期刊
ASTROPHYSICAL JOURNAL
卷 926, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-4357/ac4d2a
关键词
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资金
- Alexander von Humboldt Foundation at Max-Planck-Institut fur Astronomie, Heidelberg
- IAU's Gruber Foundation Fellowship Programme
- Agence Nationale de la Recherche (ANR project) [ANR-18-CE31-0006, ANR-18-CE31-0017, ANR-19-CE31-0017]
- CNRS/INSU through the Programme National Galaxies et Cosmologie
- European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program [834148]
- INAF, through the Mainstream grant [1.05.01.86.22]
- Agencia Estatal de Investigacion (AEI) of the Ministerio de Ciencia e Innovacion (MCINN) [FJC2018-037323-I]
- AEI/FEDER, UE [AYA2017-89076-P]
- Ministerio de Ciencia, Innovacion y Universidades (MCIU)
- Consejeria de Economia, Industria, Comercio y Conocimiento of the Canary Islands Autonomous Community
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy Office of Science
- National Development and Reform Commission
We uncover the merging process of the Milky Way halo by detecting groupings of globular clusters, stellar streams, and satellite galaxies in action space. We find a total of 6 mergers, including a new one, and discover that the most-metal-poor streams are associated with one of the mergers.
The Milky Way halo was predominantly formed by the merging of numerous progenitor galaxies. However, our knowledge of this process is still incomplete, especially in regard to the total number of mergers, their global dynamical properties and their contribution to the stellar population of the Galactic halo. Here, we uncover the Milky Way mergers by detecting groupings of globular clusters, stellar streams, and satellite galaxies in action ( J ) space. While actions fully characterize the orbits, we additionally use the redundant information on their energy (E) to enhance the contrast between the groupings. For this endeavor, we use Gaia EDR3-based measurements of 170 globular clusters, 41 streams, and 46 satellites to derive their J and E. To detect groups, we use the ENLINK software, coupled with a statistical procedure that accounts for the observed phase-space uncertainties of these objects. We detect a total of N = 6 groups, including the previously known mergers Sagittarius, Cetus, Gaia-Sausage/Enceladus, LMS-1/Wukong, Arjuna/Sequoia/I'itoi, and one new merger that we call Pontus. All of these mergers, together, comprise 62 objects (approximate to 25% of our sample). We discuss their members, orbital properties, and metallicity distributions. We find that the three most-metal-poor streams of our galaxy-C-19 ([Fe/H] = -3.4 dex), Sylgr ([Fe/H] = -2.9 dex), and Phoenix ([Fe/H] = -2.7 dex)-are associated with LMS-1/Wukong, showing it to be the most-metal-poor merger. The global dynamical atlas of Milky Way mergers that we present here provides a present-day reference for galaxy formation models.
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