的，Fornax 3D项目是一项缪斯调查，目标是Fornax维里半径内的早期和晚期类型星系。在考虑了GC光谱中的星系背景后，我们提取了视线速度，并测定了238个GC子样的金属度。我们在GC系统中发现了自转的信号，并将GC运动学与恒星的运动学进行了比较，结果表明GC跟踪星系的椭球体。虽然红色的GC被证明与宿主星系的金属丰度轮廓密切相关，但蓝色的GC显示出大量的金属性分布，但它们通常比宿主星系更缺乏金属。
Globular clusters (GCs) are found ubiquitously in massive galaxies and due to their old ages, they are regarded as fossil records of galaxy evolution. Spectroscopic studies of GC systems are often limited to the outskirts of galaxies, where GCs stand out against the galaxy background and serve as bright tracers of galaxy assembly. In this work, we use the capabilities of the Multi Unit Explorer Spectrograph (MUSE) to extract a spectroscopic sample of 722 GCs in the inner regions (≲3 Reff) of 32 galaxies in the Fornax cluster. These galaxies were observed as part of the Fornax 3D project, a MUSE survey that targets early and late-type galaxies within the virial radius of Fornax. After accounting for the galaxy background in the GC spectra, we extracted line-of-sight velocities and determined metallicities of a sub-sample of 238 GCs. We found signatures of rotation within GC systems, and comparing the GC kinematics and that of the stellar body shows that the GCs trace the spheroid of the galaxies. While the red GCs prove to closely follow the metallicity profile of the host galaxy, the blue GCs show a large spread of metallicities but they are generally more metal-poor than the host.