  HD163296 is a Herbig Ae star which drives a bipolar knotty jet with a total
length of ~6000au. Strong evidence exists that the disk of HD163296 harbors
planets. Studies have shown that the presence of companions around jet-driving
stars could affect the morphology of the jets. This includes a `wiggling' of
the jet axis and a periodicity in the positions of the jet knots. In this study
we investigate the morphology (including the jet width and axis position) and
proper motions of the HD163296 jets, and use our results to better understand
the whole system.This study is based on optical integral-field spectroscopy
observations obtained with VLT/MUSE in 2017. Using spectro-images and position
velocity diagrams extracted from the MUSE data cube, we investigated the number
and positions of the jet knots. A comparison was made to X-Shooter data
collected in 2012 and the knot proper motions were estimated. The jet width and
jet axis position with distance from the star were studied from the extracted
spectro-images. We observe the merging of knots and identify two previously
undetected knots. Measurements of the jet axis position reveal a similar
pattern of deviation in all forbidden emission lines along the first 20 arc
seconds of the jets. This result is interpreted as being due to asymmetric
shocks and not due to a wiggling of the jet axis. The number of new knots
detected and their positions challenge the 16-year knot ejection periodicity
proposed in prior studies, arguing for a more complicated jet system than was
previously assumed. We use the non-detection of a jet axis wiggling to rule out
companions with a mass $>$0.1~\Msun\ and orbits between 1~au and 35~au. Any
object inferred at these distances using other methods must be a brown dwarf or
planet, otherwise it would have impacted the jet axis position. Both the
precession and orbital motion scenarios are considered.
