{"paper":{"title":"MOA-2010-BLG-328Lb: a sub-Neptune orbiting very late M dwarf ?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"A.A.Cole, A.Cassan, A.Fukui, A.Gould, A.Udalski, A.Williams, B.G. Park, B.S.Gaudi, B.Shappee, C.B.Henderson, C.Black, C.Coutures, C.Han, C.H.Ling, C.Liebig, C.S.Bennett, C.S.Botzler, C.Snodgrass, C.-U.Lee, D.Dominis Prester, D.J.Sullivan, D.Kubas, D.L.DePoy, D.M.Bramich, D.Moorhouse, D.P.Bennett, D.Ricci, D.Suzuki, D.Wouters, E.Bachelet, E.Corrales, E.Kerins, E.Ofek, F.Abe, F.Finet, F.Schonebeck, G.Pietrzynski, G.Scarpetta, G.Thornley, G.W.Christie, H.Park, I.A.Bond, I.A.Steele, I.-G.Shin, I.Soszynski, J.A.R.Caldwell, J.-B.Marquette, J.C.Yee, J.Donatowicz, J.Drummond, J.Greenhill, J.McCormick, J.-P.Beaulieu, J.Skowron, J.Southworth, J.Surdej, J.van Saders, J.Wambsganss, J.W.Menzies, J.Y.Choi, K.A.Alsubai, K.C.Sahu, K.Furusawa, K.Harpsoe, K.Horne, K.Masuda, K.Ohnishi, K.Ulaczyk, K.Wada, L.Mancini, L.-W.Hung, L.Wyrzykowski, M.D.Albrow, M.Dominik, M.Freeman, M.Hundertmark, M.J.Burgdorf, M.K.Szymanski, M.Kubiak, M.Mathiasen, M.Nola, M.T.Penny, M.Zub, N.J.Rattenbury, N.Kains, N.Miyake, P.Browne, P.Chote, P.C.M.Yock, P.Dodds, P.Fouque, P.Harris, P.J.Tristram, R.A.Street, R.Bowens-Rubin, R.Martin, R.Poleski, R.W.Pogge, R.Zellem, S.Brillant, S.Calchi Novati, S.Dieters, S.Dong, S.Hardis, S.Proft, S.Rahvar, S.Schafer, T.C.Hinse, T.G.Beatty, T.Gerner, T.Natusch, To.Saito, T.Sumi, U.G.Jorgensen, V.Batista, V.Bozza, W.L.Sweatman, Y.Itow, Y.-K.Jung, Y.Matsubara, Y.Muraki, Y.Tsapras","submitted_at":"2013-09-30T03:28:38Z","abstract_excerpt":"We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of Mh = 0.11+/-0.01 M_{sun} and Mp = 9.2+/-2.2M_Earth, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at DL = 0.81 +/- 0.10 kpc with projected separation r = 0.92 +/- 0.16 AU. Because of the host's a-priori-unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1309.7714","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}