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Fig. 3.


Microturbulence velocity values obtained for the sample stars by the ASPCAP pipeline (upper panel) and by our preliminary run with the BACCHUS code (lower panel). Red points indicate stars with [Fe/H] < −1.5 and black points stars with [Fe/H] > −1.5. The dashed line shows the relation derived in the optical by the Gaia-ESO survey assuming Teff = 4500 K and [Fe/H] = −1.5. Both works show a good correspondence with the optical data for the metal-rich stars, but a larger dispersion is obtained for low-metallicity stars.

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