IRAS 16293-2422 is a very well studied young stellar system seen in projection towards the L1689N cloud in the Ophiuchus complex .
However , its distance is still uncertain with a range of values from 120 pc to 180 pc .
Our goal is to measure the trigonometric parallax of this young star by means of H _ { 2 } O maser emission .
We use archival data from 15 epochs of VLBA observations of the 22.2 GHz water maser line .
By modeling the displacement on the sky of the H _ { 2 } O maser spots , we derived a trigonometric parallax of 7.1 \pm 0.6 mas , corresponding to a distance of 141 _ { -21 } ^ { +30 } pc .
This new distance is in good agreement with recent values obtained for other magnetically active young stars in the L1689 cloud .
We relate the kinematics of these masers with the outflows and the recent ejections powered by source A in the system .