  Highly collimated parsec-scale jets, generally linked to the presence of an
accretion disk, are a commonly observed phenomenon from revealed low-mass young
stellar objects. In the past two decades, only a very few of these objects have
been directly (or indirectly) observed towards high-mass (M > 8 M$_{\odot}$)
young stellar objects, adding to the growing evidence that disk-mediated
accretion is a phenomenon also occurring in high-mass stars, the formation
mechanism of which is still poorly understood. Of the observed jets from
massive young stars, none is in the optical regime (due to these being
typically highly obscured by their native material), and none are found outside
of the Milky Way. Here, we report the detection of HH 1177, the first
extragalactic optical ionized jet originating from a massive young stellar
object located in the Large Magellanic Cloud. The jet is highly collimated over
the entire measured extent of at least 10 pc, and has a bipolar geometry. The
presence of a jet indicates ongoing, disk-mediated accretion, and together with
the high degree of collimation, this system is therefore likely to be an
up-scaled version of low-mass star formation. We conclude that the physics
governing jet launching and collimation is independent of stellar mass.
