Bianchi, E.E.BianchiChandler, C. J.C. J.ChandlerCeccarelli, C.C.CeccarelliCODELLA, CLAUDIOCLAUDIOCODELLASakai, N.N.SakaiLópez-Sepulcre, A.A.López-SepulcreMaud, L. T.L. T.MaudMoellenbrock, G.G.MoellenbrockSvoboda, B.B.SvobodaWatanabe, Y.Y.WatanabeSakai, T.T.SakaiMénard, F.F.MénardAikawa, Y.Y.AikawaAlves, F.F.AlvesBalucani, N.N.BalucaniBouvier, M.M.BouvierCaselli, P.P.CaselliCaux, E.E.CauxCharnley, S.S.CharnleyChoudhury, S.S.ChoudhuryDe Simone, M.M.De SimoneDulieu, F.F.DulieuDurán, A.A.DuránEvans, L.L.EvansFavre, C.C.FavreFEDELE , DAVIDEDAVIDEFEDELEFeng, S.S.FengFONTANI, FRANCESCOFRANCESCOFONTANIFrancis, L.L.FrancisHama, T.T.HamaHanawa, T.T.HanawaHerbst, E.E.HerbstHirota, T.T.HirotaImai, M.M.ImaiIsella, A.A.IsellaJiménez-Serra, I.I.Jiménez-SerraJohnstone, D.D.JohnstoneKahane, C.C.KahaneLefloch, B.B.LeflochLoinard, L.L.LoinardMaureira, M. J.M. J.MaureiraMERCIMEK, SEYMASEYMAMERCIMEKMiotello, A.A.MiotelloMori, S.S.MoriNakatani, R.R.NakataniNomura, H.H.NomuraOba, Y.Y.ObaOhashi, S.S.OhashiOkoda, Y.Y.OkodaOspina-Zamudio, J.J.Ospina-ZamudioOya, Y.Y.OyaPineda, J.J.PinedaPODIO, LINDALINDAPODIORimola, A.A.RimolaCox, D. SeguraD. SeguraCoxShirley, Y.Y.ShirleyTAQUET, VIANNEY DANIEL FRANCOISVIANNEY DANIEL FRANCOISTAQUETTESTI, LeonardoLeonardoTESTIVastel, C.C.VastelViti, S.S.VitiWatanabe, N.N.WatanabeWitzel, A.A.WitzelXue, C.C.XueZhang, Y.Y.ZhangZhao, B.B.ZhaoYamamoto, S.S.Yamamoto2021-12-272021-12-2720201745-3925http://hdl.handle.net/20.500.12386/31252The study of hot corinos in Solar-like protostars has been so far mostly limited to the Class 0 phase, hampering our understanding of their origin and evolution. In addition, recent evidence suggests that planet formation starts already during Class I phase, which, therefore, represents a crucial step in the future planetary system chemical composition. Hence, the study of hot corinos in Class I protostars has become of paramount importance. Here we report the discovery of a hot corino towards the prototypical Class I protostar L1551 IRS5, obtained within the ALMA Large Program FAUST. We detected several lines from methanol and its isopotologues (<SUP>13</SUP>CH<SUB>3</SUB>OH and CH<SUB>2</SUB>DOH), methyl formate and ethanol. Lines are bright toward the north component of the IRS5 binary system, and a possible second hot corino may be associated with the south component. The methanol lines non-LTE analysis constrains the gas temperature (˜100 K), density (≥1.5 × 10<SUP>8</SUP> cm<SUP>-3</SUP>), and emitting size (˜10 au in radius). All CH<SUB>3</SUB>OH and <SUP>13</SUP>CH<SUB>3</SUB>OH lines are optically thick, preventing a reliable measure of the deuteration. The methyl formate and ethanol relative abundances are compatible with those measured in Class 0 hot corinos. Thus, based on the present work, little chemical evolution from Class 0 to I hot corinos occurs.STAMPAenArticle10.1093/mnrasl/slaa1302-s2.0-85096870166WOS:000587744400018https://academic.oup.com/mnrasl/article-abstract/498/1/L87/5874261?redirectedFrom=fulltexthttp://arxiv.org/abs/2007.10275v12020MNRAS.498L..87BFIS/05 - ASTRONOMIA E ASTROFISICA