TY - JOUR
T1 - A Sub-Saturn Mass Planet, MOA-2009-BLG-319Lb
AU - Miyake..[et al.], N.
AU - Sumi, T.
AU - Dong, S.
AU - Street, R.
AU - Jørgensen, Uffe Gråe
PY - 2011/2/20
Y1 - 2011/2/20
N2 - 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.
AB - 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.
U2 - 10.1088/0004-637X/728/2/120
DO - 10.1088/0004-637X/728/2/120
M3 - Journal article
SN - 0004-637X
VL - 728
SP - 120
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
ER -