Co-formation of the disc and the stellar halo★
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ID: 302944
2018
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Abstract
Using a large sample of Main Sequence stars with 7-D measurements supplied by Gaia and SDSS, we study the kinematic properties of the local (within ~10 kpc from the Sun) stellar halo. We demonstrate that the halo's velocity ellipsoid evolves strongly with metallicity. At the low [Fe/H] end, the orbital anisotropy (the amount of motion in the radial direction compared to the tangential one) is mildly radial with 0.2-1.7 we measure extreme values of beta~0.9. Across the metallicity range considered, i.e. -3<[Fe/H]<-1, the stellar halo's spin is minimal, at the level of 2010^10 Msun around the epoch of the Galactic disc formation, i.e. between 8 and 11 Gyr ago. The radical halo anisotropy is the result of the dramatic radialisation of the massive progenitor's orbit, amplified by the action of the growing disc.
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| Reference Key |
openalex_W2785892561
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|---|---|
| Authors | Vasily Belokurov, Denis Erkal, N. W. Evans, S. E. Koposov, Alis J. Deason |
| Journal | monthly notices of the royal astronomical society |
| Year | 2018 |
| DOI |
10.1093/mnras/sty982
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| URL | |
| Keywords | Keywords not found |
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