  EUV jets situated in coronal holes are thought to play an important role in
supplying heated material to the corona and solar wind. The multi-wavelength
capabilities and high signal-to-noise of detectors on-board SDO allows for
detailed study of these jet's evolution. We aim to exploit SDO's capabilities
to reveal information on the jet dynamics and obtain estimates for plasma
properties associated with the jet. We study the dynamics an EUV jet with
AIA/SDO at a coronal hole boundary. The details of the jet evolution are
discussed and measurements of the jet's parameters, e.g. length, width, life
time, outward speed, are obtained. Further, automated emission measure analysis
is exploited to determine estimates for the temperature and density of the jet.
A propagating transverse wave supported by the jet spire is also observed.
Measurement of the wave properties are exploited for magneto-seismology and are
used in conjunction with the emission measure results to estimate the magnetic
field strength of the jet. We present a detailed description of the jet's
evolution, with new evidence for plasma flows, prior to the jet's initiation,
along the loops at the base of the jet and also find further evidence that
flows along the jet spire consist of multiple, quasi-periodic small-scale
plasma ejection events. In addition, DEM analysis suggests that the jet has
temperatures of $\log{5.89\pm0.08}$ K and electron densities of
$\log{8.75\pm0.05}$ cm$^{-3}$. Measured properties of the transverse wave
suggest the wave is heavily damped as it propagates along the jet spire with
speeds of $\sim110$ km/s. The magneto-seismological inversion of the wave
parameters provides values of $B=1.21\pm0.2$ G along the jet spire, which is in
line with previous estimates for open fields in coronal holes.}
