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Using the Very Long Baseline Array (VLBA), we have observed the radiocontinuum emission from the young stellar object HW 9 in the Cepheus Astar-forming region at ten epochs between 2007 February and 2009 November. Dueto its strong radio variability, the source was detected at only four of theten epochs. From these observations, the trigonometric parallax of HW 9 wasdetermined to be $\pi$ = 1.43 $\pm$ 0.07 mas, in excellent agreement with arecent independent VLBA determination of the trigonometric parallax of amethanol maser associated with the nearby young stellar source HW 2 ($\pi$ =1.43 $\pm$ 0.08 mas). This concordance in results, obtained in one case fromcontinuum and in the other from line observations, confirms the reliability ofVery Long Baseline Array trigonometric parallax measurements. By combining thetwo results, we constrain the distance to Cepheus A to be 700$_{-28}^{+31}$ pc,an uncertainty of 3.5%.

VLBA determination of the distance to nearby star-forming regions VI. The distance to the young stellar object HW 9 in Cepheus A