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MOA-2010-BLG-328LB: A sub-Neptune orbiting very late M dwarf?


Furusawa, K and Udalski, A and Sumi, T and Bennett, DP and Bond, IA and Gould, A and Jorgensen, UG and Snodgrass, C and Prester, DD and Albrow, MD and Abe, F and Botzler, CS and Chote, P and Freeman, M and Fukui, A and Harris, P and Itow, Y and Ling, CH and Masuda, K and Matsubara, Y and Miyake, N and Muraki, Y and Ohnishi, K and Rattenbury, NJ and Saito, T and Sullivan, DJ and Suzuki, D and Sweatman, WL and Tristram, PJ and Wada, K and Yock, PCM and Szymanski, MK and Soszynski, I and Kubiak, M and Poleski, R and Ulaczyk, K and Pietrzynski, G and Wyrzykowski, A and Choi, J-Y and Christie, GW and DePoy, DL and Dong, S and Drummond, J and Gaudi, BS and Han, C and Hung, L-W and Hwang, K-H and Lee, C-U and McCormick, J and Moorhouse, D and Natusch, T and Nola, M and Ofek, E and Pogge, RW and Shin, I-G and Skowron, J and Thornley, G and Yee, JC and Alsubai, KA and Bozza, V and Browne, P and Burgdorf, MJ and Novati, SC and Dodds, P and Dominik, M and Finet, F and Gerner, T and Hardis, S and Harpsoe, K and Hinse, TC and Hundertmark, M and Kains, N and Kerins, E and Liebig, C and Mancini, L and Mathiasen, M and Penny, MT and Proft, S and Rahvar, S and Ricci, D and Scarpetta, G and Schafer, S and Schonebeck, F and Southworth, J and Surdej, J and Wambsganss, J and Street, RA and Bramich, DM and Steele, IA and Tsapras, Y and Horne, K and Donatowicz, J and Sahu, KC and Bachelet, E and Batista, V and Beatty, TG and Beaulieu, J-P and Bennett, CS and Black, C and Bowens-Rubin, R and Brillant, S and Caldwell, JAR and Cassan, A and Cole, AA and Corrales, E and Coutures, C and Dieters, S and Fouque, P and Greenhill, J and Henderson, CB and Kubas, D and Marquette, J-B and Martin, R and Menzies, JW and Shappee, B and Williams, A and Wouters, D and van Saders, J and Zellem, R and Zub, M, MOA-2010-BLG-328LB: A sub-Neptune orbiting very late M dwarf?, Astrophysical Journal, 779, (2) Article 91. ISSN 0004-637X (2013) [Refereed Article]

Copyright Statement

Copyright 2013 The American Astronomical Society

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


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.

Item Details

Item Type:Refereed Article
Keywords:gravitational lensing: micro; planetary systems
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Galactic astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Black, C (Ms Christine Black)
UTAS Author:Cole, AA (Associate Professor Andrew Cole)
UTAS Author:Dieters, S (Dr Stefan Dieters)
UTAS Author:Greenhill, J (Dr John Greenhill)
ID Code:88678
Year Published:2013
Web of Science® Times Cited:17
Deposited By:Mathematics and Physics
Deposited On:2014-02-12
Last Modified:2017-11-01

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