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The high transverse velocity stars in Gaia-LAMOST

Published online by Cambridge University Press:  14 May 2020

João A. S. Amarante Open the ORCID record for João A. S. Amarante [Opens in a new window] ,
Martin C. Smith  and
Corrado Boeche
João A. S. Amarante
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory, Chinese Academy of Sciences 80 Nandan Road, Shanghai200030, China emails: [email protected], [email protected]
Martin C. Smith
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory, Chinese Academy of Sciences 80 Nandan Road, Shanghai200030, China emails: [email protected], [email protected]
Corrado Boeche
Affiliation:
INAF-Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, Italy email: [email protected]
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Abstract

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Although the stellar halo accounts for just ∼1% of the total stellar mass of the Milky Way, the kinematics of halo stars can tell us a lot about the origins and evolution of our Galaxy. It has been shown that the high transverse velocity stars in Gaia DR2 reveal a double sequence in the Hertzsprung-Russell (HR) diagram, indicating a duality in the local halo within 1 kpc. We fit these stars by updating the popular Besançon/Galaxia model, incorporating the latest observational results for the stellar halo. We are able to obtain a good match to the Gaia data and provide new constraints on the properties of the disc and halo. In particular, we show that the thick disc contribution to this high velocity tail is small, but not negligible, and likely has an influence on the red sequence of the HR diagram.

Keywords

Galaxy: haloGalaxy: discGalaxy: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S353: Galactic Dynamics in the Era of Large Surveys , June 2019 , pp. 59 - 60
Copyright
© International Astronomical Union 2020

References

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