Astronomy and Astrophysics – Astrophysics – Galaxy Astrophysics
Scientist
Astronomy and Astrophysics
Astrophysics
Galaxy Astrophysics
Scientist
Instituto de Astrofisica de Canarias
IAC
IoA, Univ.Tokyo
Durham, Tokyo
Instituto de Astrofisica de Canarias, Tenerife, Spain
Institute of Astronomy, University of Tokyo, Osawa, 2-21-1, Mitaka, Tokyo, Japan
Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK
Department of Physics, University of Durham, Durham DH1 3LE, England, UK; Instituto de Astrofisica de Canarias, E-38200 La Laguna, Tenerife, Spain de Astrofísica de Canarias, La Laguna 38200, Tenerife, Spain
Instituto de Astrofísica de Canarias, C / Vía Láctea s / n, 38200 La Laguna, Tenerife, Spain
Instituto de Astrofísica de Canarias, C / Vía Láctea, S / N, E-38205, La Laguna, Tenerife, Spain
Instituto de Astrofísica de Canarias
Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain
IAC, Tenerife
Instituto de Astrofisica de Canarias, Spain
IoA, Univ.Tokyo, currently at Univ.Durham, UK
Instituto de Astrofísica de Canarias; Departamento de Astrofísica, Universidad de La Laguna
Instituto de Astrofísica de Canarias, La Laguna, 38200, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, 38205, La Laguna, Tenerife, Spain
Institute of Astronomy, University of Tokyo, Tokyo, Japan Tenerife.
Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain.
Instituto de Astrofísica de Canarias, Vía Láctea s / n, E-38200 La Laguna, Tenerife, Spain de Astrofísica de Canarias, La Laguna, E-38200 Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain
Instituto de Astrofísica de Canarias. c / Vía Láctea S / N, E38205, La Laguna, Tenerife, Spain
Inst. de Astrofísica de Canarias
47 Tuc: The Spectroscopic Versus CMD Age Discrepancy
47 Tucanae: The Spectroscopic versus Color-Magnitude Diagram Age Discrepancy
A correlation between light profile and [Mg/Fe] abundance ratio in early-type galaxies
A Database for Galaxy Evolution Modeling
A new approach to derive [α/Fe] for integrated stellar populations
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