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Fig. 10


Zoomed view on the central part of the sky (projected as in Fig. 7) after step 1 described in Sect. 3.3. The intensities are equivalent to the sum of four original sky images after background subtraction. In this example, the central proper motion grid point is at (μαcosδ,μδ) = (2.5, 2.5) mas/yr, similar to the proper motion bin shown in Fig. 7. Top: set A (sum of four 2MAst HQb5 images), middle: set B (UCAC4 HQ sum), and bottom: set AB (the square root of the product of the two sums). Open squares mark the cluster candidates found after step 4 of Sect. 3.3 with the given central proper motion. Open lozenges indicate candidates with similar (overlapping) proper motions.

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