We present two Very Large Array observations of the pre-main-sequence star PV Cephei , taken with a separation of 10.5 years .
These data show that the proper motions of this star are \mu _ { \alpha } \cos \delta = +10.9 \pm 3.0 mas yr ^ { -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 illumination of the nearby reflection nebula NGC 7023 .
This result suggests that PV Cephei is not a rapidly moving run-away star as suggested by previous studies .
The large velocity of PV Cephei had been inferred from the systematic eastward displacement of the bisectors of successive pairs of Herbig Haro knots along its flow .
These systematic shifts might instead result from an intrinsic dissymmetry in the ejection mechanisms , or from an asymmetric distribution of the circumstellar material .