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Many young and intermediate age massive stellar clusters host bimodaldistributions in the rotation rates of their stellar populations, with adominant peak of rapidly rotating stars and a secondary peak of slow rotators.The origin of this bimodal rotational distribution is currently debated and twomain theories have been put forward in the literature. The first is thatall/most stars are born as rapid rotators and that interacting binaries brake afraction of the stars, resulting in two populations. The second is that therotational distribution is a reflection of the early evolution of pre-mainsequence stars, in particular, whether they are able to retain or lose theirprotoplanetary discs during the first few Myr. Here, we test the binary channelby exploiting multi-epoch VLT/MUSE observations of NGC 1850, a 100Myr massivecluster in the LMC, to search for differences in the binary fractions of theslow and fast rotating populations. If binarity is the cause of the rotationalbimodality, we would expect that the slowly rotating population should have amuch larger binary fraction than the rapid rotators. However, in our data wedetect similar fractions of binary stars in the slow and rapidly rotatingpopulations (5.9+/-1.1% and 4.5+/-0.6%, respectively).Hence, we conclude thatbinarity is not a dominant mechanism in the formation of the observed bimodalrotational distributions.

Exploring the role of binarity in the origin of the bimodal rotational velocity distribution in stellar clusters