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Fig. 10


Rotation of the NGC 4636 globular cluster system. Left: circles show the rotation of the final blue sample (BlueFinal) computed for moving bins of 50 GCs with a step site of 5 GCs. The grey area indicates the radial coverage and the uncertainties. Dots indicate independent bins. The upper sub-panel shows the rotation angle Θ0 vs. projected galactocentric radius. The NGC 4636 photometric major and minor axis are shown as long-dashed and dotted horizontal lines, respectively. The lower sub-panel shows the amplitude A as function of radius. Middle: the same as the left panel but for the final red sample (RedFinal). In both plots, the dashed vertical lines indicate the radial range for which we have the best spatial coverage of the GCS (see also Sect. 4.1). Right: velocity versus position angle for the 141 blue GCs (circles) from the sample BlueFinal with distances between  and 8′. The thick solid curve shows the best fit of Eq. (3) to the data, the thin dashed curves are offset by the sample dispersion (σ = 180   km   s-1). The vertical dashed and solid lines show the best-fit Θ0 and the photometric major axis of NGC 4636, respectively. The grey areas indicate the uncertainty ΔΘ0. The squares show the mean velocity for bins of 60°. The unfilled histogram at the bottom shows the angular distribution of the GCs (the bins have a width of 20° and the counts are multiplied by a factor of 20 for graphic convenience).

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