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, Genta Sato E-mail: g.sato@astr.tohoku.ac.jp Search for other works by this author on: Oxford Academic Masashi Chiba Astronomical Institute, Tohoku University , Aoba-ku, Sendai, Miyagi 980-8578 , Japan Search for other works by this author on: Oxford Academic
Publications of the Astronomical Society of Japan, Volume 76, Issue 3, June 2024, Pages 498–511, https://doi.org/10.1093/pasj/psae026
Published:
22 April 2024
Article history
Received:
16 January 2024
Accepted:
21 March 2024
Published:
22 April 2024
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Genta Sato, Masashi Chiba, New insights on the dynamics of satellite galaxies: Effects of the figurerotation of a host galaxy, Publications of the Astronomical Society of Japan, Volume 76, Issue 3, June 2024, Pages 498–511, https://doi.org/10.1093/pasj/psae026
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Abstract
We investigate a mechanism to form and keep a planar spatial distribution of satellite galaxies in the Milky Way (MW), which is called the satellite plane. It has been pointed out that the ΛCDM cosmological model hardly explains the existence of such a satellite plane, so it is regarded as one of the serious problems in the current cosmology. We here focus on a rotation of the gravitational potential of a host galaxy, i.e., a so-called figurerotation, following the previous suggestion that this effect can induce the tilt of a so-called tube orbit. Our calculation shows that a figurerotation of a triaxial potential forms a stable orbital plane perpendicular to the rotational axis of the potential. Thus, it is suggested that the MW’s dark halo is rotating with its axis being around the normal line of the satellite plane. Additionally, we find that a small velocity dispersion of satellites is required to keep the flatness of the planar structure, namely the standard derivation of their velocities perpendicular to the satellite plane needs to be smaller than their mean rotational velocity on the plane. Although not all the MW’s satellites satisfy this condition, a fraction of them, called member satellites, which are prominently on the plane, do satisfy it. We suggest that this picture explaining the observed satellite plane can be achieved by the filamentary accretion of dark matter associated with the formation of the MW and a group infall of member satellites along this cosmic filament.
© The Author(s) 2024. Published by Oxford University Press on behalf of the Astronomical Society of Japan.
This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model)
Subject
Galaxy: evolution Galaxy: halo Galaxy: kinematics and dynamics Galaxy: structure (galaxies:) Local Group
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