  We present a high-angular-resolution molecular line and millimeter continuum
study of the massive star formation site IRAS 05358+3543. The most remarkable
feature is a highly collimated (collimation factor ~10) and massive (>10 M_sun)
bipolar outflow of 1 pc length, which is part of a quadrupolar outflow system.
The three observed molecular outflows forming the IRAS 05358+3543 outflow
system resemble, in structure and collimation, those typical of low-mass
star-forming regions. They might therefore, just like low-mass outflows, be
explained by shock entrainment models of jets. We estimate a mass accretion
rate of 10^{-4) M_sun/yr, sufficient to overcome the radiative pressure of the
central object and to build up a massive star, lending further support to the
hypothesis that massive star formation occurs similarly to low-mass star
formation, only with higher accretion rates and energetics.
