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Low-mass members of young stellar associations exhibit a wide spread ofrotation periods. Such a spread originates from distributions of masses andinitial rotation periods. However, multiplicity can also play a significantrole. We investigate the role played by physical companions in shortening theprimordial disc lifetime. We have compiled the most extensive list of low-massmembers of the young 25-Myr beta Pictoris association. We have measured therotation periods of about all members and used updated UVWXYZ components toassess their membership. We built the rotation period distributiondistinguishing between bona fide members and candidate members and according totheir multiplicity status. We found that single stars and components ofmultiple systems in wide orbits (>80 AU) have rotation periods that exhibit awell defined sequence arising from mass distribution. All components ofmultiple systems in close orbits (<80 AU) have rotation periods significantlyshorter than their equal-mass single counterparts. A comparison with theyounger 13 Myr h Per cluster and with the older 40-Myr open clusters/stellarassociations NGC2547, IC2391, Argus, and IC2602 and the 130-Myr Pleiades showsthat whereas the evolution of F-G stars is well reproduced by angular momentumevolution models, this is not the case for the slow K and early-M stars.Finally, we found that the amplitude of their light curves is correlatedneither with rotation nor with mass. Once single stars and wide components ofmultiple systems are separated from close components of multiple systems, therotation period distributions exhibit a well defined dependence on mass thatallows to make a meaningful comparison with similar distributions of eitheryounger or older associations/clusters. Such cleaned distributions allow to usethe stellar rotation period as age indicator, meaningfully for F and G typestars.

The beta Pictoris association low-mass members: membership assessment, rotation period distribution, and dependence on multiplicity