Lessons from the Auriga discs: the hunt for the Milky Way's ex-situ disc is not yet over
We characterize the contribution from accreted material to the galactic discs of the Auriga Project, a set of high resolution magnetohydrodynamic cosmological simulations of late-type galaxies performed with the moving-mesh code AREPO. Our goal is to explore whether a significant accreted (or ex-sit...
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| Main Authors: | , , , , |
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| Format: | Article (Journal) Chapter/Article |
| Language: | English |
| Published: |
26 Apr 2017
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| In: |
Arxiv
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| Online Access: | Verlag, kostenfrei, Volltext: http://arxiv.org/abs/1704.08261
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| Author Notes: | Facundo A. Gómez, Robert J.J. Grand, Antonela Monachesi, Simon D.M. White, Sebastian Bustamante, Federico Marinacci, Rüdiger Pakmor, Christine M. Simpson, Volker Springel, and Carlos S. Frenk |
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| 245 | 1 | 0 | |a Lessons from the Auriga discs |b the hunt for the Milky Way's ex-situ disc is not yet over |c Facundo A. Gómez, Robert J.J. Grand, Antonela Monachesi, Simon D.M. White, Sebastian Bustamante, Federico Marinacci, Rüdiger Pakmor, Christine M. Simpson, Volker Springel, and Carlos S. Frenk |
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| 520 | |a We characterize the contribution from accreted material to the galactic discs of the Auriga Project, a set of high resolution magnetohydrodynamic cosmological simulations of late-type galaxies performed with the moving-mesh code AREPO. Our goal is to explore whether a significant accreted (or ex-situ) stellar component in the Milky Way disc could be hidden within the near-circular orbit population, which is strongly dominated by stars born in-situ. One third of our models shows a significant ex-situ disc but this fraction would be larger if constraints on orbital circularity were relaxed. Most of the ex-situ material ($\gtrsim 50\%$) comes from single massive satellites ($> 6 \times 10^{10}~M_{\odot}$). These satellites are accreted with a wide range of infall times and inclination angles (up to $85^{\circ}$). Ex-situ discs are thicker, older and more metal-poor than their in-situ counterparts. They show a flat median age profile, which differs from the negative gradient observed in the in-situ component. As a result, the likelihood of identifying an ex-situ disc in samples of old stars on near-circular orbits increases towards the outskirts of the disc. We show three examples that, in addition to ex-situ discs, have a strongly rotating dark matter component. Interestingly, two of these ex-situ stellar discs show an orbital circularity distribution that is consistent with that of the in-situ disc. Thus, they would not be detected in typical kinematic studies. | ||
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