Fig. 2.

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Distribution of the additional proper motion components in right ascension (Δμα*) and declination (Δμδ) caused by secular aberration drift due to the change in the line of sight for Galactic stars with a total proper motion exceeding 1 mas yr−1. (a) Scatter plot of Δμα* versus Δμδ. The ten sources with the greatest additional proper motion are highlighted, with their names labeled near the data points. (b) Histogram of Δμα*. (c) Histogram of Δμδ.
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