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Observing the spatial distribution and excitation processes of atomic andmolecular gas in the inner regions (< 20 au) of young (< 10 Myr) protoplanetarydisks helps us to understand the conditions for the formation and evolution ofplanetary systems. In the framework of the PENELLOPE and ULLYSES projects, weaim to characterize the atomic and molecular component of protoplanetary disksin a sample of 11 Classical T Tauri Stars (CTTs) of the Orion OB1 and$\sigma$-Orionis associations. We analyzed the flux-calibratedoptical-forbidden lines and the fluorescent ultraviolet $\rm H_2$ progressionsusing spectra acquired with ESPRESSO at VLT, UVES at VLT and HST-COS. Linemorphologies were characterized through Gaussian decomposition. We then focusedon the properties of the narrow low-velocity (FWHM < 40 $km$ $s^{-1}$ and|$v_p$| < 30 $km$ $s^{-1}$) component (NLVC) of the [OI] 630 nm line, comparedwith the properties of the UV-$\rm H_2$ lines. We found that the [OI]630 NLVCand the UV-$\rm H_2$ lines are strongly correlated in terms of peak velocities,full width at half maximum, and luminosity. The luminosities of the [OI]630NLVC and UV-$\rm H_2$ correlate with the accretion luminosity with a similarslope, as well as with the luminosity of the CIV 154.8, 155 nm doublet. Wediscuss such correlations in the framework of the currently suggestedexcitation processes for the [OI]630 NLVC. Our results can be interpreted in ascenario in which the [OI]630 NLVC and UV-$\rm H_2$ have a common disk originwith a partially overlapped radial extension. We also suggest that theexcitation of the [OI] NLVC is mainly induced by stellar FUV continuum photonsmore than being of thermal origin. This study demonstrates the potential ofcontemporaneous wide-band high-resolution spectroscopy in linking differenttracers of protoplanetary disks.

PENELLOPE IV. A comparison between optical forbidden lines and $\rm H_2$ UV lines in the Orion OB1b and $\sigma$-Ori associations