Fig. 7.
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CF of stars in different systems as a function of the primary mass. For reference, values from Duchêne & Kraus (2013), GRAVITY Collaboration (2018), and Sana et al. (2014) are also presented for different mass ranges. The results from Sana et al. (2014) (SMaSH+ Survey) presented here are those that include companions separated by up to 16 000 au. Unresolved and resolved companions are taken into account in the final derived companion rate.
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