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

Open Access

Fig. 3

$σ_{v_{l o s}}$ ${\sigma _{{{\rm{\v }}_{los}}}}$ line-of-sight velocity dispersion profiles of our quality APOGEE sample (error bar curves) and of our mock catalogue (shaded areas of height ±σ). The profiles are plotted for stars with |X| < 1.5 kpc and |ℓ|< 2°, for metal-rich stars ([Fe/H] > 0), and two metal-rich populations defined as very metal-rich (0 < [Fe/H] ≤ 0.3) and extremely metal-rich ([Fe/H] > 0.3).

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