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Dwarf galaxies: evidence of differential tidal effects in the Large Magellanic Cloud

Published online by Cambridge University Press:  30 October 2019

Andrés E. Piatti Open the ORCID record for Andrés E. Piatti [Opens in a new window]  and
Dougal Mackey
Andrés E. Piatti
Affiliation:
Consejo Nacional de Investigaciones Cientficas y Técnicas, Av. Rivadavia 1917, C1033AAJ, Buenos Aires, Argentina Observatorio Astronómico de Córdoba, Laprida 854, 5000, Córdoba, Argentina email: [email protected]
Dougal Mackey
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australiaemail: [email protected]
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Abstract

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We built the most extended stellar density and/or surface brightness radial profiles for 13 old Large Magellanic Cloud (LMC) globular clusters (GCs). The studied GCs located farther than ~ 5 kpc from the LMC center would not seem to present any hint of extended stellar structures, while those closer than ~ 5 kpc do show extended structures. Such an excess of stars tightly depends on the position of the GCs, so that the closer the GC to the LMC center, the larger the excess of stars. Furthermore, the GC radii also show a remarkable trend with the position of the GC in the LMC disc. These outcomes can be fully interpreted in the light of the known GC radial velocity disc-like kinematics, from which GCs have been somehow mostly experiencing the influence of the LMC gravitational field at their respective mean distances from the LMC center.

Keywords

techniques: photometricgalaxies: star clusters(galaxies:) Magellanic Clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S344: Dwarf Galaxies: From the Deep Universe to the Present , August 2018 , pp. 114 - 117
Copyright
© International Astronomical Union 2019 

Footnotes

†

This is an abridged version of the article published in extense in MNRAS (2018), 478, 2164.

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