Fig. 8.
Left panel: mean Y-position versus mean X-position for the determination of the pattern speed of NGC 5257 using the Tremaine–Weinberg (TW) method. The galaxy has been rotated so that the PA lies along the X axis. Dotted colours trace the monochromatic (Hα) emission of the galaxy. Top right panel: ⟨V(x)⟩ versus ⟨x⟩ for NGC 5257. Bottom right panel: zoom of the ⟨V(x)⟩ versus ⟨x⟩ plot for NGC 5257. The variables ⟨V(x)⟩ and ⟨x⟩ are described in Sect. 4.6.
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