Dreizler, S.S.DreizlerCrossfield, I. J. M.I. J. M.CrossfieldKossakowski, D.D.KossakowskiPlavchan, P.P.PlavchanJeffers, S., VS., VJeffersKemmer, J.J.KemmerLuque, R.R.LuqueEspinoza, N.N.EspinozaPalle, E.E.PalleStassun, K.K.StassunMatthews, E.E.MatthewsCale, B.B.CaleCaballero, J. A.J. A.CaballeroSchlecker, M.M.SchleckerLillo-Box, J.J.Lillo-BoxZechmeister, M.M.ZechmeisterLalitha, S.S.LalithaReiners, A.A.ReinersSoubkiou, A.A.SoubkiouBitsch, B.B.BitschOsorio, M. R. ZapateroM. R. ZapateroOsorioChaturvedi, P.P.ChaturvediHatzes, A. P.A. P.HatzesRicker, G.G.RickerVanderspek, R.R.VanderspekLatham, D. W.D. W.LathamSeager, S.S.SeagerWinn, J.J.WinnJenkins, J. M.J. M.JenkinsAceituno, J.J.AceitunoAmado, P. J.P. J.AmadoBarkaoui, K.K.BarkaouiBarbieri, M.M.BarbieriBatalha, N. M.N. M.BatalhaBauer, F. F.F. F.BauerBenneke, B.B.BennekeBenkhaldoun, Z.Z.BenkhaldounBeichman, C.C.BeichmanBerberian, J.J.BerberianBurt, J.J.BurtButler, R. P.R. P.ButlerCaldwell, D. A.D. A.CaldwellChintada, A.A.ChintadaChontos, A.A.ChontosChristiansen, J. L.J. L.ChristiansenCiardi, D. R.D. R.CiardiCifuentes, C.C.CifuentesCollins, K. A.K. A.CollinsCollins, K., IK., ICollinsCombs, D.D.CombsCortes-Contreras, M.M.Cortes-ContrerasCrane, J. D.J. D.CraneDaylan, T.T.DaylanDragomir, D.D.DragomirEsparza-Borges, E.E.Esparza-BorgesEvans, P.P.EvansFeng, F.F.FengFlowers, E. E.E. E.FlowersFukui, A.A.FukuiFulton, B.B.FultonFurlan, E.E.FurlanGaidos, E.E.GaidosGeneser, C.C.GeneserGiacalone, S.S.GiacaloneGillon, M.M.GillonGonzales, E.E.GonzalesGorjian, VVGorjianHellier, C.C.HellierHidalgo, D.D.HidalgoHoward, A. W.A. W.HowardHowell, S.S.HowellHuber, D.D.HuberIsaacson, H.H.IsaacsonJehin, E.E.JehinJensen, E. L. N.E. L. N.JensenKaminski, A.A.KaminskiKane, S. R.S. R.KaneKawauchi, K.K.KawauchiKielkopf, J. F.J. F.KielkopfKlahr, H.H.KlahrKosiarek, M. R.M. R.KosiarekKreidberg, L.L.KreidbergKurster, M.M.KursterLafarga, M.M.LafargaLivingston, J.J.LivingstonLouie, D.D.LouieMann, A.A.MannMadrigal-Aguado, A.A.Madrigal-AguadoMatson, R. A.R. A.MatsonMocnik, T.T.MocnikMorales, J. C.J. C.MoralesMuirhead, P. S.P. S.MuirheadMurgas, F.F.MurgasNandakumar, S.S.NandakumarNarita, N.N.NaritaNowak, G.G.NowakOshagh, M.M.OshaghParviainen, H.H.ParviainenPassegger, V. M.V. M.PasseggerPollacco, D.D.PollaccoPozuelos, F. J.F. J.PozuelosQuirrenbach, A.A.QuirrenbachReefe, M.M.ReefeRibas, IIRibasRobertson, P.P.RobertsonRodriguez-Lopez, C.C.Rodriguez-LopezRose, M. E.M. E.RoseRoy, A.A.RoySchweitzer, A.A.SchweitzerSchlieder, J.J.SchliederShectman, S.S.ShectmanTanner, A.A.TannerSenavci, H., VH., VSenavciTeske, J.J.TeskeTwicken, J. D.J. D.TwickenVillasenor, J.J.VillasenorWang, S. X.S. X.WangWeiss, L. M.L. M.WeissWittrock, J.J.WittrockYilmaz, M.M.YilmazZohrabi, F.F.Zohrabi2025-12-302025-12-3020201432-0746https://hdl.handle.net/20.500.12740/24171We report the discovery of a Neptune-like planet (LP 714-47 b, P = 4.05204 d, m(b) = 30.8 +/- 1.5M(circle plus), R-b = 4.7 +/- 0.3 R-circle plus) located in the hot Neptune desert. Confirmation of the TESS Object of Interest (TOI 442.01) was achieved with radial-velocity follow-up using CARMENES, ESPRESSO, HIRES, iSHELL, and PFS, as well as from photometric data using TESS, Spitzer, and ground-based photometry from MuSCAT2, TRAPPIST-South, MONET-South, the George Mason University telescope, the Las Cumbres Observatory Global Telescope network, the El Sauce telescope, the TuBTAK National Observatory, the University of Louisville Manner Telescope, and WASP-South. We also present high-spatial resolution adaptive optics imaging with the Gemini Near-Infrared Imager. The low uncertainties in the mass and radius determination place LP 714-47 b among physically well-characterised planets, allowing for a meaningful comparison with planet structure models. The host star LP 714-47 is a slowly rotating early M dwarf (T-eff = 3950 +/- 51 K) with a mass of 0.59 +/- 0.02M(circle dot) and a radius of 0.58 +/- 0.02R(circle dot). From long-term photometric monitoring and spectroscopic activity indicators, we determine a stellar rotation period of about 33 d. The stellar activity is also manifested as correlated noise in the radial-velocity data. In the power spectrum of the radial-velocity data, we detect a second signal with a period of 16 days in addition to the four-day signal of the planet. This could be shown to be a harmonic of the stellar rotation period or the signal of a second planet. It may be possible to tell the difference once more TESS data and radial-velocity data are obtained.Acceso Abiertomethods: data analysisplanetary systemsstars: late-typestars: individual: LP 714-47planets and satellites: individual: LP 714-47 bhttp://dx.doi.org/10.1051/0004-6361/202038016