tokens: be expected at a distance of 5000 au or more. Sana et al. (2014) show that at a separation of 8, the cumulative multiplicity frequency reaches 91%. It would correspond to a distance of 16 000 au at a typical distance of 2 kpc. For deprojected distances above 10 000 au the neighbour star is probably not bound to the main star ( Sana et al. 2014 , actually indicate that at large separation only the brightest companions are bound to the main star). The maximum projected separation in arcsec corresponding to the linear separation of 10 000 au in the image is also provided (see Table 5 ). The results are indicated in Table 5 , Cols. 3 to 5. Stars P4; HD 168625b; HD 168607b; MWC314b,c; MWC930c; WR102e; HD 152234b; and HD 164794b,c,d are separated from the main component by less than 10 000 au. This test eliminates 50% of the potential companions visible in the images as bound in a binary system. According to the study by Sana et al. (2014) among massive stars, it is not rare to find binaries with a magnitude difference in K or Lp of 88.5. The limiting magnitude would ensure that almost all potential companions are caught. In addition, they also used NACO to find binaries in O stars, as this threshold would be adequate for LBV stars and corresponds to a late B-type star (using the models from Schaller et al. 1992 ). The results are provided in Table 5 , Col. 6, while we give the angular projected separation corresponding to 10 000 au as an indication in Col. 5. This test allows us to discard 30% of the potential companions visible in the images as bound in a binary system. The results are discussed in Sect. 3.4 . 3.4. Binarity assessment and discussion To summarize, a companion is bound to the main star if it complies with the following criteria: The deprojected/probable separation must be smaller than10 000 au. This value is given inTable 5 , Col. 4. The projectedseparation (from Col. 2) is corrected with the mostprobable angle of projection to provide a more realistic angularseparation (Col. 3) converted to au inCol. 4. The difference in magnitudes must be mag 8.5 (Table 5 , Col. 6). The chance projection probability (field) must be smaller than 10%, (field) smaller than the cut-off probability, or (field) smaller than 5%. In Col. 7 we indicate the chance projection probability for the potential companion considering the stars counted in the NACO images (except for WR102ka for which SINFONI image is used). In Col. 8, we provide the chance projection probability for the potential companion considering the stars counted in the results of simulations with the trilegal code ( Girardi et al. 2005 ). They differ by the magnitude ranges used: all trilegal stars, stars with a maximum difference of 2 and 1. In Col. 9, the chance projection probability following the formula of Correia et al. (2006) is provided and the scaled cut-off probability is given in Col. 10. In Col. 11, the chance projection probabilities (field), (field), and (field) respectively
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