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GaiaReveals a Metal-rich, in situ Component of the Local Stellar Halo

  • Author(s): Bonaca, Ana
  • Conroy, Charlie
  • Wetzel, Andrew
  • Hopkins, Philip F
  • Kereš, Dušan
  • et al.

Published Web Location

https://arxiv.org/abs/1704.05463
No data is associated with this publication.
Abstract

© 2017. The American Astronomical Society. All rights reserved. We use the first Gaia data release, combined with the RAVE and APOGEE spectroscopic surveys, to investigate the origin of halo stars ≲3 kpc within kpc from the Sun. We identify halo stars kinematically as moving at a relative speed of at least 220 km s-1 with respect to the local standard of rest. These stars are generally less metal-rich than the disk, but surprisingly, half of our halo sample is comprised of stars with [Fe H] >-1. The orbital directions of these metal-rich halo stars are preferentially aligned with the disk rotation, in sharp contrast with the intrinsically isotropic orbital distribution of the metal-poor halo stars. We find similar properties in the Latte cosmological zoom-in simulation of a Milky Way-like galaxy from the FIRE project. In Latte, metal-rich halo stars formed primarily inside of the solar circle, whereas lower-metallicity halo stars preferentially formed at larger distances (extending beyond the virial radius). This suggests that metal-rich halo stars in the solar neighborhood actually formed in situ within the Galactic disk, rather than having been accreted from satellite systems. These stars, currently on halo-like orbits, therefore have likely undergone substantial radial migration/heating.

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