Two cold , gas giant planets orbiting a G-type main sequence star in the galactic disk have previously been discovered in the high magnification microlensing event OGLE-2012-BLG-0026 ( ) .
Here we present revised host star flux measurements and a refined model for the two-planet system using additional light curve data .
We performed high angular resolution adaptive optics imaging with the Keck and Subaru telescopes at two epochs while the source star was still amplified .
We detected the lens flux , H = 16.39 \pm 0.08 .
The lens , a disk star , is brighter than predicted from the modeling in the original study .
We revisited the light curve modeling using additional photometric data from the B & C telescope in New Zealand and CTIO 1.3m H band light curve .
We then include the Keck and Subaru adaptive optic observation constraints .
The system is composed of a \sim 4 - 9 Gyr lens star of M _ { lens } = 1.06 \pm 0.05 ~ { } M _ { \odot } at a distance of D _ { lens } = 4.0 \pm 0.3 ~ { } kpc , orbited by two giant planets of 0.145 \pm 0.008 M _ { Jup } and 0.86 \pm 0.06 ~ { } M _ { Jup } with projected separations of 4.0 \pm 0.5 AU and 4.8 \pm 0.7 AU respectively .
Since the lens is brighter than the source star by 16 \pm 8 \% in H , with no other blend within one arcsec , it will be possible to estimate its metallicity by subsequent IR spectroscopy with 8–10Â m class telescopes .
By adding a constraint on the metallicity it will be possible to refine the age of the system .