  We have made a serendipitous discovery of an enigmatic outflow source, IRAS
05506+2414 (hereafter IRAS 05506), as part of a multi-wavelength survey of
pre-planetary nebulae (PPNs). The HST optical and near-infrared images show a
bright compact central source with a jet-like extension, and a fan-like spray
of high-velocity (with radial velocities upto 350 kms/s) elongated knots which
appear to emanate from it. These structures are possibly analogous to the
near-IR "bullets" seen in the Orion nebula. Interferometric observations at 2.6
mm show the presence of a high-velocity CO outflow and a continuum source also
with a faint extension, both of which are aligned with the optical jet
structure. IRAS 05506 is most likely not a PPN. We find extended NH3 (1,1)
emission towards IRAS 05506; these data together with the combined presence of
far-IR emission, H2O and OH masers, and CO and CS J=2-1 emission, strongly
argue for a dense, dusty star-forming core associated with IRAS 05506. IRAS
05506 is probably an intermediate-mass or massive protostar, and the very short
time-scale (200 yr) of its outflows indicates that it is very young. If IRAS
05506 is a massive star, then the lack of radio continuum and the late G --
early K spectral type we find from our optical spectra implies that in this
object we are witnessing the earliest stages of its life, while its temperature
is still too low to provide sufficient UV flux for ionisation.
