Very massive stars at low metallicity: evolution, synthetic spectroscopy, and impact on the integrated light of starbursts

Abstract

We study the spectroscopic appearance of very massive stars and their effect on the integrated light of starbursts at low metallicity (Z). We adopt two frameworks for the mass loss rates of VMS: in one case we assume no Z dependence, in the other case we assume a linear scaling with Z. We compute evolutionary models for masses 150, 200, 250 and 300 Msun at Z=0.2, 0.1 and 0.01 Zsun. We compute the associated synthetic spectra at selected points along the evolutionary tracks. Finally we build population synthesis models including VMS. We find that the evolution of VMS critically depends on the assumptions regarding mass loss rates. In case of no Z dependence VMS remain hot for all their lifetime. Conversely when mass loss rates are reduced because of lower Z VMS follow a classical evolution towards the red part of the HR diagram. VMS display HeII 1640 emission in most phases of their evolution, except when they become too cool. This line is present in the integrated light of population synthesis models down to 0.1 Zsun whatever the star formation history, and is also sometimes seen at Z=0.01 Zsun. HeII 1640 is weaker in models that include a Z scaling of the mass loss rates. The optical spectra of starbursts, especially the Wolf-Rayet bumps, sometimes display VMS signatures when these stars are present. At low Z, adding VMS to population synthesis models produces more ionising photons down to 45 eV. At higher energy the ionising flux depends on age, Z, assumption regarding VMS mass loss rates, and on the very short phases at the end of VMS evolution. HeII ionising fluxes large enough to produce some amount of nebular HeII 4686 emission can be produced under specific circumstances. Our models are able to reproduce qualitatively and sometimes also quantitatively the UV spectra of star-forming regions. However we are not able to clearly identify which mass loss framework is favoured.

Accepted in Astronomy & Astrophysics. Authors' version

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