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

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

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

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

Identifier: http://hdl.handle.net/2292/16617

Issue Date: 2011

Reference: Astrophysical Journal 728(2) 2011

Rights: Copyright: American Astronomical Society

Rights (URI): https://researchspace.auckland.ac.nz/docs/uoa-docs/rights.htm

Abstract:

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 thismicrolensing 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, tE, and angular Einstein radius, θE, along with a standard Galactic model indicates a host star mass of ML = 0.38+0.34 −0.18M and a planet mass of Mp = 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.

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