A sub-Saturn mass planet, MOA-2009-BLG-319Lb

N. Miyake, T. Sumi, Subo Dong, R. Street, L. Mancini, A. Gould, D. P. Bennett, Y. Tsapras, J. C. Yee, M. D. Albrow, I. A. Bond, P. Fouqué, P. Browne, C. Han, C. Snodgrass, F. Finet, K. Furusawa, K. Harpsøe, W. Allen, M. HundertmarkM. Freeman, D. Suzuk, F. Abe, C. S. Botzler, D. Douchin, A. Fukui, F. Hayashi, J. B. Hearnshaw, S. Hosaka, Y. Itow, K. Kamiya, P. M. Kilmartin, A. Korpela, W. Lin, C. H. Ling, S. Makita, K. Masuda, Y. Matsubara, Y. Muraki, T. Nagayama, K. Nishimoto, K. Ohnishi, Y. C. Perrott, N. Rattenbury, To Saito, L. Skuljan, D. J. Sullivan, W. L. Sweatman, P. J. Tristram, K. Wada, P. C.M. Yock, G. Bolt, M. Bos, G. W. Christie, D. L. Depoy, J. Drummond, A. Gal-Yam, B. S. Gaudi, E. Gorbikov, D. Higgins, K. H. Hwang, J. Janczak, S. Kaspi, C. U. Lee, J. R. Koo, S. Kozllowski, Y. Lee, F. Mallia, A. Maury, D. Maoz, J. McCormick, L. A.G. Monard, D. Moorhouse, J. A. Muñoz, T. Natusch, E. O. Ofek, R. W. Pogge, D. Polishook, R. Santallo, A. Shporer, O. Spector, G. Thornley, A. Allan, D. M. Bramich, K. Horne, N. Kains, I. Steele, V. Bozza, M. J. Burgdorf, S. Calchi Novati, M. Dominik, S. Dreizler, M. Glitrup, F. V. Hessman, T. C. Hinse, U. G. Jørgensen, C. Liebig, G. Maier, M. Mathiasen, S. Rahvar, D. Ricci, G. Scarpetta, J. Skottfelt, J. Southworth, J. Surdej, J. Wambsganss, F. Zimmer, V. Batista, J. P. Beaulieu, S. Brillant, A. Cassan, A. Cole, E. Corrales, Ch Coutures, S. Dieters, J. Greenhill, D. Kubas, J. Menzies

Research output: Contribution to journalArticlepeer-review


We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K-or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 ± 0.02) × 10-4 and a separation of d = 0.97537 ± 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t e, and angular Einstein radius, θe, along with a standard Galactic model indicates a host star mass of Ml = 0.38 +0.34-0.18 M and a planet mass of M p = 50+44-24 M>, which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4+1.2-0.6 AU and a distance to the planetary system of Dl = 6.1+1.1-1.2 kpc. This separation is ∼2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.

Original languageEnglish
JournalAstrophysical Journal
Issue number2
StatePublished - 20 Feb 2011


  • Gravitational lensing: micro
  • Planetary systems


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