* Astronomy

Title: OGLE-2011-BLG-0265Lb: a Jovian Microlensing Planet Orbiting an M Dwarf
Author: J. Skowron, I.-G. Shin, A. Udalski, C. Han, T. Sumi, Y. Shvartzvald, A. Gould, D. Dominis-Prester, R. A. Street, U. G. Jørgensen, D. P. Bennett, V. Bozza, M. K. Szymanski, M. Kubiak, G. Pietrzynski, I. Soszynski, R. Poleski, S. Kozlowski, P. Pietrukowicz, K. Ulaczyk, L. Wyrzykowski, F. Abe, A. Bhattacharya, I. A. Bond, C. S. Botzler, M. Freeman, A. Fukui, D. Fukunaga, Y. Itow, C. H. Ling, N. Koshimoto, K. Masuda, Y. Matsubara, Y. Muraki, S. Namba, K. Ohnishi, L. C. Philpott, N. Rattenbury, T. Saito, D. J. Sullivan, D. Suzuki, P. J. Tristram, P. C. M. Yock, D. Maoz, S. Kaspi, M. Friedman, L. A. Almeida, V. Batista, G. Christie, J.-Y. Choi, D. L. DePoy, B. S. Gaudi, C. Henderson, K.-H. Hwang, F. Jablonski, Y. K. Jung, C.-U. Lee, J. McCormick, T. Natusch, H. Ngan, et al. (64 additional authors not shown)

We report the discovery of a Jupiter-mass planet orbiting an M-dwarf star that gave rise to the microlensing event OGLE-2011-BLG-0265. Such a system is very rare among known planetary systems and thus the discovery is important for theoretical studies of planetary formation and evolution. High-cadence temporal coverage of the planetary signal combined with extended observations throughout the event allows us to accurately model the observed light curve. The final microlensing solution remains, however, degenerate yielding two possible configurations of the planet and the host star. In the case of the preferred solution, the mass of the planet is M_p = 1.0 ± 0.3 M_J, and the planet is orbiting a star with a mass M = 0.23 ± 0.07 solar masses. The second possible configuration (2\sigma away) consists of a planet with M_p = 0.6 ± 0.2 M_J and host star with M = 0.15 ± 0.06 solar masses. The system is located in the Galactic disk 3-4 kpc towards the Galactic bulge. In both cases, with an orbit size of 2 AU, the planet is a "cold Jupiter" -- located well beyond the "snow line" of the host star. Currently available data make the secure selection of the correct solution difficult, but there are prospects for lifting the degeneracy with additional follow-up observations in the future, when the lens and source star separate.

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