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Velocity-space substructures and bar resonances in an N-body Milky Way

Published online by Cambridge University Press:  20 January 2023

Tetsuro Asano Open the ORCID record for Tetsuro Asano [Opens in a new window] ,
Michiko S. Fujii Open the ORCID record for Michiko S. Fujii [Opens in a new window] ,
Junich Baba ,
Jeroen Bédorf ,
Elena Sellentin  and
Simon Portegies Zwart
Tetsuro Asano*
Affiliation:
Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
Michiko S. Fujii
Affiliation:
Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
Junich Baba
Affiliation:
National Astronomical Observatory of Japan, Mitaka-shi, Tokyo 181-8588, Japan
Jeroen Bédorf
Affiliation:
Leiden Observatory, Leiden University, NL-2300RA Leiden, The Netherlands Minds.ai, Inc., Santa Cruz, the United States
Elena Sellentin
Affiliation:
Leiden Observatory, Leiden University, NL-2300RA Leiden, The Netherlands Mathematical Institute, Leiden University, NL-2300RA Leiden, The Netherlands
Simon Portegies Zwart
Affiliation:
Leiden Observatory, Leiden University, NL-2300RA Leiden, The Netherlands
*
†email: [email protected]
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Abstract

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The velocity-space distribution of the solar neighborhood stars shows complex substructures (moving groups) including the well-known Hercules stream. Recently, the Gaia observation revealed their detailed structures, but their origins are still in debate. We analyzed a high-resolution N-body simulation of a Milky Way (MW)-like galaxy. To find velocity-space distributions similar to that of the solar neighborhood stars, we used Kullback-Leibler divergence (KLD), which is a metric to measure similarities between probability distributions. The KLD analysis shows the time evolution and the spatial variation of the velocity-space distribution. Velocity-space distributions with small KLDs (i.e. high similarities) are frequently but not always detected around in the simulated MW. In the velocity-map with smallest KLD, the velocity-space substructures are made from bar resonances.

Keywords

Galaxy: diskGalaxy: kinematics and dynamics(Galaxy:) solar neighborhoodGalaxy: structuremethods: numerical
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S362: The Predictive Power of Computational Astrophysics as a Discovery Tool , June 2020 , pp. 116 - 121
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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