Fig. 10.
Multi-wavelength rotation curves of NGC 5257 (top panel) and NGC 5258 (bottom panel) displaying all observed points. Small squares in the inner parts of the curve correspond to optical Fabry–Perot Hα observations. Empty circles in the inner parts correspond to the CO(1-0) curve derived by Iono et al. (2005). Empty squares in the outer parts correspond to the HI curve also derived by Iono et al. (2005).
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