* Astronomy

Title: MOA-2013-BLG-220Lb: Planetary Companion to a Possible Brown Dwarf Host
Author: 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. Szymanski, K. Ulaczyk, S. Kozlowski, R. Poleski, L. Wyrzykowski, M. Kubiak, P. Pietrukowicz, G. Pietrzynski, I. Soszynski, et al. (9 additional authors not shown)

Based on its high proper motion \mu=12.5± 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, H~24. The planet-star mass ratio is q=3.01±0.02 x 10^-3. 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.

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