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We present observations from the Gaia-ESO Survey in the lines of H$\alpha$,[N II], [S II] and He I of nebular emission in the central part of the CarinaNebula.  We investigate the properties of the two already known kinematic components(approaching and receding, respectively), which account for the bulk ofemission. Moreover, we investigate the features of the much less knownlow-intensity high-velocity (absolute RV $>$50 km/s) gas emission.  We show that gas giving rise to H$\alpha$ and He I emission is dynamicallywell correlated, but not identical, to gas seen through forbidden-lineemission. Gas temperatures are derived from line-width ratios, and densitiesfrom [S II] doublet ratios. The spatial variation of N ionization is alsostudied, and found to differ between the approaching and receding components.The main result is that the bulk of the emission lines in the central part ofCarina arises from several distinct shell-like expanding regions, the mostevident found around $\eta$ Car, the Trumpler 14 core, and the star WR25. Such"shells" are non-spherical, and show distortions probably caused by collisionswith other shells or colder, higher-density gas. Part of them is also obscuredby foreground dust lanes, while only very little dust is found in theirinterior. Preferential directions, parallel to the dark dust lanes, are foundin the shell geometries and physical properties, probably related to strongdensity gradients in the studied region. We also find evidence that theionizing flux emerging from $\eta$ Car and the surrounding Homunculus nebulavaries with polar angle. The high-velocity components in the wings of H$\alpha$are found to arise from expanding dust reflecting the $\eta$ Car spectrum.

Gaia-ESO Survey: Gas dynamics in the Carina Nebula through optical emission lines