  The Sun produces highly dynamic and eruptive events that can drive shocks
through the corona. These shocks can accelerate electrons, which result in
plasma emission in the form of a type II radio burst. Despite the large number
of type II radio bursts observations, the precise origin of coronal shocks is
still subject to investigation. Here we present a well observed solar eruptive
event that occurred on 16 October 2015, focusing on a jet observed in the
extreme ultraviolet (EUV) by the Atmospheric Imaging Assembly (SDO/AIA), a
streamer observed in white-light by the Large Angle and Spectrometric
Coronagraph (SOHO/LASCO), and a metric type II radio burst observed by the LOw
Frequency Array (LOFAR). LOFAR interferometrically imaged the fundamental and
harmonic sources of a type II radio burst and revealed that the sources did not
appear to be co-spatial, as would be expected from the plasma emission
mechanism. We correct for the separation between the fundamental and harmonic
using a model which accounts for scattering of radio waves by electron density
fluctuations in a turbulent plasma. This allows us to show the type II radio
sources were located $\sim$0.5 R$_\odot$ above the jet and propagated at a
speed of $\sim$1000 kms$^{-1}$, which was significantly faster than the jet
speed of $\sim$200 kms$^{-1}$. This suggests that the type II burst was
generated by a piston shock driven by the jet in the low corona.
