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In Disguise or Out of Reach: First Clues about In Situ and Accreted Stars in the Stellar Halo of the Milky Way from Gaia DR2
Open accessAbstract
We investigate the nature of the double color–magnitude sequence observed in the Gaia DR2 HR diagram of stars with high transverse velocities. The stars in the reddest-color sequence are likely dominated by the dynamically hot tail of the thick disk population. Information from Nissen & Schuster and from the APOGEE survey suggests that stars in the blue-color sequence have elemental abundance patterns that can be explained by this population having a relatively low star formation efficiency during its formation. In dynamical and orbital spaces, such as the “Toomre diagram,” the two sequences show a significant overlap, but with a tendency for stars on the blue-color sequence to dominate regions with no or retrograde rotation and high total orbital energy. In the plane defined by the maximal vertical excursion of the orbits versus their apocenters, stars of both sequences redistribute into discrete wedges. We conclude that stars that are typically assigned to the halo in the solar vicinity are actually both accreted stars lying along the blue sequence in the HR diagram, and the low rotational velocity tail of the old Galactic disk, possibly dynamically heated by past accretion events. Our results imply that a halo population formed in situ and responsible for the early chemical enrichment prior to the formation of the thick disk has yet to be robustly identified, and that what has been defined as the stars of the in situ stellar halo of the Galaxy may in fact be fossil records of its last significant merger.
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“The other very important contributor in the vicinity of the Sun to stars on halo-like orbits is the (tail of the) Milky Way thick disk (Gaia Collab. et al. 2018a, Haywood et al. 2018, Koppelman et al. 2018), as can be seen Figure 2a.”
From Streams, Substructures, and the Early History of the Milky Way (2020) · cites this paper as Haywood et al. 2018
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“However, the second sequence is populated by stars that, kinematically, are clearly part of the tail of the thick disk seen in Figure 5b (Di Matteo et al. 2019, Haywood et al. 2018).”
From Streams, Substructures, and the Early History of the Milky Way (2020) · cites this paper as Haywood et al. 2018
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Metadata
- Authors
- Haywood, M., Di Matteo, P., Lehnert, M. D., Snaith, O., Khoperskov, S., & Gómez, A.
- Affiliations
- Centre National de la Recherche Scientifique (FR)
- Korea Institute for Advanced Study (KR)
- Corresponding author
- Haywood, M.
- Gómez, A.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2018-08-16
- Volume
- 863
- Issue
- 2
- Pages
- 113
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2802061397
- Cited by
- 360
- References
- 32
- Citations by year
- 2026: 26 · 2025: 54 · 2024: 49 · 2023: 46 · 2022: 42 · 2021: 55 · 2020: 46 · 2019: 33 · 2018: 9
- FWCI
- 19.29
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Licence
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- HAL (submittedVersion, cc-by)
- HAL (submittedVersion)
- arXiv (Cornell University)
- Funders
- Agence Nationale de la Recherche (ANR-15-CE31-0007)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Keywords
- Milky Way stellar halo, thick disk, retrograde rotation, orbital energies, chemical enrichment, Gaia DR2, APOGEE
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