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Fig. 1.


Galactic rotational curve. Shown are the potential of model I, model II, and model III (in red, green, and blue, respectively). For each model the galactic components behave as follows: the bulge contributes the most within 2 kpc, the disk reaches a peak at around 10 kpc, and the extended rotational curve is due to the halo component. Observational data from Bhattacharjee et al. (2014) within 10 kpc is plotted with error lines (in black).

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