Olmschenk GBennett DPBond IAZang WJung YKYee JCBachelet EAbe FBarry RKBhattacharya AFujii HFukui AHirao YSilva SIItow YKirikawa RKondo IKoshimoto NMatsubara YMatsumoto SMiyazaki SMunford BMuraki YOkamura ARanc CRattenbury NJSatoh YSumi TSuzuki DToda TTristram PJVandorou AYama HAlbrow MDCha S-MChung S-JGould AHan CHwang K-HKim D-JKim H-WKim S-LLee C-ULee D-JLee YPark B-GPogge RWRyu Y-HShin I-GShvartzvald YChristie GCooper TDrummond JGreen JHennerley SMcCormick JMonard LAGNatusch TPorritt ITan T-GMao SMaoz DPenny MTZhu WBozza VCassan ADominik MHundertmark MJaimes RFKruszyńska KRybicki KAStreet RATsapras YWambsganss JWyrzykowski LZieliński PRau G2024-05-142024-05-142023-03Olmschenk G, Bennett DP, Bond IA, Zang W, Jung YK, Yee JC, Bachelet E, Abe F, Barry RK, Bhattacharya A, Fujii H, Fukui A, Hirao Y, Silva SI, Itow Y, Kirikawa R, Kondo I, Koshimoto N, Matsubara Y, Matsumoto S, Miyazaki S, Munford B, Muraki Y, Okamura A, Ranc C, Rattenbury NJ, Satoh Y, Sumi T, Suzuki D, Toda T, Tristram PJ, Vandorou A, Yama H, Albrow MD, Cha SM, Chung SJ, Gould A, Han C, Hwang KH, Kim DJ, Kim HW, Kim SL, Lee CU, Lee DJ, Lee Y, Park BG, Pogge RW, Ryu YH, Shin IG, Shvartzvald Y, Christie G, Cooper T, Drummond J, Green J, Hennerley S, McCormick J, Monard LAG, Natusch T, Porritt I, Tan TG, Mao S, Maoz D, Penny MT, Zhu W, Bozza V, Cassan A, Dominik M, Hundertmark M, Jaimes RF, Kruszyńska K, Rybicki KA, Street RA, Tsapras Y, Wambsganss J, Wyrzykowski , Zieliński P, Rau G. (2023). MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert. Astronomical Journal. 165. 4.0004-6256https://mro.massey.ac.nz/handle/10179/69553We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio q=3.17-0.26+0.28×10-4, the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass mplanet=46-24+42M⊕ and a host star of mass Mhost=0.43-0.23+0.39M⊙, located at a distance DL=7.49-1.13+0.99kpc . For the second scenario, we estimate mplanet=69-34+37M⊕, Mhost=0.66-0.32+0.35M⊙, and DL=7.81-0.93+0.93kpc . The planet has a projected separation as a fraction of the Einstein ring radius s=1.3807-0.0018+0.0018 . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models(c) 2023 The Author/sCC BY 4.0https://creativecommons.org/licenses/by/4.0/Binary Lens microlensingGravitational MicrolensingGravitational Microlensing exoplanet detectionJournal article10.3847/1538-3881/acbcc81538-3881journal-article175