GANGI, Manuele EttoreManuele EttoreGANGINISINI, BrunellaBrunellaNISINIMANARA, CARLO FELICE MARIACARLO FELICE MARIAMANARAFrance, K.K.FranceANTONIUCCI, SimoneSimoneANTONIUCCIBIAZZO, KatiaKatiaBIAZZOGIANNINI, TeresaTeresaGIANNINIHerczeg, G. J.G. J.HerczegALCALA', JUAN MANUELJUAN MANUELALCALA'FRASCA, AntonioAntonioFRASCAMaucó, K.K.MaucóCampbell-White, J.J.Campbell-WhiteSiwak, M.M.SiwakVENUTI, LAURALAURAVENUTISchneider, P. C.P. C.SchneiderKóspál, Á.Á.KóspálCARATTI O GARATTI, AlessioAlessioCARATTI O GARATTIFIORELLINO, EleonoraEleonoraFIORELLINORIGLIACO, ElisabettaElisabettaRIGLIACOYadav, R. K.R. K.Yadav2025-05-072025-05-0720230004-6361http://hdl.handle.net/20.500.12386/37094Context. Observing the spatial distribution and excitation processes of atomic and molecular gas in the inner regions (<20 au) of young (<10 Myr) protoplanetary disks helps us to understand the conditions for the formation and evolution of planetary systems. <BR /> Aims: In the framework of the PENELLOPE and ULLYSES projects, we aim to characterize the atomic and molecular component of protoplanetary disks in a sample of 11 classical T Tauri stars of the Orion OB1 and σ-Orionis associations. <BR /> Methods: We analyzed the flux-calibrated optical forbidden lines and the fluorescent ultraviolet H<SUB>2</SUB> progressions using spectra acquired with ESPRESSO at VLT, UVES at VLT, and HST-COS. Line morphologies were characterized through Gaussian decomposition. We then focused on the properties of the narrow low-velocity (full width half maximum <40 km s<SUP>−1</SUP> and |υ<SUB>p</SUB>| < 30 km s<SUP>−1</SUP>) component (NLVC) of the [O I] 630 nm line and compared them with those of the UV-H<SUB>2</SUB> lines. <BR /> Results: We found that the [O I]630 NLVC and the UV-H<SUB>2</SUB> lines are strongly correlated in terms of peak velocities, full width at half maximum values, and luminosity. Assuming that the line width is dominated by Keplerian broadening, the [O I]630 NLVC originates from a disk region between 0.5 and 3.5 au, while that of UV-H<SUB>2</SUB> originates in a region from 0.05 to 1 au. The luminosities of [O I]630 NLVC and UV-H<SUB>2</SUB> correlate with an accretion luminosity with a similar slope, as well as with the luminosity of the C IV154.8, 155 nm doublet. We discuss such correlations in the framework of the currently suggested excitation processes for the [O I]630 NLVC. <BR /> Conclusions: Our results can be interpreted in a scenario in which the [O I]630 NLVC and UV-H<SUB>2</SUB> have a common disk origin with a partially overlapped radial extension. We also suggest that the excitation of the [O I] NLVC is mainly induced by stellar far-ultraviolet continuum photons, than being of mostly thermal origin. This study demonstrates the potential of contemporaneous wide-band highresolution spectroscopy in linking different tracers of protoplanetary disks.STAMPAenArticle10.1051/0004-6361/2023465432-s2.0-85166037645https://www.aanda.org/articles/aa/full_html/2023/07/aa46543-23/aa46543-23.htmlhttp://arxiv.org/abs/2305.18940v12023A&A...675A.153GFIS/05 - ASTRONOMIA E ASTROFISICA