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Two kinematically different Large Magellanic Cloud old globular cluster populations unveiled from Gaia DR2 data sets

Published online by Cambridge University Press:  11 March 2020

Andrés E. Piatti Open the ORCID record for Andrés E. Piatti [Opens in a new window] ,
Emilio J. Alfaro  and
Tristan Cantat-Gaudin
Andrés E. Piatti
Affiliation:
Consejo Nacional de Investigaciones Cientficas y Técnicas, Godoy Cruz 2290, C1425FQB, Buenos Aires, Argentina Observatorio Astronómico de Córdoba, Laprida 854, 5000, Córdoba, Argentina email: [email protected]
Emilio J. Alfaro
Affiliation:
Instituto de Astrofsica de Andaluca, (CSIC), Glorieta de la Astronoma, S/N, Granada, 18008, Spain email: [email protected]
Tristan Cantat-Gaudin
Affiliation:
Institut de Ciències del Cosmos, Universitat de Barcelona (IEEC-UB), Mart i Franquès 1, E-08028 Barcelona, Spain email: [email protected]
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Abstract

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We derive mean proper motions of 15 known Large Magellanic Cloud (LMC) old globular clusters (GCs) from the Gaia DR2 data sets. When these mean proper motions are gathered with existent radial velocities to compose the GCs’ velocity vectors, we found that the projection of the velocity vectors onto the LMC plane and those perpendicular to it tell us about two distinct kinematical GC populations. Such a distinction becomes clear if the GCs are split at a perpendicular velocity of 10 km/s (absolute value). The two different kinematics groups also exhibit different spatial distributions. Those with smaller vertical velocities are part of the LMC disk, while those with larger values are closely distributed like a spheroidal component. Since GCs in both kinematic-structural components share similar ages and metallicities, we speculate with the possibility that their origins could have occurred through a fast collapse that formed halo and disk concurrently.

Keywords

galaxies: individual: LMCgalaxies: star clusters: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 139 - 142
Copyright
© International Astronomical Union 2020

Footnotes

†

This is an abridged version of the article published in extenso in MNRAS (2019), 484, L19.

References

Grocholski, A. J., Cole, A. A., Sarajedini, A., Geisler, D., & Smith, V. V. 2006, AJ, 132, 163CrossRefGoogle Scholar
Piatti, A. E. & Mackey, A. D. 2018, MNRAS, 478, 2164CrossRefGoogle Scholar
Piatti, A. E., Hwang, N., Cole, A. A., Angelo, M. S., & Emptage, B. 2018, MNRAS, 481, 49CrossRefGoogle Scholar
Schommer, R. A., Suntzeff, N. B., Olszewski, E. W., & Harris, H. C. 1992, AJ, 103, 447CrossRefGoogle Scholar
Sharma, S., Borissova, J., Kurtev, R., Ivanov, V. D., & Geisler, D. 2010, AJ, 139, 878CrossRefGoogle Scholar
van der Marel, R. P. & Kallivayalil, N. 2014, ApJ, 781, 121CrossRefGoogle Scholar
van der Marel, R. P., Alves, D. R., Hardy, E., & Suntzeff, N. B. 2002, AJ, 124, 2639CrossRefGoogle Scholar
Vasiliev, E. 2018, MNRAS, 481, L100CrossRefGoogle Scholar