We present an overview of the Middle Ages Galaxy Properties with Integral Field Spectroscopy (MAGPI) survey, a Large Program on the European Southern Observatory Very Large Telescope. MAGPI is designed to study the physical drivers of galaxy transformation at a lookback time of 3–4 Gyr, during which the dynamical, morphological, and chemical properties of galaxies are predicted to evolve significantly. The survey uses new medium-deep adaptive optics aided Multi-Unit Spectroscopic Explorer (MUSE) observations of fields selected from the Galaxy and Mass Assembly (GAMA) survey, providing a wealth of publicly available ancillary multi-wavelength data. With these data, MAGPI will map the kinematic and chemical properties of stars and ionised gas for a sample of 60 massive ( ${>}7 \times 10^{10} {\mathrm{M}}_\odot$ ) central galaxies at $0.25 < z <0.35$ in a representative range of environments (isolated, groups and clusters). The spatial resolution delivered by MUSE with Ground Layer Adaptive Optics ( $0.6-0.8$ arcsec FWHM) will facilitate a direct comparison with Integral Field Spectroscopy surveys of the nearby Universe, such as SAMI and MaNGA, and at higher redshifts using adaptive optics, for example, SINS. In addition to the primary (central) galaxy sample, MAGPI will deliver resolved and unresolved spectra for as many as 150 satellite galaxies at $0.25 < z <0.35$ , as well as hundreds of emission-line sources at $z < 6$ . This paper outlines the science goals, survey design, and observing strategy of MAGPI. We also present a first look at the MAGPI data, and the theoretical framework to which MAGPI data will be compared using the current generation of cosmological hydrodynamical simulations including EAGLE, Magneticum, HORIZON-AGN, and Illustris-TNG. Our results show that cosmological hydrodynamical simulations make discrepant predictions in the spatially resolved properties of galaxies at $z\approx 0.3$ . MAGPI observations will place new constraints and allow for tangible improvements in galaxy formation theory.

中文翻译：

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MAGPI 调查：科学目标、设计、观测策略、早期结果和理论框架

我们概述了米中间一种格斯G阿拉西磷与一世积分场光谱（MAGPI）调查，欧洲南方天文台超大望远镜的一个大型项目。MAGPI 旨在研究星系转变的物理驱动因素，回顾时间为 3-4 Gyr，在此期间，预计星系的动力学、形态和化学性质将发生显着变化。该调查使用新的中深度自适应光学辅助多单位光谱探测器（MUSE）对从银河和质量组装（GAMA）调查中选择的场进行观测，提供大量公开可用的辅助多波长数据。有了这些数据，MAGPI 将为 60 个大质量 ( ${>}7 \times 10^{10} {\mathrm{M}}_\odot$ ) 中央星系在 $0.25 < z <0.35$ 在具有代表性的环境范围内（隔离、组和集群）。MUSE 提供的空间分辨率与地面层自适应光学 ( $0.6-0.8$ arcsec FWHM）将有助于与附近宇宙的积分场光谱调查（例如 SAMI 和 MaNGA）以及使用自适应光学（例如 SINS）的更高红移进行直接比较。除了主要（中央）星系样本外，MAGPI 还将提供多达 150 个卫星星系的已解析和未解析光谱 $0.25 < z <0.35$ ，以及数百个发射线源 $z < 6$ . 本文概述了 MAGPI 的科学目标、调查设计和观测策略。我们还首次介绍了 MAGPI 数据，以及将使用当前一代的宇宙学流体动力学模拟与 MAGPI 数据进行比较的理论框架，包括鹰,磁,地平线-AGN， 和插画-TNG. 我们的结果表明，宇宙学流体动力学模拟对星系的空间分辨特性做出了不一致的预测 $z\约 0.3$ . MAGPI 观测将带来新的限制，并允许对星系形成理论进行切实的改进。