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We present high resolution images of the bipolar outflow from W51e2, whichare produced from the Submillimeter Array archival data observed for CO(3-2)and HCN(4-3) lines with angular resolutions of 0.8" x 0.6" and 0.3" x 0.2",respectively. The images show that the powerful outflow originates from theprotostellar core W51e2-E rather than from the ultracompact HII region W51e2-W.The kinematic timescale of the outflow from W51e2-E is about 1000 yr, youngerthan the age (~5000 yr) of the ultracompact HII region W51e2-W. A large massloss rate of ~1 x 10^{-3} M_sun yr^{-1} and a high mechanical power of 120L_sun are inferred, suggesting that an O star or a cluster of B stars areforming in W51e2-E. The observed outflow activity along with the inferred largeaccretion rate indicates that at present W51e2-E is in a rapid phase of starformation.

A bipolar outflow from the massive protostellar core W51e2-E