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Observations of massive stars in young open clusters (< ~8 Myr) have shownthat a majority of them are in binary systems, most of which will interactduring their life. Populations of massive stars older than ~20 Myr allow us toprobe the outcome of such interactions after many systems have experienced massand angular momentum transfer. Using multi-epoch integral-field spectroscopy,we investigate the multiplicity properties of the massive-star population inNGC 330 (~40 Myr) in the Small Magellanic Cloud to search for imprints ofstellar evolution on the multiplicity properties. From six epochs of VLT/MUSEobservations supported by adaptive optics we extract spectra and measure radialvelocities for stars brighter than F814W = 19. We identify single-linedspectroscopic binaries through significant RV variability as well asdouble-lined spectroscopic binaries, and quantify the observational biases forbinary detection. The observed spectroscopic binary fraction is 13.2+/-2.0 %.Considering period and mass ratio ranges from log(P)=0.15-3.5, and q = 0.1-1.0,and a representative set of orbital parameter distributions, we find abias-corrected close binary fraction of 34 +8 -7 %. This seems to decline forthe fainter stars, which indicates either that the close binary fraction dropsin the B-type domain, or that the period distribution becomes more heavilyweighted towards longer orbital periods. Both fractions vary strongly indifferent regions of the color-magnitude diagram which probably reveals theimprint of the binary history of different groups of stars. We provide thefirst homogeneous RV study of a large sample of B-type stars at a lowmetallicity. The overall bias-corrected close binary fraction of B stars in NGC330 is lower than the one reported for younger Galactic and LMC clusters. Moredata are needed to establish whether this result from an age or a metallictyeffect.

The young massive SMC cluster NGC 330 seen by MUSE II. Multiplicity properties of the massive-star population