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The formation of massive stars remains poorly understood and little is knownabout their birth multiplicity properties. Here, we investigate the strikinglylow radial-velocity dispersion measured for a sample of 11 massive pre- andnear-main-sequence stars (sigma_rv = 5.6 +/- 0.2 km/s) in the young massivestar forming region M17 to obtain first constraints on the multiplicityproperties of young massive stellar objects. Methods: We compute the RVdispersion of synthetic populations of massive stars for various multiplicityproperties and we compare the simulated sigma_rv distributions to the observedvalue. We specifically investigate two scenarios: a low binary fraction and adearth of short-period binary systems. Results: Simulated populations with lowbinary fractions (f_bin = 0.12_{-0.09}^{+0.16}) or with truncated perioddistributions (P_cutoff > 9 months) are able to reproduce the low sigma_rvobserved within their 68%-confidence intervals. Parent populations with f_bin >0.42 or P_cutoff < 47 d can however be rejected at the 5%-significance level.Both constraints are contrast with the high binary fraction and plethora ofshort-period systems found in few Myr-old, OB-type populations. To explain thedifference, the first scenario requires a variation of the outcome of themassive star formation process. In the the second scenario, compact binariesmust form later on, and the cut-off period may be related to physicallength-scales representative of the bloated pre-main-sequence stellar radii orof their accretion disks. Conclusions: If the obtained constraints arerepresentative of the overall properties of massive young stellar objects, ourresults may provide support to a formation process in which binaries areinitially formed at larger separations, then harden or migrate to produce thetypical (untruncated) power-law period distribution observed in few Myr-old OBbinaries.

A dearth of short-period massive binaries in the young massive star forming region M17: Evidence for a large orbital separation at birth?