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Low-metallicity (sub-SMC) massive stars

Published online by Cambridge University Press:  28 July 2017

Miriam Garcia
Affiliation:
Centro de Astrobiología (INTA-CSIC), Departamento de Astrofísica. Ctra. Torrejón a Ajalvir km.4, E-28850 Torrejón de Ardoz (Madrid), Spain email: mgg@cab.inta-csic.es
Artemio Herrero
Affiliation:
Instituto de Astrofísica de Canarias, 38205 La Laguna (Tenerife), Spain Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna (Tenerife), Spain
Francisco Najarro
Affiliation:
Centro de Astrobiología (INTA-CSIC), Departamento de Astrofísica. Ctra. Torrejón a Ajalvir km.4, E-28850 Torrejón de Ardoz (Madrid), Spain email: mgg@cab.inta-csic.es
Inés Camacho
Affiliation:
Instituto de Astrofísica de Canarias, 38205 La Laguna (Tenerife), Spain Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna (Tenerife), Spain
Daniel J. Lennon
Affiliation:
European Space Astronomy Centre (ESA/ESAC), Villanueva de la Cañada (Madrid), Spain
Miguel A. Urbaneja
Affiliation:
Institut fuer Astro- und Teilchenphysik, Universitaet Innsbruck, Innsbruck, Austria
Norberto Castro
Affiliation:
Astronomy Department, University of Michigan, Ann Arbor, MI 48109, USA
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Abstract

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The double distance and metallicity frontier marked by the SMC has been finally broken with the aid of powerful multi-object spectrographs installed at 8-10m class telescopes. VLT, GTC and Keck have enabled studies of massive stars in dwarf irregular galaxies of the Local Group with poorer metal-content than the SMC. The community is working to test the predictions of evolutionary models in the low-metallicity regime, set the new standard for the metal-poor high-redshift Universe, and test the extrapolation of the physics of massive stars to environments of decreasing metallicity. In this paper, we review current knowledge on this topic.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2017 

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