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This paper aims at revisit the physical and dynamical properties of the warmatomic gas in the inner disk region of classical T Tauri stars (CTTs) andrelate them to the properties of the outer dusty disk. We used the highresolution (R=115,000) spectra of 36 CTTs observed as part of the GHOsT projectand analysed the profile and luminosity of the brightest optical forbiddenlines, namely [OI]630 and 557nm, [SII]406 and 673nm, and [NII]658nm. We findthat in about 40% of sources the so-called narrow low-velocity component (NLVC)display a peak velocity compatible with the stellar velocity. In these sources,that typically show lower mass accretion rates and the absence of a jet, the[OI]630nm profiles are well fitted by a simple Keplerian disk model, indicatingthat the emission from the disk is dominant with respect to the windcontribution. For transitional disks (TD), no correlation is found between$R_{kep}$, derived from the line HWHM, and the size of the dust cavity. We alsosee an anti-correlation between the [OI] 557/630 nm ratio and $R_{kep}$, whichsuggests that the [OI] emitting region expands as the gas cools and becomesless dense. We confirmed previous findings on the density and temperatureranges implied by the line ratios, and additionally constrained the ionisationfraction in the NLVC to be < 0.1. We however discuss the limits of applyingthis diagnostic to winds that are not spatially resolved. For the outflowcomponent, we estimated the mass-loss for both the disk winds and jets andcompared the results with X-ray photoevaporative models. We conclude thatwithout better knowledge of the wind geometry, and given the limitation of thediagnostics, the mass-loss in the wind traced by the LVC cannot be constrainedbetter than a factor of 100, with a mass-loss/mass-accretion ratio spanningbetween ~ 0.01 and more than 1.

GIARPS High-resolution Observations of T Tauri stars (GHOST) V. New insights into disk winds from 3 km/s resolution observations