English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
Add to Basket
  Local TagsRelease HistoryDetailsSummary

Released
Journal Article

The Gaia-ESO Survey: Churning through the Milky Way

MPS-Authors

Hayden,  M. R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Recio-Blanco,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

de Laverny,  P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Mikolaitis,  S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Guiglion,  G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hill,  V.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Gilmore,  G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Randich,  S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bayo,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bensby,  T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bergemann,  M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bragaglia,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Casey,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Costado,  M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Feltzing,  S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Franciosini,  E.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hourihane,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Jofre,  P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Koposov,  S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kordopatis,  G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lanzafame,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lardo,  C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lewis,  J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lind,  K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Magrini,  L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Monaco,  L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Morbidelli,  L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pancino,  E.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Sacco,  G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Stonkute,  E.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Worley,  C. C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zwitter,  T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2018A&A...609A..79H
(Any fulltext)

Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Hayden, M. R., Recio-Blanco, A., de Laverny, P., Mikolaitis, S., Guiglion, G., Hill, V., et al. (2018). The Gaia-ESO Survey: Churning through the Milky Way. Astronomy and Astrophysics, 609.


Cite as: https://hdl.handle.net/21.11116/0000-0005-CD62-6
Abstract
Context. There have been conflicting results with respect to the extent that radial migration has played in the evolution of the Galaxy. Additionally, observations of the solar neighborhood have shown evidence of a merger in the past history of the Milky Way that drives enhanced radial migration.
Aims: We attempt to determine the relative fraction of stars that have undergone significant radial migration by studying the orbital properties of metal-rich ([Fe/H] > 0.1) stars within 2 kpc of the Sun. We also aim to investigate the kinematic properties, such as velocity dispersion and orbital parameters, of stellar populations near the Sun as a function of [Mg/Fe] and [Fe/H], which could show evidence of a major merger in the past history of the Milky Way.
Methods: We used a sample of more than 3000 stars selected from the fourth internal data release of the Gaia-ESO Survey. We used the stellar parameters from the Gaia-ESO Survey along with proper motions from PPMXL to determine distances, kinematics, and orbital properties for these stars to analyze the chemodynamic properties of stellar populations near the Sun.
Results: Analyzing the kinematics of the most metal-rich stars ([Fe/H] > 0.1), we find that more than half have small eccentricities (e< 0.2) or are on nearly circular orbits. Slightly more than 20% of the metal-rich stars have perigalacticons Rp> 7 kpc. We find that the highest [Mg/Fe], metal-poor populations have lower vertical and radial velocity dispersions compared to lower [Mg/Fe] populations of similar metallicity by 10 km s-1. The median eccentricity increases linearly with [Mg/Fe] across all metallicities, while the perigalacticon decreases with increasing [Mg/Fe] for all metallicities. Finally, the most [Mg/Fe]-rich stars are found to have significant asymmetric drift and rotate more than 40 km s-1 slower than stars with lower [Mg/Fe] ratios.
Conclusions: While our results cannot constrain how far stars have migrated, we propose that migration processes are likely to have played an important role in the evolution of the Milky Way, with metal-rich stars migrating from the inner disk toward to solar neighborhood and past mergers potentially driving enhanced migration of older stellar populations in the disk.