different epochs independently, and measured the position of stars at each epoch. Stellar positions have been corrected for geometrical distortion by using of the solutions provided by @bellini2009b [@bellini2011]. We measured proper motions as in @piotto2012 [see their Section 4] by comparing the distortion-corrected stellar positions at different epochs. To derive the proper motion of each star and minimize the effect of any residual distortion, we used the sample of 45 nearest cluster members as reference stars to fix the zero point of the motion. Hence, our measurements from [*HST*]{} data provide proper motions relative to the average local cluster motion.

    CAMERA     FILTER        DATE              N$\times$EXPTIME         PROGRAM   PI
  ----------- -------- ---------------- ------------------------------- --------- ---------------------
                                                      M22                         
    ACS/WFC    F606W     Jul 01 2006           3s$+$4$\times$55s        10775     A.Sarajedini
    ACS/WFC    F814W     Jul 01 2006           3s$+$4$\times$65s        10775     A.Sarajedini
   WFC3/UVIS   F814W     Sep 23 2010             2$\times$50s           12311     G.Piotto
   WFC3/UVIS   F814W    Mar 17-18 2011           2$\times$50s           12311     G.Piotto
   WFC3/UVIS   F395N     May 18 2011     2$\times$631s$+$2$\times$697s  12193     J.-W.Lee
   WFC3/UVIS   F467M     May 18 2011     2$\times$361s$+$2$\times$367s  12193     J.-W.Lee
   WFC3/UVIS   F547M     May 18 2011          74s$+$3$\times$75s        12193     J.-W.Lee
   WFC3/UVIS   F438W     Jul 17 2014             2$\times$141s          13297     G.Piotto
                                              $\omega\,$Centauri                  
    ACS/WFC    F435W     Jun 27 2002          12s$+$3$\times$340s       9442      A.Cool
   WFC3/UVIS   F438W     Jul 15 2009                  35s               11452     J.Kim Quijano
   WFC3/UVIS   F814W     Jul 15 