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Context. Brown dwarfs are poorly understood transition objects between starsand planets, with several competing mechanisms having been proposed for theirformation. Mass measurements are generally difficult for isolated objects butalso for brown dwarfs orbiting low-mass stars, which are often too faint forspectroscopic follow-up. Aims. Microlensing provides an alternative tool forthe discovery and investigation of such faint systems. Here we present theanalysis of the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035, whichis due to a binary system composed of a brown dwarf orbiting a red dwarf.Methods. Thanks to extensive ground observations and the availability of spaceobservations from Spitzer, it has been possible to obtain accurate estimates ofall microlensing parameters, including parallax, source radius and orbitalmotion of the binary lens. Results. After accurate modeling, we find that thelens is composed of a red dwarf with mass $M_1 = 0.149 \pm 0.010M_\odot$ and abrown dwarf with mass $M_2 = 0.0463 \pm 0.0031M_\odot$, at a projectedseparation of $a_\perp = 0.585$ au. The system has a peculiar velocity that istypical of old metal-poor populations in the thick disk. Percent precision inthe mass measurement of brown dwarfs has been achieved only in a fewmicrolensing events up to now, but will likely become common with the Romanspace telescope.

Precision measurement of a brown dwarf mass in a binary system in the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035