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tokens: (top) WC/WN versus metallicity. Blue lines correspond to BPASS binary models and red dashed lines the single models. The black star shows the averaged WC/WN estimation for the Antennae. For comparison, we also show the values for the Magellanic Clouds and the Milky Way taken from Rosslowe Crowther ( 2015 ), shown with open stars. (bottom) WR/O versus metallicity. The upside down arrow represents an upper limit for the Antennae, since we only computed the number of O-type stars in the SSCs with WR stars. Finally, the template-fitting method has been used in several works to classify WR stars (e.g. Hadfield Crowther 2006 , 2007 ; Kehrig et al. 2013 ; Gómez-González et al. 2020 ). However, it is still not clear how representative a template spectrum is for a given subtype. That is, what is the dispersion in the strengths of different lines in the individual spectra used for obtaining the template. An in-depth study of line strengths of WR stars in the Galaxy updated with new astrometric and photometric information from Gaia would be required to address this question. 5 SUMMARY AND CONCLUDING REMARKS We have used VLT MUSE data cubes from the ESO archive to search for WR stars in star-forming complexes of the Antennae galaxies. We reported their number, classification, and distribution. Our results can be summarized as follows. We detected 38 WR SSC complexes with 4053 ± 84 WR stars, out of which 2021 ± 60 are WNL, 2032 ± 59 WC-types. We cannot uncover a plausible presence of WO-type stars given the limited spectral range covered by the observations used for this study. Further observations that covering the VB could confirm or rule out this population, the rarest type of WR stars. However, thanks to the GTC spectrum of WR 1, we can rule out the presence of WO-type stars in this SSC complex, the one with the highest number of WR stars in the Antennae. Galactic WR templates of WNL, WCE, and WCL subtypes were appropriate to classify and quantify the WR stars of each SSC complex, given the metallicity of the Antennae, with an oxygen abundance 12 + log(O/H) ≈ 8.9. We analysed the observed WR blue and red bumps using multiple-component Gaussian fitting in order to recover the ionic transitions responsible for the bumps and report their main parameters. In all cases, the recovered ions are consistent with those expected for the inferred subtype using the templates. Avoiding any nebular contamination, we evaluated the contribution for each broad emission line to the entire luminosity of the BB and the RB of the entire WR sample. We do not find any evidence of the nebular He ii emission line. This is explained by theoretical models, as discussed, given the high metallicity of the Antennae. We estimated the main physical properties of the WR nebular environments, oxygen abundances, and presented information regarding their kinematics. We derive a global WC/WN ratio ∼1, which, according to predictions of the current BPASS models is consistent with the