Gas flows play a fundamental role in galaxy formation and evolution, providing the fuel for the star formation process. These mechanisms leave an imprint in the amount of heavy elements. Thus, the analysis of this metallicity signature provides additional constraint on the galaxy formation scenario. We aim to discriminate between four different galaxy formation models based on two accretion scenarios and two different star formation recipes. We address the impact of a bimodal accretion scenario and a strongly regulated star formation recipe. We present a new extension of the eGalICS model, which allows us to track the metal enrichment process. Our new chemodynamical model is applicable for situations ranging from metal-free primordial accretion to very enriched interstellar gas contents. We use this new tool to predict the metallicity evolution of both the stellar populations and gas phase. We also address the evolution of the gas metallicity with the star formation rate (SFR). We then focus on a sub-sample of Milky Way-like galaxies. We compare both the cosmic stellar mass assembly and the metal enrichment process of such galaxies with observations and detailed chemical evolution models. Our models, based on a strong star formation regulation, allow us to reproduce well the stellar mass to gas-phase metallicity relation observed in the local universe. However, we observe a systematic shift towards high masses. Our $Mstar-Zg-SFR relation is in good agreement with recent measurements: our best model predicts a clear dependence with the SFR. Both SFR and metal enrichment histories of our Milky Way-like galaxies are consistent with observational measurements and detailed chemical evolution models. We finally show that Milky Way progenitors start their evolution below the observed main sequence and progressively reach this observed relation at z = 0.
Milky Way Mapper decoded abundances -- II: From patterns to paths
Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）；Department of Astronomy, Columbia University（哥伦比亚大学天文学系）；Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado（科罗拉多大学天体物理学与行星科学系天体物理学与空间天文中心）；Department of Physics & Astronomy, University of Utah（犹他大学物理与天文学系）；Department of Physics and Astronomy, Vanderbilt University（范德堡大学物理与天文学系）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）；School of Physics and Astronomy, Monash University（莫纳什大学物理与天文学院）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）；Center for Cosmology and Astroparticle Physics (CCAPP), The Ohio State University（俄亥俄州立大学宇宙学与高能粒子物理中心）
The disrupted chemical enrichment history of the Milky Way driven by gas accretion
South-Western Institute for Astronomy Research, Yunnan University（西南天文研究所，云南大学）；Yunnan Key Laboratory of Survey Science, Yunnan University（云南省测绘科学重点实验室，云南大学）；Department of Astronomy, Xiamen University（天文学系，厦门大学）；Institute of Astronomy, University of Cambridge（天文学研究所，剑桥大学）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（天文与空间科学学院，中国科学院大学）；National Astronomical Observatories, Chinese Academy of Sciences（国家天文台，中国科学院）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（天文与天体物理前沿研究院，北京师范大学）；Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences（射电天文与技术重点实验室，中国科学院）
Milky Way Mapper decoded abundances -- I. Shared disc enrichment patterns
Australian National University（澳大利亚国立大学）；Columbia University（哥伦比亚大学）；University of Colorado（科罗拉多大学）；University of Utah（犹他大学）；Vanderbilt University（范德堡大学）；Flatiron Institute（平顿研究所）；Monash University（莫纳什大学）；The Ohio State University（俄亥俄州立大学）；New York University（纽约大学）
Ripples of Stellar Enrichment (RoSE) - simulating element production and mixing in a Milky Way-mass galactic disc star-by-star
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）；Centre for Extragalactic Astronomy, Department of Physics, Durham University（杜伦大学物理系河外天文中心）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学柯立夫天文与天体物理研究所）
The colour-magnitude relation of Globular Clusters in Centaurus and Hydra - Constraints on star cluster self-enrichment with a link to massive Milky Way GCs
Chemical Taxonomy of $ω$~Centauri: Ten Populations Reveal a Multi-Phase Enrichment History
Institute of Graduate Studies in Science, Istanbul University（伊斯坦布尔大学研究生科学院）；Faculty of Science, Department of Astronomy and Space Sciences, Istanbul University（伊斯坦布尔大学理学院天文与空间科学系）；Department of Space Sciences and Technologies, Faculty of Science, Akdeniz University（安塔利亚阿特纳兹大学理学院空间科学与技术系）
ISM metallicity variations across spiral arms in disk galaxies: the impact of local enrichment and gas migration in the presence of radial metallicity gradient
The Stellar Abundances for Galactic Archaeology (SAGA) Database III - Analysis of Enrichment Histories for Elements and Two Modes of Star Formation during the Early Evolution of Milky Way
Abundances of planetary nebulae and evolved stars: Iron and sulfur depletion, and carbon and nitrogen enrichment, in low- and intermediate-mass stellar populations in the Milky Way
Nitrogen-Loud Quasars from the Dark Energy Spectroscopic Instrument. II. Broad-Line Region Metallicity and Relative Nitrogen Enrichment
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Technology and Engineering Center for Space Utilization, Chinese Academy of Sciences（中国科学院空间应用工程与技术中心）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文学院）；Key Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所粒子天体物理重点实验室）
Mass Assembly and Chemical Complexity in the Milky Way
UK Astronomy Technology Centre（英国天文技术中心）；University of Bath（巴斯大学）；INAF-IAPS（意大利国家天体物理研究所-行星科学研究所）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；INAF–Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所-阿切特里天文台）；Observatoire Astronomique de Strasbourg（斯特拉斯堡天文台）；University of Hertfordshire（赫特福德大学）；Centro de Astrobiología, CSIC–INTA（西班牙国家航空航天技术研究院-西班牙国家科学研究委员会天体生物学中心）；Max Planck Institute for Radio Astronomy（马克斯·普朗克射电天文研究所）；NRC Herzberg Astronomy & Astrophysics（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究所）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Academia Sinica Institute of Astronomy & Astrophysics（中央研究院天文及天文物理研究所）；European Southern Observatory（欧洲南方天文台）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）
Revisiting the Radial Metallicity Gradient-Age Relation in the Milky Way's Thin and Thick Disks
Shanghai Jiao Tong University（上海交通大学）；University of Chinese Academy of Sciences（中国科学院大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Tianjin Normal University（天津师范大学）
