MOA-2010-BLG-328Lb: a sub-Neptune orbiting very Late M dwarf?

K. Furusawa, A. Udalski, T. Sumi, D. P. Bennett, I. A. Bond, A. Gould, U. G. Jørgensen, C. Snodgrass, D. Dominis Prester, M. D. Albrow, F. Abe, C. S. Botzler, P. Chote, M. Freeman, A. Fukui, P. Harris, Y. Itow, C. H. Ling, K. Masuda, Y. MatsubaraN. Miyake, Y. Muraki, K. Ohnishi, N. J. Rattenbury, To. Saito, D. J. Sullivan, D. Suzuki, W. L. Sweatman, P. J. Tristram, K. Wada, P. C. M. Yock, M. K. Szymański, I. Soszyński, M. Kubiak, R. Poleski, K. Ulaczyk, G. Pietrzyński, Ł. Wyrzykowski, J.-Y. Choi, G. W. Christie, D. L. DePoy, Subo Dong, J. Drummond, B. S. Gaudi, C. Han, L.-W. Hung, K.-H. Hwang, C.-U. Lee, J. McCormick, D. Moorhouse, T. Natusch, M. Nola, E. Ofek, R. W. Pogge, I.-G. Shin, J. Skowron, G. Thornley, J. C. Yee, K. A. Alsubai, V. Bozza, P. Browne, M. J. Burgdorf, S. Calchi Novati, P. Dodds, M. Dominik, F. Finet, T. Gerner, S. Hardis, K. Harpsøe, T. C. Hinse, M. Hundertmark, Noé Kains, E. Kerins, C. Liebig, L. Mancini, M. Mathiasen, M. T. Penny, S. Proft, S. Rahvar, D. Ricci, G. Scarpetta, S. Schäfer, F. Schönebeck, J. Southworth, J. Surdej, J. Wambsganss, R. A. Street, D. M. Bramich, I. A. Steele, Y. Tsapras, K. Horne, J. Donatowicz, K. C. Sahu, E. Bachelet, V. Batista, T. G. Beatty, J.-P. Beaulieu, C. S. Bennett, C. Black, R. Bowens-Rubin, S. Brillant, J. A. R. Caldwell, A. Cassan, A. A. Cole, E. Corrales, C. Coutures, S. Dieters, P. Fouqué, J. Greenhill, C. B. Henderson, D. Kubas, J.-B. Marquette, R. Martin, J. W. Menzies, B. Shappee, A. Williams, D. Wouters, J. van Saders, R. Zellem, M. Zub

Research output: Contribution to journalArticlepeer-review

22 Citations (Scopus)


We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of M h = 0.11 ± 0.01 M and M p = 9.2 ± 2.2 M , corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at D L = 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 is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions.

Original languageEnglish
Article number91
Number of pages12
JournalAstrophysical Journal
Issue number2
Early online date26 Nov 2013
Publication statusPublished - 20 Dec 2013


  • Gravitational lensing: micro
  • Planetary systems


Dive into the research topics of 'MOA-2010-BLG-328Lb: a sub-Neptune orbiting very Late M dwarf?'. Together they form a unique fingerprint.

Cite this