Hostname: page-component-7479d7b7d-c9gpj Total loading time: 0 Render date: 2024-07-15T22:41:43.289Z Has data issue: false hasContentIssue false
  • English
  • Français

VMC proper motions of the Magellanic Bridge

Published online by Cambridge University Press:  30 October 2019

Thomas Schmidt ,
Maria-Rosa Cioni ,
Florian Niederhofer ,
Jonathan Diaz  and
Gal Matijevic
Thomas Schmidt
Affiliation:
Leibniz-Institut für Astrophysik Potsdam An der Sternwarte 16, D-14482 Potsdam, Germany email: [email protected]
Maria-Rosa Cioni
Affiliation:
Leibniz-Institut für Astrophysik Potsdam An der Sternwarte 16, D-14482 Potsdam, Germany email: [email protected]
Florian Niederhofer
Affiliation:
Leibniz-Institut für Astrophysik Potsdam An der Sternwarte 16, D-14482 Potsdam, Germany email: [email protected]
Jonathan Diaz
Affiliation:
International Centre for Radio Astronomy Research, The University of Western Australia, M468, 35 Stirling Hwy, Crawley WA 6009, Australia
Gal Matijevic
Affiliation:
Leibniz-Institut für Astrophysik Potsdam An der Sternwarte 16, D-14482 Potsdam, Germany email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Dwarf galaxies enable us to study early phases of galaxy evolution and are key to many open questions about the hierarchical structure of the Universe. The Large and Small Magellanic Cloud (LMC and SMC) are the most luminous dwarf galaxy satellites of the Milky Way (MW). They are most likely gravitationally bound to each other, and their last interaction occurred about 200 Myr ago. Also, they are in an early phase of minor merging with the MW and will impact the Galactic structure in the future because of their relatively large mass. However, there are still major uncertainties regarding their origin and their interactions with one another and with the Milky Way. We cross-correlated the VMC and Gaia DR2 data to select a sample of stars that likely belong to the Magellanic Bridge, a feature formed of gas and stars which is connecting the LMC and the SMC. We removed potential MW foregound stars using a combination of parallax and colour-magnitude criteria and calculated the proper motions of the Bridge member stars. Our analysis supports a motion of star towards the LMC, which was found to be in good agreement with a dynamical simulation, of the SMC being stripped by the LMC.

Keywords

Magellanic cloudsstars: kinematicssurveys
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. 130 - 133
Copyright
© International Astronomical Union 2019 

References

Bagheri, G., et al. 2013, A&A, 551, A78 Google Scholar
Bekki, K., et al. 2013, ApJ, 779, 9 CrossRefGoogle Scholar
Carrera, R., et al. 2017, MNRAS, 471, 4571 CrossRefGoogle Scholar
Cioni, M-R. L., et al. 2011, A&A, 527, A116 Google Scholar
Diaz, J., & Bekki, K. 2012, ApJ, 750, 36 CrossRefGoogle Scholar
Dufton, P. L., et al. 2008, MNRAS 385, 2261 CrossRefGoogle Scholar
Guglielmo, M., Lewis, G. F. & Bland-Hawthorn, J. 2014, MNRAS 444, 1759 CrossRefGoogle Scholar
Hindman, J. V., 1963, ApJ, 16, 570 Google Scholar
Irwin, M. et al., 1985, Nature, 318, 160 CrossRefGoogle Scholar
Luri, X., et al. 2018, A&A 616, A9 Google Scholar
Nöel, N., et al. 2013, ApJ, 768, 109 CrossRefGoogle Scholar
Vasiliev, E. 2018, MNRAS 481, L100 CrossRefGoogle Scholar
Zivick, et al. 2018, ApJ, 864, 55 CrossRefGoogle Scholar