Trifonov, TrifonTrifonTrifonovBrahm, RafaelRafaelBrahmEspinoza, NestorNestorEspinozaHenning, ThomasThomasHenningJordan, AndresAndresJordanNesvorny, DavidDavidNesvornyDawson, Rebekah I.Rebekah I.DawsonLissauer, Jack J.Jack J.LissauerLee, Man HoiMan HoiLeeKossakowski, DianaDianaKossakowskiRojas, Felipe I.Felipe I.RojasHobson, Melissa J.Melissa J.HobsonSarkis, PaulaPaulaSarkisSchlecker, MartinMartinSchleckerBitsch, BertramBertramBitschBakos, Gaspar A.Gaspar A.BakosBarbieri, MauroMauroBarbieriBhatti, W.W.BhattiButler, R. PaulR. PaulButlerCrane, Jeffrey D.Jeffrey D.CraneNandakumar, SangeethaSangeethaNandakumarDiaz, Matias R.Matias R.DiazShectman, StephenStephenShectmanTeske, JohannaJohannaTeskeTorres, PascalPascalTorresSuc, VincentVincentSucVines, Jose I.Jose I.VinesWang, Sharon X.Sharon X.WangRicker, George R.George R.RickerShporer, AviAviShporerVanderburg, AndrewAndrewVanderburgDragomir, DianaDianaDragomirVanderspek, RolandRolandVanderspekBurke, Christopher J.Christopher J.BurkeDaylan, TansuTansuDaylanShiao, BernieBernieShiaoJenkins, Jon M.Jon M.JenkinsWohler, BillBillWohlerSeager, SaraSaraSeagerWinn, Joshua N.Joshua N.Winn2025-12-302025-12-3020211538-3881https://hdl.handle.net/20.500.12740/24118TOI-2202 b is a transiting warm Jovian-mass planet with an orbital period of P = 11.91 days identified from the Full Frame Images data of five different sectors of the TESS mission. Ten TESS transits of TOI-2202 b combined with three follow-up light curves obtained with the CHAT robotic telescope show strong transit timing variations (TTVs) with an amplitude of about 1.2 hr. Radial velocity follow-up with FEROS, HARPS, and PFS confirms the planetary nature of the transiting candidate (a (b) = 0.096 +/- 0.001 au, m (b) = 0.98 +/- 0.06 M (Jup)), and a dynamical analysis of RVs, transit data, and TTVs points to an outer Saturn-mass companion (a (c) = 0.155 +/- 0.002 au, m (c) = 0.37 +/- 0.10 M (Jup)) near the 2:1 mean motion resonance. Our stellar modeling indicates that TOI-2202 is an early K-type star with a mass of 0.82 M (circle dot), a radius of 0.79 R (circle dot), and solar-like metallicity. The TOI-2202 system is very interesting because of the two warm Jovian-mass planets near the 2:1 mean motion resonance, which is a rare configuration, and their formation and dynamical evolution are still not well understood.Acceso AbiertoEARTH-SIZED PLANETSUPER-EARTHHOT JUPITERSTESSSYSTEMSTRANSITNEPTUNEMODELPERIODOGRAMSCATTERINGhttp://dx.doi.org/10.3847/1538-3881/ac1bbe