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

Furusawa, K.; Udalski, A.; Sumi, T.; Bennett, D. P.; Bond, I. A.; Gould, A.; Jørgensen, U. G.; Snodgrass, C.; Dominis Prester, D.; Albrow, M. D.; Abe, F.; Botzler, C. S.; Chote, P.; Freeman, M.; Fukui, A.; Harris, P.; Itow, Y.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Ohnishi, K.; Rattenbury, N. J.; Saito, To.; Sullivan, D. J.; Suzuki, D.; Sweatman, W. L.; Tristram, P. J.; Wada, K.; Yock, P. C. M.; Szymański, M. K.; Soszyński, I.; Kubiak, M.; Poleski, R.; Ulaczyk, K.; Pietrzyński, G.; Wyrzykowski, Ł.; Choi, J.-Y.; Christie, G. W.; DePoy, D. L.; Dong, Subo; Drummond, J.; Gaudi, B. S.; Han, C.; Hung, L.-W.; Hwang, K.-H.; Lee, C.-U.; McCormick, J.; Moorhouse, D.; Natusch, T.; Nola, M.; Ofek, E.; Pogge, R. W.; Shin, I.-G.; Skowron, J.; Thornley, G.; Yee, J. C.; Alsubai, K. A.; Bozza, V.; Browne, P.; Burgdorf, M. J.; Calchi Novati, S.; Dodds, P.; Dominik, M.; Finet, F.; Gerner, T.; Hardis, S.; Harpsøe, K.; Hinse, T. C.; Hundertmark, M.; Kains, N.; Kerins, E.; Liebig, C.; Mancini, L.; Mathiasen, M.; Penny, M. T.; Proft, S.; Rahvar, S.; Ricci, D.; Scarpetta, G.; Schäfer, S.; Schönebeck, F.; Southworth, J.; Surdej, J.; Wambsganss, J.; Street, R. A.; Bramich, D. M.; Steele, I. A.; Tsapras, Y.; Horne, K.; Donatowicz, J.; Sahu, K. C.; Bachelet, E.; Batista, V.; Beatty, T. G.; Beaulieu, J.-P.; Bennett, C. S.; Black, C.; Bowens-Rubin, R.; Brillant, S.; Caldwell, J. A. R.; Cassan, A.; Cole, A. A.; Corrales, E.; Coutures, C.; Dieters, S.; Fouqué, P.; Greenhill, J.; Henderson, C. B.; Kubas, D.; Marquette, J.-B.; Martin, R.; Menzies, J. W.; Shappee, B.; Williams, A.; Wouters, D.; van Saders, J.; Zellem, R. and Zub, M. (2013). MOA-2010-BLG-328Lb: a sub-Neptune orbiting very late M dwarf? Astrophysical Journal, 779(2), article no. 91.

DOI: https://doi.org/10.1088/0004-637X/779/2/91

Abstract

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.

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