a series of photometric and spectroscopic observations carried out by p. ostrov between from 1998 to 2001 revealed that lh54-425 varied very slightly with a regular period of 2.2475 days due to distorted stars in a close binary system composed by an o3 class giant and an approximately o5 class companion. the masses of the two stars were estimated at and . a derivation of the orbit in 2008 using more accurate radial velocity data defined the companions as o3 and o5 main sequence stars with masses of and respectively.