Montalto, M.M.MontaltoGreco, N.N.GrecoBIAZZO, KatiaKatiaBIAZZODESIDERA, SilvanoSilvanoDESIDERAANDREUZZI, GloriaGloriaANDREUZZIBieryla, A.A.BierylaBIGNAMINI, ANDREAANDREABIGNAMINIBONOMO, ALDO STEFANOALDO STEFANOBONOMOBriceño, C.C.BriceñoCabona, L.L.CabonaCOSENTINO, RosarioRosarioCOSENTINODAMASSO, MarioMarioDAMASSOFiorenzano, A.A.FiorenzanoFong, W.W.FongGoeke, B.B.GoekeHesse, K. M.K. M.HesseKostov, V. B.V. B.KostovLANZA, Antonino FrancescoAntonino FrancescoLANZALatham, D. W.D. W.LathamLaw, N.N.LawMancini, L.L.ManciniMAGGIO, AntonioAntonioMAGGIOMOLINARO, MarcoMarcoMOLINAROMann, A. W.A. W.MannMantovan, G.G.MantovanNaponiello, L.L.NaponielloNardiello, D.D.NardielloNASCIMBENI, VALERIOVALERIONASCIMBENIPAGANO, IsabellaIsabellaPAGANOPedani, M.M.PedaniSafonov, B. S.B. S.SafonovSCANDARIATO, GAETANOGAETANOSCANDARIATOSeager, S.S.SeagerSINGH, VIKASHVIKASHSINGHSOZZETTI, AlessandroAlessandroSOZZETTIStrakhov, I. A.I. A.StrakhovWinn, J. N.J. N.WinnZiegler, C.C.ZieglerZingales, T.T.Zingales2024-09-232024-09-2320240004-6361http://hdl.handle.net/20.500.12386/35312Aims: We report the confirmation of a new transiting exoplanet orbiting the star TOI-5076. <BR /> Methods: We present our vetting procedure and follow-up observations which led to the confirmation of the exoplanet TOI-5076b. In particular, we employed high-precision TESS photometry, high-angular-resolution imaging from several telescopes, and high-precision radial velocities from HARPS-N. <BR /> Results: From the HARPS-N spectroscopy, we determined the spectroscopic parameters of the host star: T<SUB>eff</SUB> = (5070±143) K, log 𝑔 = (4.6±0.3), [Fe/H] = (+0.20±0.08), and [α/Fe] = 0.05±0.06. The transiting planet is a warm sub-Neptune with a mass m<SUB>p</SUB> = (16±2) M<SUB>⊙</SUB>, a radius r<SUB>p</SUB> =(3.2±0.l) R<SUB>⊙</SUB> yielding a density ρ<SUB>p</SUB> = (2.8±0.5) g cm<SUP>−3</SUP>. It revolves around its star approximately every 23.445 days. <BR /> Conclusions: The host star is a metal-rich, K2V dwarf, located at about 82 pc from the Sun with a radius of R<SUB>⋆</SUB> = (0.78±0.01) R<SUB>⊙</SUB> and a mass of M<SUB>⋆</SUB> = (0.80±0.07) M<SUB>⊙</SUB>. It forms a common proper motion pair with an M-dwarf companion star located at a projected separation of 2178 au. The chemical analysis of the host-star and the Galactic-space velocities indicate that TOI-5076 belongs to the old population of thin-to-thick-disk transition stars. The density of TOI-5076b suggests the presence of a large fraction by volume of volatiles overlying a massive core. We found that a circular orbit solution is marginally favored with respect to an eccentric orbit solution for TOI-5076b. <P />Full Tables 2 and 3 are available at the CDS via anonymous ftp to <A href="https://cdsarc.cds.unistra.fr/">cdsarc.cds.unistra.fr</A> (ftp://130.79.128.5) or via <A href="https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/687/A226">https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/687/A226</A>STAMPAenArticle10.1051/0004-6361/202349082https://www.aanda.org/articles/aa/full_html/2024/07/aa49082-23/aa49082-23.html2024A&A...687A.226MFIS/05 - ASTRONOMIA E ASTROFISICA