tokens: modern stellar atmosphere models were compared to the disentangled spectra of each component of HD 54662 AB in order to estimate their physical parameters. A previous quantitative spectroscopic study of the system components was performed by MMR18 using the cmfgen code (Hillier Miller 1998 ). Regarding the projected rotational velocities, using the Fourier Transform method (Simón-Díaz Herrero 2007 ) MMR18 determined 158 and 43 for the genuine 12 primary (A) and secondary (B) components, respectively. These values perfectly agree with our determinations of v sin i (see Table 6 ). However, we differ with the former authors regarding the macroturbulent velocity: while MMR18 attributed to component B a macroturbulence of 35 in order to match the observed line profiles with the synthetic spectra, we estimated a macroturbulence of 40 for component A and fixed this parameter to zero for component B, since we found no reason to modify its value when checking the broadening of the synthetic line profiles. The values computed in this work for the effective temperatures ( T eff ) and surface gravities (log g ) of the components are consistent, within the uncertainties, with the current calibrations for O stars in the Milky Way, including the classical calibration by Martins et al. ( 2005 ), as well as the most recent ones by Simón-Díaz et al. ( 2014 ) and Holgado et al. ( 2018 ). MMR18 also determined T eff , as well as helium abundances ( Y He ) for both stars. While our estimates of log g and Y He are in good agreement with their values, our T eff determinations result in slightly higher values than theirs (Δ T eff 1500 K). We re-analysed both stars using the line broadening parameters estimated by MMR18 . We obtained good agreement for component A, in contrast to component B. Moreover, the broadening of the fastwind synthetic lines using MMR18 ’s v sin i and v mac values cannot reconcile the broadening of the lines observed in our disentangled spectra. Therefore, line broadening only cannot explain the differences in T eff with MMR18 . In Section 3.1 , we mentioned that the presence of residuals in the Balmer lines originated from the disentangling process may affect the surface gravity determination. As explained in Section 5 , for our analysis we used the least affected lines (H γ and H ε) in order to minimize this effect. Regarding the He lines, some profile distortions which could be playing a role are also observed, in particular in the He i λ 4388 Å line, mostly for the primary component. In any case, Fig. 6 shows that the synthetic composite spectrum resulting from the addition of the individual models for the A and B components reproduces well the observed spectrum of the system. We then conclude that potential differences in the shape of the lines of the individual spectra due to different disentangling processes may be the cause of the disagreement between our determinations and those from MMR18 . Note also that, unlike the results presented
ner_tags: O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O B-Citation O O B-Software O B-Citation I-Citation I-Citation O O O O O O O O O O O B-Citation I-Citation I-Citation O B-Citation O O O O O O O O B-CelestialObject B-CelestialObject O B-CelestialObject B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation B-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O B-Citation O O O O O O B-CelestialObject I-CelestialObject O O O B-CelestialObject I-CelestialObject O O O O O O O O O B-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation O O O O O O O O