MOA-2013-BLG-220Lb: Planetary Companion to a Possible Brown Dwarf Host

J.C. Yee, C. Han, A. Gould, J. Skowron, I.A. Bond, A. Udalski, M. Hundertmark, L.A.G. Monard, I. Porritt, P. Nelson, V. Bozza, M.D. Albrow, J.-Y. Choi, G.W. Christie, D.L. DePoy, B.S. Gaudi, K.-H. Hwang, Y.K. Jung, C.-U. Lee, J. McCormick, T. Natusch, H. Ngan, H. Park, R.W. Pogge, I.-G. Shin, T.-G. Tan, F. Abe, D.P. Bennett, I.A. Bond, C.S. Botzler, M. Freeman, A. Fukui, D. Fukunaga, Y. Itow, N. Koshimoto, P. Larsen, C.H. Ling, K. Masuda, Y. Matsubara, Y. Muraki, S. Namba, K. Ohnishi, L. Philpott, N.J. Rattenbury, To. Saito, D.J. Sullivan, T. Sumi, W.L. Sweatman, D. Suzuki, P.J. Tristram, N. Tsurumi, K. Wada, N. Yamai, P.C.M. Yock, A. Yonehara, M.K. Szymaski, K. Ulaczyk, S. Kozowski, R. Poleski, . Wyrzykowski, M. Kubiak, P. Pietrukowicz, G. Pietrzyski, I. Soszyski, et al. (9 additional authors not shown) You must enabled JavaScript to view entire author list.

(Submitted on 10 Mar 2014)

Based on its high proper motion $\mu=12.5\pm 1\,\masyr$, MOA-2013-BLG-220Lb is the best candidate to date for a microlensing planet with a verifiable brown dwarf host. This candidacy can be partially tested immediately and more fully tested by 2021, when the source and lens will have separated sufficiently to be resolved in high-resolution images even if the lens is at the bottom of the main sequence, and so extremely faint,

H24. The planet-star mass ratio is

q=3.01+/-0.02103. The planet could have been detected and characterized purely with follow-up data. The potential to completely characterize planetary events from followup data has far-reaching implications for microlensing surveys, both current and into the LSST era.

Comments: 2 tables, 2 figures

Subjects: Earth and Planetary Astrophysics (astro-ph.EP)

Cite as: arXiv:1403.2134 [astro-ph.EP] (or arXiv:1403.2134v1 [astro-ph.EP] for this version)

Submission history

From: Cheongho Han 

[v1] Mon, 10 Mar 2014 03:24:09 GMT (168kb)