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We present two Very Large Array observations of the pre-main-sequence star PVCephei, taken with a separation of 10.5 years. These data show that the propermotions of this star are $\mu_\alpha \cos \delta = +10.9 \pm 3.0$ masyr$^{-1}$; $\mu_\delta = +0.2 \pm 1.8$ mas yr$^{-1}$, very similar to those-previously known- of HD 200775, the B2Ve star that dominates the illuminationof the nearby reflection nebula NGC 7023. This result suggests that PV Cepheiis not a rapidly moving run-away star as suggested by previous studies. Thelarge velocity of PV Cephei had been inferred from the systematic eastwarddisplacement of the bisectors of successive pairs of Herbig Haro knots alongits flow. These systematic shifts might instead result from an intrinsicdissymmetry in the ejection mechanisms, or from an asymmetric distribution ofthe circumstellar material.

A reassessment of the kinematics of PV Cephei based on accurate proper motion measurements