Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 478, Issue 2, Pages 2164-2176Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty1048
Keywords
techniques: photometric; galaxies: individual: LMC; galaxies: star clusters: general
Categories
Funding
- U.S. Department of Energy
- U.S. National Science Foundation
- Ministry of Science and Education of Spain
- Science and Technology Facilities Council of the United Kingdom
- Higher Education Funding Council for England
- National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
- Kavli Institute of Cosmological Physics at the University of Chicago
- Center for Cosmology and Astro-Particle Physics at the Ohio State University
- Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University
- Financiadora de Estudos e Projetos
- Fundacao Carlos Chagas Filho de Amparo 'a Pesquisa do Estado do Rio de Janeiro
- Conselho Nacional de Desenvolvimento Cientifico e Tecnologico
- Ministerio da Ciencia, Tecnologia e Inovacao
- Deutsche Forschungsgemeinschaft
- Collaborating Institutions in the DES
- SMASH, NOAO program [2013B-0440]
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We present for the first time extended stellar density and/or surface brightness radial profiles for almost all the known LargeMagellanic Cloud (LMC) old globular clusters (GCs). These were built from DECam images and reach out to similar to 4 times the GCs' tidal radii. The background subtracted radial profiles reveal that the GCs located closer than similar to 5 kpc from the LMC centre contain an excess of stars in their outermost regions with respect to the stellar density expected from a King profile. Such a residual amount of stars, not seen in GCs located farther than similar to 5 kpc from the LMC centre, as well as the GCs' dimensions, shows a clear dependence with the GCs' positions in the galaxy, in the sense that, the farther the GC from the centre of the LMC, the larger both the excess of stars in its outskirts and size. Although the masses of GCs located inside and outside similar to 5 kpc are commensurate, the outermost regions of GCs located closer than similar to 5 kpc from the LMC centre appear to have dynamically evolved more quickly. 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 centre.
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