Bourrier, V.V.BourrierKitzmann, D.D.KitzmannKuntzer, T.T.KuntzerNascimbeni, V.V.NascimbeniLendl, M.M.LendlLavie, B.B.LavieHoeijmakers, H. J.H. J.HoeijmakersPino, LorenzoLorenzoPinoEhrenreich, D.D.EhrenreichHeng, K.K.HengAllart, R.R.AllartCegla, H. M.H. M.CeglaDumusque, X.X.DumusqueMelo, C.C.MeloAstudillo-Defru, N.N.Astudillo-DefruCaldwell, D. A.D. A.CaldwellCretignier, M.M.CretignierGiles, H.H.GilesHenze, C. E.C. E.HenzeJenkins, J.J.JenkinsLovis, C.C.LovisMurgas, F.F.MurgasPepe, F.F.PepeRicker, G. R.G. R.RickerRose, M. E.M. E.RoseSeager, S.S.SeagerSegransan, D.D.SegransanSuárez-Mascareño, A.A.Suárez-MascareñoUdry, S.S.UdryVanderspek, R.R.VanderspekWyttenbach, A.A.Wyttenbach2022-04-012022-04-0120200004-6361http://hdl.handle.net/20.500.12386/32073We present the analysis of TESS optical photometry of WASP-121b, which reveals the phase curve of this transiting ultra-hot Jupiter. Its hotspot is located at the sub-stellar point, showing inefficient heat transport from the dayside (2870 ± 50 K) to the nightside (<2500 K at 3σ) at the altitudes probed by TESS. The TESS eclipse depth, measured at the shortest wavelength to date for WASP-121b, confirms the strong deviation from blackbody planetary emission. Our atmospheric retrieval on the complete emission spectrum supports the presence of a temperature inversion, which can be explained by the presence of VO and possibly TiO and FeH. The strong planetary emission at short wavelengths could arise from an H<SUP>-</SUP> continuum. <P />The reduced light curve of WASP-121, phase-folded at the planet orbital period and binned (Fig. 2) is available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/637/A36">http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/637/A36</A>STAMPAenArticle10.1051/0004-6361/201936647https://www.aanda.org/articles/aa/full_html/2020/05/aa36647-19/aa36647-19.html2020A&A...637A..36BFIS/05 - ASTRONOMIA E ASTROFISICA