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The LMC vs. the Milky Way

Published online by Cambridge University Press:  14 May 2020

Gurtina Besla Open the ORCID record for Gurtina Besla [Opens in a new window]  and
Nicolás Garavito-Camargo
Gurtina Besla
Affiliation:
Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ85721, USA email: gbesla@email.arizona.edu
Nicolás Garavito-Camargo
Affiliation:
Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ85721, USA email: gbesla@email.arizona.edu
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Abstract

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Recent advancements in astrometry and in cosmological models of dark matter halo growth have significantly changed our understanding of the dynamics of the Local Group. The most dramatic changes owe to a new picture of the structure and dynamics of the Milky Way’s most massive satellite galaxy, the Large Magellanic Cloud (LMC), which is most likely on its first passage about the Milky Way and ten times larger in mass than previously assumed. The LMC’s orbit through the Milky Way’s dark matter and stellar halo will leave characteristic signatures in both density and kinematics. Furthermore, the gravitational perturbations produced by both direct tidal forcing from the LMC and the response of the halo to its passage will together cause significant perturbations to the orbits of tracers of the Milky Way’s dark matter distribution. We advocate for the use of basis field expansion methods to fully capture and quantify these effects.

Keywords

(galaxies:) Magellanic CloudsGalaxy: haloGalaxy: kinematics and dynamicsmethods: numerical(cosmology:) dark matter
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. 123 - 127
Copyright
© International Astronomical Union 2020

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