Abstract
^{12}CO (J=1 → 0) observations towards WR 102 and its associated nebula (G2.4+1.4) revealed the presence of two molecular concentrations associated with them. The radial velocity of these concentrations are 24 and 13 km s^{-1}, respectively. The former represents the molecular cloud envisaged in the model of Dopita and Lozinskaya, whilst the latter may be molecular gas accelerated towards the observer by the strong stellar winds. The total amount of molecular gas in this complex is about 760 solar masses.
