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Time series of spectroscopic, speckle-interferometric, and opticallong-baseline-interferometric observations confirm that $\nu$ Gem is ahierarchical triple system. It consists of an inner binary composed of twoB-type stars and an outer classical Be star. Several photospheric spectrallines of the inner components were disentangled, revealing two stars with verydifferent rotational broadening ($\sim$260 and $\sim$140 kms$^{-1}$,respectively), while the photospheric lines of the Be star remain undetected.From the combined spectroscopic and astrometric orbital solution it is notpossible to unambiguously cross-identify the inner astrometric components withthe spectroscopic components. In the preferred solution based on modeling ofthe disentangled line profiles, the inner binary is composed of two stars withnearly identical masses of 3.3 M$_\odot$ and the more rapidly rotating star isthe fainter one. These two stars are in a marginally elliptical orbit ($e$ =0.06) about each other with a period of 53.8 d. The third star also has a massof 3.3 M$_\odot$ and follows a more eccentric ($e$ = 0.24) orbit with a periodof 19.1 yr. The two orbits are co-directional and, at inclinations of79$^{\circ}$ and 76$^{\circ}$ of the inner and the outer orbit, respectively,about coplanar. No astrometric or spectroscopic evidence could be found thatthe Be star itself is double. The system appears dynamically stable and notsubject to eccentric Lidov-Kozai oscillations. After disentangling, the spectraof the components of the inner binary do not exhibit peculiarities that wouldbe indicative of past interactions. Motivations for a wide range of follow-upstudies are suggested.

$\nu$ Gem: a hierarchical triple system with an outer Be star