Probing the weak wind phenomenon in Galactic O-type giants

International audience ; Aims. Analyses of Galactic late O dwarfs (O8-O9.5V stars) raised the "weak wind problem": spectroscopic mass loss rates (˙ M) are up to two orders of magnitude lower than the theoretical values. We investigated the stellar and wind properties of Galactic late O giants (O8-O9.5III stars). These stars have luminosities log(L /L) ≈ 5.2, this is the critical value (onset of weak winds) proposed in the literature. Methods. We performed a spectroscopic analysis of nine O8-O9.5III stars in the ultraviolet (UV) and optical regions using the model atmosphere code CMFGEN. Results. Stellar luminosities were adopted using calibrations from the literature. Overall, our model spectral energy distributions agree well with the observed ones considering parallaxes from the latest GAIA data release (DR2). The effective temperature derived from the UV region agrees well with the ones from the optical. As expected, the analysis of the Hertzsprung-Russell (HR) diagram shows that our sample is more evolved than late O dwarfs. From the UV region, we found ˙ M ∼ 10 −8 − 10 −9 M yr-1 in overall. This is lower by ≈ 0.9 − 2.3 dex than the predicted values based on the (global) conservation of energy in the wind. ˙ M predicted from first principles, based on the moving reversing layer theory, agrees better with our findings, but it fails to match the spectroscopic ˙ M for the most luminous OB stars. The region of log(L /L) ≈ 5.2 is critical for both sets of predictions in comparison with the spectroscopic mass-loss rates. CMFGEN models with the predicted ˙ M (the former one) fail to reproduce the UV wind lines for all stars of our sample. We reproduce the observed Hα profiles of four objects with our ˙ M derived from the UV. Hence, low ˙ M values (weak winds) are favored to fit the observations (UV + optical), but discrepancies between the UV and Hα diagnostics remain for some objects. Conclusions. Our results indicate weak winds beyond the O8-9.5V class, being the region of log(L /L) ≈ 5.2 indeed critical to the ...