The disc origin of the Milky Way bulge - The high velocity dispersion of metal-rich stars at low latitudes

Open Access

Fig. A.1

Line-of-sight velocity dispersion, $σ_{v_{l o s}}$ ${\sigma _{{{\rm{\v }}_{los}}}}$ , profiles of the three components in their initial condition (hatched areas and dotted lines) compared to the final profiles (filled areas and solid lines), with the same binning and colour coding used in Fig. 2. The profiles are plotted for stars with |ℓ|< 2° and |X| < 1.5kpc.

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