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The mechanism for jet formation in the disks of T Tauri stars is poorlyunderstood. Observational benchmarks to launching models can be provided bytracing the physical properties of the kinematic components of the wind and jetin the inner 100 au of the disk surface. In the framework of the GHOsT (GIARPSHigh-resolution Observations of T Tauri stars) project, we aim to perform amulti-line analysis of the velocity components of the gas in the jetacceleration zone. We analyzed the GIARPS-TNG spectra of six objects in theTaurus-Auriga complex (RY Tau, DG Tau, DL Tau, HN Tau, DO Tau, RW Aur A).Thanks to the combined high-spectral resolution (R=50000-115000) and widespectral coverage (~400-2400 nm) we observed several O, S+, N, N+, and Fe+forbidden lines spanning a large range of excitation and ionization conditions.In four objects (DG Tau, HN Tau, DO Tau, RW Aur A), temperature (T_e), electronand total density (n_e, n_H), and fractional ionization (x_e) were derived as afunction of velocity through an excitation and ionization model. The abundanceof gaseous iron, X(Fe), a probe of the dust content in the jet, was derived inselected velocity channels. The physical parameters vary smoothly withvelocity, suggesting a common origin for the different kinematic components. InDG Tau and HN Tau, T_e, x_e, and X(Fe) increase with velocity (roughly from6000 K, 0.05, 10% X(Fe)_sun to 15000 K, 0.6, 90% X(Fe)_sun). This trend is inagreement with disk-wind models in which the jet is launched from regions ofthe disk at different radii. In DO Tau and RW Aur A, we infer x_e < 0.1, n_H~10^6-7 cm^-3, and X(Fe) <~ X(Fe)_sun at all velocities. These findings aretentatively explained by the formation of these jets from dense regions insidethe inner, gaseous disk, or as a consequence of their high degree ofcollimation.

GIARPS High-resolution Observations of T Tauri stars (GHOsT). I. Jet line emission