Young massive star clusters in 3D - spectrophotometric mapping with MUSE

3D 年轻大质量星团 - 使用 MUSE 进行分光光度测绘

• 批准号: 398719443
• 负责人: Dr. Peter Zeidler
• 金额: --
• 依托单位: Space Telescope Science Instiute
• 依托单位国家: 德国
• 项目类别: Research Fellowships
• 财政年份: 2018
• 资助国家: 德国
• 起止时间: 2017-12-31 至 2020-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/398719443?language=en
• 关键词: Young; massive; star; clusters; 3D

Most stars form in clustered environments, of which the majority dissolve within a few million years forming the Galactic field population. The densest and most massive star clusters have the potential to remain gravitationally bound and might be long-lived. The physical processes and interactions between the stellar cluster population and its parental HII region are not very well understood. The properties of the majority of these young massive star clusters (YMCs) are difficult to access due to their location in other galaxies. This makes the Galactic YMCs important objects to study, yet, compared to starburst galaxies, YMCs are rare in the Milky Way (MW). For the first time, new instruments and telescopes make it possible to perform detailed, large scale spectroscopic surveys with a reasonable amount of telescope time.For the proposed two-year research project, I plan to perform a study of YMCs, specifically Westerlund 2 (Wd2), using data obtained with the integral field spectrograph MUSE to gain, for the absolute first time, a conclusive insight into the 3D structure, formation, present status, and future evolution of such a YMC. With an age of 1 – 2 Myr at a distance of 4 kpc, Wd2 is the second most massive YMC in the MW (total stellar mass: 37000 solar masses). This highly mass segregated YMC hosts a fully intact upper main sequence and is built from two coeval sub-clumps. These properties, the numerous OB stars, and the surrounding HII region makes Wd2 a perfect test bed to study the interactions of YMCs with their parental molecular gas cloud. Together with the existing deep, multi-epoch Hubble Space Telescope photometry this new instrument gives me the unique opportunity to simultaneously observe and examine the stellar population and the remaining gas to study their feedback and interactions. Determining the velocity dispersion of a large sample of cluster stars will provide information about massive clusters and their long-term stability toward internal and external influences, such as supernova explosions and gravitational interactions with giant molecular clouds or the Galactic disk. I will also address the question on how much the far ultra-violet flux of the OB stars impact the disk dispersal of protostellar disks around low-mass PMS stars. Faster dispersing disks mean that the low-mass stars will grow less in mass, which alters the stellar mass function of the cluster impacting the long-term stability.This project will help to adjust the initial parameters of N-body simulations to trace the long-term evolution of massive clusters over a significant fraction of a Hubble time. These simulations are essential to get a step closer to understand the link between the observed YMCs and the old globular cluster population. I will use Wd2 as an example case to develop new methods for reducing and analyzing such datasets, which will be extended to other YMCs in the MW and the more distant and more massive ones in the Magellanic Clouds.

大多数恒星是在星团环境中形成的，其中大多数恒星在数百万年内溶解，形成了银河系外场人口。密度最大、质量最大的星团有可能保持引力束缚，而且寿命可能很长。星系团和它的母体HII区之间的物理过程和相互作用还没有被很好地理解。这些年轻的大质量星团(YMC)中的大多数都很难获得，因为它们位于其他星系中。这使得银河系YMC成为重要的研究对象，然而，与恒星爆发星系相比，YMC在银河系(MW)中是罕见的。第一次，新的仪器和望远镜使得在合理的望远镜时间内进行详细的、大规模的光谱测量成为可能。在拟议的两年研究项目中，我计划对YMC进行研究，特别是Westlund 2(WD2)，使用从积分场光谱仪缪斯获得的数据，绝对第一次对这样的YMC的3D结构、形成、现状和未来的演变有一个决定性的洞察。WD2的年龄为1-2Myr，距离4kpc，是MW中质量第二大的YMC(总恒星质量：37000个太阳质量)。这种高度质量分离的YMC拥有一个完全完整的上主层序，并由两个同时代的亚块组成。这些性质、众多的OB星和周围的HII区使WD2成为研究YMC与其母分子气体云相互作用的完美试验台。与现有的深地、多纪元哈勃太空望远镜测光技术一起，这台新仪器给了我一个独特的机会，可以同时观察和检查恒星群和剩余气体，以研究它们的反馈和相互作用。确定大样本星团恒星的速度离散度将提供有关大质量星团及其对内部和外部影响的长期稳定性的信息，例如超新星爆炸和与巨型分子云或银盘的引力相互作用。我还将讨论OB恒星的远紫外线通量对低质量PMS恒星周围原恒星圆盘扩散的影响有多大这个问题。更快的弥散圆盘意味着低质量恒星的质量增长将减少，这将改变星团的恒星质量函数，影响长期稳定性。该项目将有助于调整N体模拟的初始参数，以跟踪大质量星团在哈勃时间的很大一部分时间内的长期演化。这些模拟对于进一步了解观测到的YMC和旧的球状星团种群之间的联系是至关重要的。我将以WD2为例，开发新的方法来减少和分析这样的数据集，这将扩展到MW中的其他YMC和更远、更大的麦哲伦云中的YMC。

项目成果

The Young Massive Star Cluster Westerlund 2 Observed with MUSE. I. First Results on the Cluster Internal Motion from Stellar Radial Velocities

• DOI: 10.3847/1538-3881/aae258
• 发表时间: 2018-09
• 期刊: The Astronomical Journal
• 作者: P. Zeidler;E. Sabbi;A. Nota;A. Pasquali;E. Grebel;A. McLeod;S. Kamann;M. Tosi;M. Cignoni

Star Clusters Near and Far

• DOI: 10.1007/s11214-020-00690-x
• 发表时间: 2020-05
• 期刊: Space Science Reviews
• 影响因子: 10.3
• 作者: A. Adamo;Peter Zeidler;Peter Zeidler;J. Kruijssen;M. Chevance;M. Gieles;D. Calzetti;Corinne Charbonnel;Corinne Charbonnel;H. Zinnecker;M. Krause

Stellar Feedback and Resolved Stellar IFU Spectroscopy in the Nearby Spiral Galaxy NGC 300

• DOI: 10.3847/1538-4357/ab6d63
• 发表时间: 2019-10
• 期刊: The Astrophysical Journal
• 作者: A. McLeod;J. Kruijssen;D. Weisz;Peter Zeidler;A. Schruba;J. Dalcanton;S. Longmore;M. Chevance;C. Faesi;N. Byler