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Fig. 12


Mean proper motions and dispersions as a function of the photometric parallax M*, for the subsample of main sequence stars in Field 4-7, where each point corresponds to 180 stars. The higher number of stars on this field has allowed us to explore the proper motions as a function of M*. The rotation pattern speed clearly appears on this field for μl (top left). Similarly, σl (bottom left) also indicates a decreasing dispersion for stars lying farther away, as expected when observing the Galactic rotation.

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