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THE DUAL ORIGIN OF STELLAR HALOS
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We investigate the formation of the stellar halos of four simulated disk galaxies using high-resolution, cosmological SPH + N -body simulations. These simulations include a self-consistent treatment of all the major physical processes involved in galaxy formation. The simulated galaxies presented here each have a total mass of ∼10 12 M ☉ , but span a range of merger histories. These simulations allow us to study the competing importance of in situ star formation (stars formed in the primary galaxy) and accretion of stars from subhalos in the building of stellar halos in a ΛCDM universe. All four simulated galaxies are surrounded by a stellar halo, whose inner regions ( r < 20 kpc) contain both accreted stars, and an in situ stellar population. The outer regions of the galaxies' halos were assembled through pure accretion and disruption of satellites. Most of the in situ halo stars formed at high redshift out of smoothly accreted cold gas in the inner 1 kpc of the galaxies' potential wells, possibly as part of their primordial disks. These stars were displaced from their central locations into the halos through a succession of major mergers. We find that the two galaxies with recently quiescent merger histories have a higher fraction of in situ stars (∼20%–50%) in their inner halos than the two galaxies with many recent mergers (∼5%–10% in situ fraction). Observational studies concentrating on stellar populations in the inner halo of the Milky Way will be the most affected by the presence of in situ stars with halo kinematics, as we find that their existence in the inner few tens of kpc is a generic feature of galaxy formation.
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“We now know from the Gaia DR2 data that what Norris (1994) called the contracted halo is actually largely heated (proto-)thick disk.So it was indeed formed mostly in situ; however, the stars did not form during a collapse but in a disk that was heavily dynamically perturbed during a merger, as in the simulations of Zolotov et al. (2009) and Tissera et al. (2013).”
From Streams, Substructures, and the Early History of the Milky Way (2020) · cites this paper as Zolotov et al. 2009
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“Depending on the mass ratio, such an event could lead to the formation of a bulge (Barnes 1992), or merely to the thickening of the disk (Quinn et al. 1993), and possibly also to the formation of a halo of stars from the original disk and the destroyed satellite (Zolotov et al. 2009, Purcell et al. 2010), as seems to have happened for the Milky Way (see Section 4.2 for details).”
From Streams, Substructures, and the Early History of the Milky Way (2020) · cites this paper as Zolotov et al. 2009
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Angular momentum evolution in dark-matter haloes
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Self-citationExistence of the Metal-rich Stellar Halo and High-velocity Thick Disk in the Galaxy
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Exploration of Halo Substructures in Integrals-of-motion Space with Gaia Data Release 3
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Where Did the Outskirts Go? Outer Stellar Halos as a Sensitive Probe of Supernova Feedback
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Low-metallicity stellar halo populations as tracers of dark matter haloes
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Chemical Abundances as Population Tracers
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THE EXTENDED STELLAR COMPONENT OF GALAXIES THE NATURE OF DARK MATTER
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Origins and Interpretation of Tidal Debris
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Kinematics in galactic tidal tails - A source for Hypervelocity stars?Preprint
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TREX: Kinematic Characterization of a High-dispersion Intermediate-age Stellar Component in M33
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Action-based dynamical models of M31-like galaxies
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HALO7D. III. Chemical Abundances of Milky Way Halo Stars from Medium-resolution Spectra
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AuriDESI: mock catalogues for the DESI Milky Way Survey
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On the Use of Field RR Lyrae as Galactic Probes. VIII. Early Formation of the Galactic Spheroid*
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Alpha Element Populations Among Local Halo Stars
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The chemical diversity of the metal-poor Milky Way
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Building blocks of the Milky Way's accreted spheroid
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Metadata
- Authors
- Zolotov, A., Willman, B., Brooks, A. M., Governato, F., Brook, C. B., Hogg, D. W., Quinn, T., & Stinson, G.
- Affiliations
- Haverford College (US)
- California Institute of Technology (US)
- University of Washington (US)
- University of Lancashire (GB)
- New York University (US)
- McMaster University (CA)
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2009-08-18
- Volume
- 702
- Issue
- 2
- Pages
- 1058-1067
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2085130064
- Cited by
- 342
- References
- 54
- Citations by year
- 2026: 5 · 2025: 14 · 2024: 20 · 2023: 15 · 2022: 15 · 2021: 8 · 2020: 30 · 2019: 32 · 2018: 18 · 2017: 18 · 2016: 29 · 2015: 18 · 2014: 17 · 2013: 19 · 2012: 27
- FWCI
- 13.95
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (acceptedVersion)
- Rutgers University Community Repository (Rutgers University) (submittedVersion)
- CaltechAUTHORS (California Institute of Technology) (submittedVersion)
- arXiv (Cornell University)
- PhDT
- Funders
- National Science Foundation (0205413, 0607819)
- Smithsonian Institution
- National Aeronautics and Space Administration (NNX08AJ48G, ATP NNX08AG84G, NNX08AG84G)
- Haverford College
- York University
- Ames Research Center
- Smithsonian Astrophysical Observatory
- Science and Technology Facilities Council (ST/F002432/1)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Keywords
- stellar halo, in situ star formation, halo accretion, major mergers, disk galaxy evolution, satellite disruption, halo kinematics, Galactic halo
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