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B-supergiants in IC1613: testing low-Z massive star physics and evolution

Published online by Cambridge University Press:  28 July 2017

Inés Camacho ,
Miriam García ,
Miguel A. Urbaneja  and
Artemio Herrero
Inés Camacho
Affiliation:
Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain
Miriam García
Affiliation:
Centro de Astrobiología CAB (CSIC/INTA), Madrid, Spain
Miguel A. Urbaneja
Affiliation:
Institute of Astro and Particle Physics, Universität Innsbruck, Innsbruck, Austria
Artemio Herrero
Affiliation:
Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain
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Abstract

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The physical processes taking place in massive stars during their life and death are highly dependent on the metallicity (Z) of their parent cloud. Observations of these stars in low-Z nearby galaxies are crucial to understand these processes. IC1613 is the nearest Local Group galaxy with ongoing star formation and O-abundance lower than the SMC, although UV spectroscopy suggests it is not so metal poor. We performed a spectral analysis of early B-type stars in the galaxy, obtaining physical parameters and abundances. Our results confirm the low O-abundance of IC1613.

Keywords

IC1613massive starsgalaxyabundancesmetallicity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 389
Copyright
Copyright © International Astronomical Union 2017