Stars behind Bars II

A Cosmological Formation Scenario for the Milky Way's Central Stellar Structure

Tobias Buck, Melissa Ness, Aura Obreja, Andrea Maccio, Aaron A. Dutton

    Research output: Contribution to journalArticle

    Abstract

    The stellar populations in the inner kiloparsecs of the Milky Way (MW) show complex kinematical and chemical structures. The origin and evolution of these structures are still under debate. Here we study the central region of a fully cosmological hydrodynamical simulation of a disk galaxy that reproduces key properties of the inner kiloparsecs of the MW: it has a boxy morphology and shows an overall rotation and dispersion profile in agreement with observations. We use a clustering algorithm on stellar kinematics to identify a number of discrete kinematic components: a high- and low-spin disk, a stellar halo, and two bulge components, one fast-rotating and one slow-rotating. We focus on the two bulge components and show that the slow-rotating one is spherically symmetric while the fast-rotating component shows a boxy/peanut morphology. Although the two bulge components are kinematically discrete populations at present day, they are both mostly formed over similar timescales, from disk material. We find that stellar particles with lower initial birth angular momentum (most likely thick-disk stars) end up in the slow-rotating low-spin bulge, while stars with higher birth angular momentum (most likely thin-disk stars) are found in the high-spin bulge. This has the important consequence that a bulge population with a spheroidal morphology does not necessarily indicate a merger origin. In fact, we do find that only ∼2.3% of the stars in the bulge components are ex situ stars brought in by accreted dwarf galaxies early on. We identify these ex situ stars as the oldest and most metal-poor stars on highly radial orbits with large vertical excursions from the disk.

    Original languageEnglish (US)
    Article number67
    JournalAstrophysical Journal
    Volume874
    Issue number1
    DOIs
    StatePublished - Mar 20 2019

    Fingerprint

    stellar structure
    stars
    angular momentum
    kinematics
    merger
    timescale
    metal
    disk galaxies
    dwarf galaxies
    simulation
    halos
    orbits
    profiles
    metals

    Keywords

    • dark matter
    • galaxies: bulges
    • galaxies: formation
    • galaxies: individual (Milky Way)
    • galaxies: kinematics and dynamics
    • methods: numerical

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Cite this

    Stars behind Bars II : A Cosmological Formation Scenario for the Milky Way's Central Stellar Structure. / Buck, Tobias; Ness, Melissa; Obreja, Aura; Maccio, Andrea; Dutton, Aaron A.

    In: Astrophysical Journal, Vol. 874, No. 1, 67, 20.03.2019.

    Research output: Contribution to journalArticle

    Buck, Tobias ; Ness, Melissa ; Obreja, Aura ; Maccio, Andrea ; Dutton, Aaron A. / Stars behind Bars II : A Cosmological Formation Scenario for the Milky Way's Central Stellar Structure. In: Astrophysical Journal. 2019 ; Vol. 874, No. 1.
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    abstract = "The stellar populations in the inner kiloparsecs of the Milky Way (MW) show complex kinematical and chemical structures. The origin and evolution of these structures are still under debate. Here we study the central region of a fully cosmological hydrodynamical simulation of a disk galaxy that reproduces key properties of the inner kiloparsecs of the MW: it has a boxy morphology and shows an overall rotation and dispersion profile in agreement with observations. We use a clustering algorithm on stellar kinematics to identify a number of discrete kinematic components: a high- and low-spin disk, a stellar halo, and two bulge components, one fast-rotating and one slow-rotating. We focus on the two bulge components and show that the slow-rotating one is spherically symmetric while the fast-rotating component shows a boxy/peanut morphology. Although the two bulge components are kinematically discrete populations at present day, they are both mostly formed over similar timescales, from disk material. We find that stellar particles with lower initial birth angular momentum (most likely thick-disk stars) end up in the slow-rotating low-spin bulge, while stars with higher birth angular momentum (most likely thin-disk stars) are found in the high-spin bulge. This has the important consequence that a bulge population with a spheroidal morphology does not necessarily indicate a merger origin. In fact, we do find that only ∼2.3{\%} of the stars in the bulge components are ex situ stars brought in by accreted dwarf galaxies early on. We identify these ex situ stars as the oldest and most metal-poor stars on highly radial orbits with large vertical excursions from the disk.",
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    KW - galaxies: individual (Milky Way)

    KW - galaxies: kinematics and dynamics

    KW - methods: numerical

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