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Bulges of edge-on galaxies are often boxy/peanut-shaped (B/PS), and unsharpmasks reveal the presence of an X shape. Simulations show that these shapes canbe produced by dynamical processes driven by a bar which vertically thickensthe centre. In the Milky Way, which contains such a B/PS bulge, the X-shapedstructure is traced by the metal-rich stars but not by the metal-poor ones.Recently Debattista et al. (2016) interpreted this property as a result of thevarying effect of the bar on stellar populations with different startingkinematics. This kinematic fractionation model predicts that cooler populationsat the time of bar formation go on to trace the X shape, whereas hotterpopulations are more uniformly distributed. As this prediction is not specificto the Milky Way, we test it with MUSE observations of the B/PS bulge in thenearby galaxy NGC 4710. We show that the metallicity map is more peanut-shapedthan the density distribution itself, in good agreement with the prediction.This result indicates that the X-shaped structure in B/PS bulges is formed ofrelatively metal-rich stars that have been vertically redistributed by the bar,whereas the metal-poor stars have a more uniform, box-shaped distribution.

Peanut-shaped metallicity distributions in bulges of edge-on galaxies: the case of NGC 4710