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Two cold, gas giant planets orbiting a G-type main sequence star in thegalactic disk have previously been discovered in the high magnificationmicrolensing event OGLE-2012-BLG-0026 (Han et al. 2013). Here we presentrevised host star flux measurements and a refined model for the two-planetsystem using additional light curve data. We performed high angular resolutionadaptive optics imaging with the Keck and Subaru telescopes at two epochs whilethe source star was still amplified. We detected the lens flux, $H=16.39 \pm0.08$. The lens, a disk star, is brighter than predicted from the modeling inthe original study. We revisited the light curve modeling using additionalphotometric data from the B\&C telescope in New Zealand and CTIO 1.3m H bandlight curve. We then include the Keck and Subaru adaptive optic observationconstraints. The system is composed of a $\sim 4-9$ Gyr lens star of $\rmM_{lens} = 1.06 \pm 0.05~\,M_\odot$ at a distance of $\rm D_{lens} = 4.0 \pm0.3~$kpc, orbited by two giant planets of $\rm 0.145 \pm 0.008\ M_{\rm Jup}$and $0.86 \pm 0.06~\rm M_{\rm Jup}$ with projected separations of $4.0 \pm 0.5$ AU and $4.8 \pm 0.7$ AU respectively. Since the lens is brighter than thesource star by $16 \pm 8 \%$ in H, with no other blend within one arcsec, itwill be possible to estimate its metallicity by subsequent IR spectroscopy with8--10~m class telescopes. By adding a constraint on the metallicity it will bepossible to refine the age of the system.

Revisiting the microlensing event OGLE 2012-BLG-0026: A solar mass star with two cold giant planets