Co-formation of the disc and the stellar halo★

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ID: 302944
2018
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Ranked #52 of 900 articles by views in monthly notices of the royal astronomical society

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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.
Reference Key
openalex_W2785892561 Use this key to autocite in the manuscript while using SciMatic Manuscript Manager or Thesis Manager
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
URL
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