  The Gaia-ESO Survey is an European Southern Observatory (ESO) public
spectroscopic survey that targeted $10^5$ stars in the Milky Way covering the
major populations of the disk, bulge and halo. The observations were made using
FLAMES on the VLT obtaining both UVES high ($R\sim47,000$) and GIRAFFE medium
($R\sim20,000$) resolution spectra.
  The analysis of the Gaia-ESO spectra was the work of multiple analysis teams
(nodes) within five working groups (WG). The homogenisation of the stellar
parameters within WG11 (high resolution observations of FGK stars) and the
homogenisation of the stellar parameters within WG10 (medium resolution
observations of FGK stars) is described here. In both cases, the homogenisation
was carried out using a bayesian Inference method developed specifically for
the Gaia-ESO Survey by WG11.
  The WG10 homogenisation primarily used the cross-match of stars with WG11 as
the reference set in both the stellar parameter and chemical abundance
homogenisation. In this way the WG10 homogenised results have been placed
directly onto the WG11 stellar parameter and chemical abundance scales. The
reference set for the metal-poor end was sparse which limited the effectiveness
of the homogenisation in that regime.
  For WG11, the total number of stars for which stellar parameters were derived
was 6,231 with typical uncertainties for Teff, log g and [Fe/H] of 32~K, 0.05
and 0.05 respectively. One or more chemical abundances out of a possible 39
elements were derived for 6,188 of the stars.
  For WG10, the total number of stars for which stellar parameters were derived
was 76,675 with typical uncertainties for Teff, log g and [Fe/H] of 64~K, 0.15
and 0.07 respectively. One or more chemical abundances out of a possible 30
elements were derived for 64,177 of the stars.
