Mapping the Youngest and most Massive Stars in the Tarantula nebula and beyond

大质量恒星是宇宙的主要化学和动力引擎，也是解释高红移星系现象的关键。研究早期再电离时代和第一个星系的形成，非常明亮的超新星，伽马射线爆发和引力波事件的速率，需要了解宇宙中诞生的最大质量恒星。然而，超大质量恒星的形成和演化仍然是不确定的。这种知识的缺乏会影响到星系中恒星形成的研究，在这些星系中，个别恒星仍未得到解决，从而模糊了结论。在进一步研究更遥远的星系之前，必须了解银河系和本星系群中最大质量恒星的演化和形成。对大多数大质量星团进行系统的光谱分析是解决这一问题、证实或驳斥恒星演化理论的基础。在2020年，我们启动了MYMST项目来绘制NGC 2070，它拥有本星系群中最强大的恒星形成区域之一，也是离我们最近的，为仔细研究最大质量恒星的演化提供了最佳基准。基于MUSE的数据，我们使用MUSE窄场模式的空间分辨率与HST相当，对星团的恒星含量进行了光谱分析，并穿透了其核心R136。在该项目的第二阶段（MYMST II），我们的目标是完成对R136的检查，并通过额外的MUSE观测和使用其他仪器（例如JWST和ERIS）研究恒星和星际介质的变异性。我们将解决最大质量的沃尔夫-拉叶星的恒星风的延伸，并研究反馈机制。我们还将利用MUSE和4MOST之间的协同作用，在麦哲伦星云的赫茨普龙-罗素图中创建最全面的OB恒星光谱考古图。作为MYMST II项目的一部分，我们将开发创新工具来可视化和分析数据集，为研究人员和公众提供新的、开放的工具。

Massive stars are the main chemical and dynamic engines of the Universe and key to interpreting phenomena in high-redshift galaxies. Studying the early reionization epoch and formation of the first galaxies, the rates of very luminous supernovae, gamma-ray bursts, and gravitational wave events requires understanding the most massive stars born in the Universe. Nevertheless, the formation and evolution of very massive stars are still uncertain. This lack of knowledge propagates to star formation studies in galaxies where individual stars remain unresolved, thus blurring the conclusions. It is mandatory to understand the evolution and formation of the most massive stars in the Milky Way and Local Group before moving forward to more distant galaxies. Systematic spectroscopic analyses in the most massive clusters are fundamental to addressing this problem, confirming or refuting stellar evolutionary theories. In 2020, we launched the MYMST project to chart NGC 2070, which harbors one of the most powerful star-forming regions in the Local Group and is also the closest to us, providing an optimal benchmark for scrutinizing the evolution of the most massive stars. Based on MUSE data, we spectroscopically examined the stellar content of the cluster and pierced its core, R136, using MUSE narrow-field mode's spatial resolution comparable to that of the HST. In the second phase of this project (the MYMST II), we aim to finalize the examination of R136 and study the variability of the stars and interstellar medium via additional MUSE observations and use of other instruments (e.g., JWST and ERIS). We will resolve the extend of stellar winds of the most massive Wolf-Rayet stars and investigate feedback mechanisms. We will also utilize synergies between MUSE and 4MOST to create the most comprehensive spectroscopic archaeological maps of OB stars in the Hertzsprung-Russell diagram in the Magellanic Clouds. As part of the MYMST II undertaking, we will develop innovative tools to visualize and analyze the datasets, offering new, open tools for both researchers and the general public.