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Modeling the kinematics and star formation history of Andromeda II by a gas-rich major merger of dwarf galaxies

Published online by Cambridge University Press:  21 March 2017

Sylvain Fouquet ,
Ewa L. Łokas  and
Andrés del Pino
Sylvain Fouquet*
Affiliation:
Nicolaus Copernicus Astronomical Centre of the Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
Ewa L. Łokas
Affiliation:
Nicolaus Copernicus Astronomical Centre of the Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
Andrés del Pino
Affiliation:
Nicolaus Copernicus Astronomical Centre of the Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
*
*email: fouquet.sylvain@gmail.com
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Abstract

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We present an evolutionary model for the origin of Andromeda II, a dwarf spheroidal satellite of M31. The model is an extension of the scenario proposed by Łokas et al. (2014) involving a major merger between two gas-rich disky dwarf galaxies.

Keywords

galaxies: dwarfevolutionLocal Groupstructurestellar contentkinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S321: Formation and Evolution of Galaxy Outskirts , March 2016 , pp. 132
Copyright
Copyright © International Astronomical Union 2017 

References

del Pino, A., et al. 2016, in prep.Google Scholar
Fouquet, S., et al. 2016, in prep.Google Scholar
Ho, N., Geha, M., Munoz, R. R., et al. 2012, ApJ, 758, 124 CrossRefGoogle Scholar
Łokas, E. L., Ebrová, I., Pino, A. d., & Semczuk, M. 2014, MNRAS, 445, 6 CrossRefGoogle Scholar