Comparison of the posterior distribution for different measurements of the proper motion of the Sun. We show our own results taking the emitter peculiar velocities into account by using the covariance matrix in Eq. (16) and by means of corrections according to Carrick et al. (2015), respectively. For comparison, we also show the results from the analysis of high multipole moments of the CMB (Saha et al. 2021) and assuming that the CMB dipole is entirely explained by solar motion (Planck Collaboration I 2020). In the latter case, the uncertainties are too small to be displayed properly. We instead indicate the value by a vertical line.