학술논문
MOA-2010-BLG-328Lb: a sub-Neptune orbiting very late M dwarf ?
Document Type
Working Paper
Author
Furusawa, K.; Udalski, A.; Sumi, T.; Bennett, D. P.; Bond, I. A.; Gould, A.; Jorgensen, U. G.; Snodgrass, C.; Prester, D. Dominis; 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.; Szymanski, M. K.; Soszynski, I.; Kubiak, M.; Poleski, R.; Ulaczyk, K.; Pietrzynski, G.; Wyrzykowski, L.; Choi, J. Y.; Christie, G. W.; DePoy, D. L.; Dong, S.; Drummond, J.; Gaudi, B. S.; Han, C.; Hung, L. -W.; Jung, Y. -K.; Lee, C. -U.; McCormick, J.; Moorhouse, D.; Natusch, T.; Nola, M.; Ofek, E.; Park, B. G.; Park, H.; Pogge, R. W.; Shin, I. -G.; Skowron, J.; Thornley, G.; Yee, J. C.; Alsubai, K. A.; Bozza, V.; Browne, P.; Burgdorf, M. J.; Novati, S. Calchi; Dodds, P.; Dominik, M.; Finet, F.; Gerner, T.; Hardis, S.; Harpsoe, 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.; Schafer, S.; Schonebeck, 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.; Fouque, 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.; Zub, M.
Source
Subject
Language
Abstract
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 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.
Comment: 30 pages, 6 figures. accepted for publication in ApJ. Figure 1 and 2 are updated
Comment: 30 pages, 6 figures. accepted for publication in ApJ. Figure 1 and 2 are updated