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Proper motion of the Magellanic Bridge: Removal of foreground stars

Published online by Cambridge University Press:  14 May 2020

Thomas Schmidt Open the ORCID record for Thomas Schmidt [Opens in a new window] ,
Maria-Rosa L. Cioni ,
Florian Niederhofer ,
Jonathan Diaz ,
Anna B. A. Queiroz ,
Gal Matijevic  and
Cristina Chiappini
Thomas Schmidt
Affiliation:
Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: tschmidt@aip.de
Maria-Rosa L. Cioni
Affiliation:
Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: tschmidt@aip.de
Florian Niederhofer
Affiliation:
Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: tschmidt@aip.de
Jonathan Diaz
Affiliation:
International Centre for Radio Astronomy Research, The University of Western Australia, M468, 35 Stirling Hwy, CrawleyWA6009, Australia
Anna B. A. Queiroz
Affiliation:
Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: tschmidt@aip.de
Gal Matijevic
Affiliation:
Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: tschmidt@aip.de
Cristina Chiappini
Affiliation:
Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: tschmidt@aip.de
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Abstract

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The Large and Small Magellanic Cloud (LMC and SMC) are the most luminous dwarf galaxy satellites of the Milky Way. Thanks to their close proximity (50-60 kpc), they provide one of the best opportunities to study in detail the kinematics of resolved stellar populations in an interacting pair of galaxies. Large photometric surveys like the ongoing Gaia mission and the near-infrared VISTA survey of the Magellanic Cloud system (VMC) will have a significant impact on our insight into the Magellanic system. We have combined the individual strengths of VMC and Gaia DR2 data to improve our understanding of the internal kinematics of the galaxies. In this study, we present results from our ongoing project dedicated to measure and analyse the proper motions of large samples of stars across the Magellanic Clouds, efficiently removing Milk Way foreground stars utilising distances derived with the StarHorse code.

Keywords

Magellanic Cloudsstars: kinematicssurveys
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. 128 - 129
Copyright
© International Astronomical Union 2020

References

Belsa, G.et al. 2007, ApJ, 668, 2Google Scholar
Cioni, M.-R. L.et al. 2011, A&A, 527, A116Google Scholar
Collaboration, Gaia, et al. 2018, A&A 616, A1Google Scholar
Schmidt, T.et al. 2018, ArXiv e-prints, https://arxiv.org/abs/1810.02701Google Scholar
Queiroz, A. B. A.et al. 2018, MNRAS, 476, 210.1093/mnras/sty330CrossRefGoogle Scholar
Anders, F.et al. 2019, A&A, 628, A94Google Scholar