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Stellar chemo-kinematics of isolated dwarf spheroidal galaxies

Published online by Cambridge University Press:  30 October 2019

S. Taibi
Affiliation:
Instituto de Astrofisica de Canarias, C/ Vía Láctea s/n, E-38205, La Laguna, Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, E-38205, La Laguna, Tenerife, Spain
G. Battaglia
Affiliation:
Instituto de Astrofisica de Canarias, C/ Vía Láctea s/n, E-38205, La Laguna, Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, E-38205, La Laguna, Tenerife, Spain
M. Rejkuba
Affiliation:
European Southern Observatory, Karl-Schwarzschild Strasse 2, D-85748 Garching, Germany
N. Kacharov
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
M. Zoccali
Affiliation:
Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile
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Abstract

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The study of dwarf spheroidal galaxies (dSph) is of great importance to understand galaxy evolution at the low-mass end. In the Local Group the majority of them are found to be satellites of the Milky Way or M31. The closest ones have been studied in great detail, however it is hard to constrain if their present-day observed properties are mainly caused by internal or environmental mechanisms. In order to minimize these effects and gain an insight into their intrinsic properties, we are studying two of the three isolated dSph galaxies in the Local Group, i.e. Cetus and Tucana, located far beyond the virial radius of the Milky Way and M31. We present here results from our recently published analysis of Cetus (Taibi2018) and preliminary results for Tucana (Taibi et al. in prep.).

Type
Contributed Papers
Copyright
© International Astronomical Union 2019 

References

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