The Origins of Massive Galaxies

当今宇宙中的大多数恒星都存在于大质量星系中，这些星系主要形成于z = 1之前的60亿年。对这些星系形成过程的详细研究对于我们全面了解星系演化至关重要。然而，在z bbb101观测它们的形成带来了巨大的挑战。OMG项目将通过精确测量大质量星系的物理特性，从z = 1到第一个十亿年，彻底改变我们的理解。这将通过我在使用两种变革性新仪器的三个关键观测项目中发挥领导作用来实现。首先是詹姆斯·韦伯太空望远镜，我是第一周期光谱项目的PI，也是PRIMER大型成像项目的核心团队成员。其次是多目标光学和近红外光谱仪（MOONS），我是200夜GTO计划的工作组负责人。该项目还将利用我在星系光谱拟合方面的领先专业知识，这是通过我开发的广泛使用的Bagpipes代码建立起来的。OMG团队将追求三个关键的研究主题：(i)第一批大质量星系的出现：大质量星系在前20亿年的数量密度和恒星形成历史是什么（z > 3）；这些是否表明了这个时代恒星形成物理学的根本差异？（ii）宇宙午时大质量星系的升起：z = 1 - 2时大质量星系的恒星年龄和金属丰度是什么；模拟能准确再现这些属性吗？（iii）大质量星系的形态转换：z >1大质量星系的形态和分辨年龄是什么；这些如何约束淬灭物理？总而言之，OMG团队将使用最新的数据和分析技术来描述zbbb101大质量星系。通过将我们的结果与最先进的模拟相结合，我们将建立对驱动这一关键种群形成的物理的详细理解。

The majority of stars in the present-day Universe reside in massive galaxies, primarily formed during the first six billion years prior to z = 1. Detailed studies of the processes that shaped these galaxies are critical for our overall understanding of galaxy evolution. However, observing their formation at z > 1 presents huge challenges. The OMG project will revolutionise our understanding by precisely measuring the physical properties of massive galaxies, from z = 1 back to the first billion years. This will be achieved via my leading roles in three key observing programmes using two transformative new instruments. Firstly, the James Webb Space Telescope, for which I am PI of a Cycle 1 spectroscopic programme, and a core team member of the PRIMER large imaging programme. Secondly, the Multi-Object Optical and Near-infrared Spectrograph (MOONS), for which I am a working group leader in the 200-night GTO programme. The project will also exploit my leading expertise in galaxy spectral fitting, established via my development of the widely used Bagpipes code. The OMG team will pursue three key research themes: (i) The emergence of the first massive galaxies: what are the number densities and star-formation histories of massive galaxies in the first two billion years (z > 3); do these suggest fundamental differences in star-formation physics at this epoch? (ii) The rise of massive galaxies at cosmic noon: what are the stellar ages and metallicities of massive galaxies at z = 1 - 2; do simulations accurately reproduce these properties? (iii) Morphological transformations in massive galaxies: what are the morphologies and resolved ages of z > 1 massive galaxies; how do these constrain quenching physics? In summary, the OMG team will use the latest data and analysis techniques to characterise z > 1 massive galaxies. By combining our results with state-of-the-art simulations, we will build a detailed understanding of the physics driving the formation of this key population.