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HD163296 is a Herbig Ae star which drives a bipolar knotty jet with a totallength of ~6000au. Strong evidence exists that the disk of HD163296 harborsplanets. Studies have shown that the presence of companions around jet-drivingstars could affect the morphology of the jets. This includes a `wiggling' ofthe jet axis and a periodicity in the positions of the jet knots. In this studywe investigate the morphology (including the jet width and axis position) andproper motions of the HD163296 jets, and use our results to better understandthe whole system.This study is based on optical integral-field spectroscopyobservations obtained with VLT/MUSE in 2017. Using spectro-images and positionvelocity diagrams extracted from the MUSE data cube, we investigated the numberand positions of the jet knots. A comparison was made to X-Shooter datacollected in 2012 and the knot proper motions were estimated. The jet width andjet axis position with distance from the star were studied from the extractedspectro-images. We observe the merging of knots and identify two previouslyundetected knots. Measurements of the jet axis position reveal a similarpattern of deviation in all forbidden emission lines along the first 20 arcseconds of the jets. This result is interpreted as being due to asymmetricshocks and not due to a wiggling of the jet axis. The number of new knotsdetected and their positions challenge the 16-year knot ejection periodicityproposed in prior studies, arguing for a more complicated jet system than waspreviously assumed. We use the non-detection of a jet axis wiggling to rule outcompanions with a mass $>$0.1~\Msun\ and orbits between 1~au and 35~au. Anyobject inferred at these distances using other methods must be a brown dwarf orplanet, otherwise it would have impacted the jet axis position. Both theprecession and orbital motion scenarios are considered.

The Morphology of the HD 163296 jet as a window on its planetary system