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Rapid rotation and nonradial pulsations enable Be stars to build decretiondisks, where the characteristic line emission forms. A major but unconstrainedfraction of Be stars owe their rapid rotation to mass and angular-momentumtransfer in a binary. The faint, stripped companions can be helium-burningsubdwarf OB-type stars (sdOBs), white dwarfs (WDs), or neutron stars. Wepresent optical/near-IR CHARA interferometry of 37 Be stars selected forspectroscopic indications of low-mass companions. From multi-epoch $H$- and/or$K$-band interferometry plus radial velocities and parallaxes collectedelsewhere, we constructed 3D orbits and derived flux ratios and absolutedynamical masses of both components for six objects, quadrupling the number ofanchor points for evolutionary models. In addition, a new wider companion wasidentified for the known Be + sdO binary 59 Cyg, while auxiliary VLTI/GRAVITYspectrointerferometry confirmed circumstellar matter around the sdO companionto HR 2142. On the other hand, we failed to detect any companion to the six Bestars with $\gamma$ Cas-like X-ray emission, with sdOB and main-sequencecompanions of the expected spectroscopic mass being ruled out for theX-ray-prototypical stars $\gamma$ Cas and $\pi$ Aqr, leaving the elusive WDcompanions as the most likely companions, as well as a likely explanation ofthe X-rays. No low-mass main-sequence close companions were identified in theother stars.

The CHARA Array interferometric program on the multiplicity of classical Be stars: new detections and orbits of stripped subdwarf companions