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Stellar orbital properties as diagnostics of the origin of the stellar halo

Published online by Cambridge University Press:  09 May 2016

Monica Valluri ,
Sarah R. Loebman ,
Jeremy Bailin ,
Adam Clarke ,
Victor P. Debattista  and
Greg Stinson
Monica Valluri
Affiliation:
University of Michigan, USA email: [email protected]
Sarah R. Loebman
Affiliation:
University of Michigan, USA email: [email protected] Michigan Society of Fellows
Jeremy Bailin
Affiliation:
University of Alabama, USA
Adam Clarke
Affiliation:
University of Central Lancashire, UK
Victor P. Debattista
Affiliation:
University of Central Lancashire, UK
Greg Stinson
Affiliation:
Max Planck Institute for Astronomie, Germany
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Abstract

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We examine metallicities, ages and orbital properties of halo stars in a Milky-Way like disk galaxy formed in the cosmological hydrodynamical MaGICC simulations. Halo stars were either accreted from satellites or they formed in situ in the disk or bulge of the galaxy and were then kicked up into the halo (“in situ/kicked-up” stars). Regardless of where they formed both types show surprisingly similar orbital properties: the majority of both types are on short-axis tubes with the same sense of rotation as the disk – implying that a large fraction of satellites are accreted onto the halo with the same sense of angular momentum as the disk.

Keywords

Galaxy: haloGalaxy: kinematics and dynamicsGalaxy: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Issue S317: The General Assembly of Galaxy Halos: Structure, Origin and Evolution , August 2015 , pp. 358 - 359
Copyright
Copyright © International Astronomical Union 2016 

References

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