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Calitz, I.A. Bond, I. Soszy, I. Steele, J.A.R. Caldwell, J.B. Hearnshaw, J.B. Marquette, J. Donatowicz, J. Greenhill, J. Janczak, J. McCormick, J. Menzies, J. Wambsganss, K. Cook, K.C. Sahu, K. Furusawa, K. Hill, K. Horne, K. Kamiya, K. Masuda, K. Ohnishi, K.R. Pollard, K. Ulaczyk, L. Skuljan, M. Bode, M.D. Albrow, M. Dominik, M.F. Duran, M. Hoffman, M.J. Burgdorf, M. Kubiak, M. Nagaya, M. Zub, N. Kains, N. Miyake, N. Rattenbury, O. Pejcha, O. Szewczyk, P., P.C.M. Yock, P. Fouqu\\'e, P. Meintjes, P.M. Kilmartin, P. Rojo, R. Martin, R. Santallo, R. Street, R.W. Pogge, S. Brillant, S. Dieters, S. Dong, S. Kane, The microFUN Collaboration: W. Allen, The MOA Collaboration: F. Abe, The OGLE Collaboration: M.K. Szyma, The PLANET Collaboration: J.P. Beaulieu, T. Nagayama, T. Natusch, T. Okumura, To. Saito, T. Sako, T. Sumi, U.G. J, U. Marboeuf, V. Batista, W. Lin, W.L. Sweatman, Y.C. Perrott, Y. Itow, Y. Matsubara, Y. Muraki, Y. Tsapras","submitted_at":"2009-12-07T08:16:06Z","abstract_excerpt":"We present the discovery of a Neptune-mass planet OGLE-2007-BLG-368Lb with a planet-star mass ratio of q=[9.5 +/- 2.1] x 10^{-5} via gravitational microlensing. The planetary deviation was detected in real-time thanks to the high cadence of the MOA survey, real-time light curve monitoring and intensive follow-up observations. A Bayesian analysis returns the stellar mass and distance at M_l = 0.64_{-0.26}^{+0.21} M_\\sun and D_l = 5.9_{-1.4}^{+0.9} kpc, respectively, so the mass and separation of the planet are M_p = 20_{-8}^{+7} M_\\oplus and a = 3.3_{-0.8}^{+1.4} AU, respectively. 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Cassan, A. Cole, A. Fukui, A. Gould, A. Korpela, A. Udalski, A. Williams, B.-G. Park, B. Macintosh, B. Monard, B.S. Gaudi, C. Han, Ch. Coutures, C.H. Ling, C.S. Botzler, C. Snodgrass, C.-U. Lee, D. Dominis Prester, D.J. Sullivan, D. Kubas, D.L. Depoy, D.M. Bramich, D.P. Bennett, E. Corrales, E. Martioli, E. Pedretti, F. Jablonski, F. Mallia, G. Pietrzy, G.W. Christie, H. Calitz, I.A. Bond, I. Soszy, I. Steele, J.A.R. Caldwell, J.B. Hearnshaw, J.B. Marquette, J. Donatowicz, J. Greenhill, J. Janczak, J. McCormick, J. Menzies, J. Wambsganss, K. Cook, K.C. Sahu, K. Furusawa, K. Hill, K. Horne, K. Kamiya, K. Masuda, K. Ohnishi, K.R. Pollard, K. Ulaczyk, L. Skuljan, M. Bode, M.D. Albrow, M. Dominik, M.F. Duran, M. Hoffman, M.J. Burgdorf, M. Kubiak, M. Nagaya, M. Zub, N. Kains, N. Miyake, N. Rattenbury, O. Pejcha, O. Szewczyk, P., P.C.M. Yock, P. Fouqu\\'e, P. Meintjes, P.M. Kilmartin, P. Rojo, R. Martin, R. Santallo, R. Street, R.W. Pogge, S. Brillant, S. Dieters, S. Dong, S. Kane, The microFUN Collaboration: W. Allen, The MOA Collaboration: F. Abe, The OGLE Collaboration: M.K. Szyma, The PLANET Collaboration: J.P. Beaulieu, T. Nagayama, T. Natusch, T. Okumura, To. Saito, T. Sako, T. Sumi, U.G. J, U. Marboeuf, V. Batista, W. Lin, W.L. Sweatman, Y.C. Perrott, Y. Itow, Y. Matsubara, Y. Muraki, Y. Tsapras","submitted_at":"2009-12-07T08:16:06Z","abstract_excerpt":"We present the discovery of a Neptune-mass planet OGLE-2007-BLG-368Lb with a planet-star mass ratio of q=[9.5 +/- 2.1] x 10^{-5} via gravitational microlensing. The planetary deviation was detected in real-time thanks to the high cadence of the MOA survey, real-time light curve monitoring and intensive follow-up observations. A Bayesian analysis returns the stellar mass and distance at M_l = 0.64_{-0.26}^{+0.21} M_\\sun and D_l = 5.9_{-1.4}^{+0.9} kpc, respectively, so the mass and separation of the planet are M_p = 20_{-8}^{+7} M_\\oplus and a = 3.3_{-0.8}^{+1.4} AU, respectively. 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