A sub-Saturn Mass Planet, MOA-2009-BLG-319Lb
Miyake, N. · Sumi, T. · Dong, Subo · Street, R. · Mancini, L. · Gould, A. · Bennett, D. P. · Tsapras, Y. · Yee, J. C. · Albrow, M. D. · Bond, I. A. · Fouque, P. · Browne, P. · Han, C. · Snodgrass, C. · Finet, F. · Furusawa, K. · Harpsoe, K. · Allen, W. · Hundertmark, M. · Freeman, M. · Suzuki, D. · Abe, F. · Botzler, C. S. · Douchin, D. · Fukui, A. · Hayashi, F. · Hearnshaw, J. B. · Hosaka, S. · Itow, Y. · Kamiya, K. · Kilmartin, P. M. · Korpela, A. · Lin, W. · Ling, C. H. · Makita, S. · Masuda, K. · Matsubara, Y. · Muraki, Y. · Nagayama, T. · Nishimoto, K. · Ohnishi, K. · Perrott, Y. C. · Rattenbury, N. · Saito, To. · Skuljan, L. · Sullivan, D. J. · Sweatman, W. L. · Tristram, P. J. · Wada, K. · Yock, P. C. M. · Collaboration, The MOA · Bolt, G. · Bos, M. · Christie, G. W. · DePoy, D. L. · Drummond, J. · Gal-Yam, A. · Gaudi, B. S. · Gorbikov, E. · Higgins, D. · Janczak, K. -H. Hwang J. · Kaspi, S. · Lee, C. -U. · Koo, J. -R. · lowski, S. Koz · Lee, Y. · Mallia, F. · Maury, A. · Maoz, D. · McCormick, J. · Monard, L. A. G. · Moorhouse, D. · Mu~noz, J. A. · Natusch, T. · Ofek, E. O. · Pogge, R. W. · Polishook, D. · Santallo, R. · Shporer, A. · Spector, O. · Thornley, G. · Collaboration, The Micro FUN · Allan, A. · Bramich, D. M. · Horne, K. · Kains, N. · Steele, I. · Collaboration, The RoboNet · Bozza, V. · Burgdorf, M. J. · Novati, S. Calchi · Dominik, M. · Dreizler, S. · Glitrup, M. · Hessman, F. V. · Hinse, T. C. · Jorgensen, U. G. · Liebig, C. · Maier, G. · Mathiasen, M. · Rahvar, S. · Ricci, D. · Scarpetta, G. · Skottfelt, J. · Southworth, J. · Surdej, J. · Wambsganss, J. · Zimmer, F. · Consortium, The MiNDSTEp · Batista, V. · Beaulieu, J. P. · Brillant, S. · Cassan, A. · Cole, A. · Corrales, E. · Coutures, Ch. · Dieters, S. · Greenhill, J. · Kubas, D. · Menzies, J. · Collaboration, The PLANET
الأصل · EN
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 hours 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) x 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, tₑ, and angular Einstein radius, θₑ, along with a standard Galactic model indicates a host star mass of Mₗ = 0.38⁺⁰.³⁴₋₀.₁₈ MSun and a planet mass of Mₚ = 50⁺⁴⁴₋₂₄ MEarth, 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.
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