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R. Maiolino, INAF – Astronomical Observatory of Rome, Italy,
S. Arribas, CSIC – Departamento de Astrofísica Molecular e Infrarroja, Madrid, Spain,
T. Böker, European Space Agency – ESTEC, Noordwijk, the Netherlands,
A. Bunker, School of Physics, University of Exeter, Exeter, UK,
S. Charlot, Institute d'Astrophysique de Paris, Paris, France,
G. de Marchi, European Space Agency – ESTEC, Noordwijk, the Netherlands,
P. Ferruit, CRAL – Observatoire de Lyon, 9 Avenue Charles André, Saint-Genis Laval, France,
M. Franx, Leiden Observatory, Leiden, the Netherlands,
P. Jakobsen, European Space Agency – ESTEC, Noordwijk, the Netherlands,
H. Moseley, NASA – Goddard Space Flight Center, MD, USA,
T. Nagao, National Astronomical Observatory of Japan, Osawa, Japan,
L. Origlia, INAF – Astronomical Observatory of Bologna, Bologna, Italy,
B. Rauscher, Leiden Observatory, Leiden, the Netherlands,
M. Regan, Space Telescope Science Institute, Baltimore, MD, USA,
H. W. Rix, Max-Planck-Institut für Astronomie, Heidelberg, Germany,
C. J. Willott, Herzberg Institute of Astrophysics, Victoria, Canada
The James Webb Space Telescope is a 6.6-m-aperture, passively cooled space observatory optimized for near-IR observations. It will be one of the most important observing facilities in the next decade, and it is designed to address numerous outstanding issues in astronomy. In this article we focus specifically on its capabilities to investigate the chemical abundances of various classes of astronomical objects and their metallicity evolution through the cosmic epochs.
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