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We present the analysis of high resolution follow-up observations ofOGLE-2016-BLG-1195 using Keck, four years after the event's peak. We find thelens system to be at $D_L = 6.87\pm 0.65$ kpc and comprised of a $M_{\rm p} =9.91\pm 1.61\ M_{\rm Earth}$ planet, orbiting an M-dwarf, $M_{\rm L} = 0.57\pm0.06\ M_{\odot}$, beyond the snow line, with a projected separation of$r_\perp=2.62\pm 0.28$ AU. Our results are consistent with the discovery paper,which reports values with 1-sigma uncertainties based on a single mass-distanceconstraint from finite source effects. However, both the discovery paper andour follow-up results disagree with the analysis of a different group that alsopresent the planetary signal detection. The latter utilizes Spitzer photometryto measure a parallax signal. Combined with finite source effects, they claimto measure the mass and distance of the system to much greater accuracy,suggesting that it is composed of an Earth-mass planet orbiting an ultracooldwarf. Their parallax signal though is improbable since it suggests a lens starin the disk moving perpendicular to disk rotation. Moreover, parallaxes areknown to be affected by systematic errors in the photometry. Therefore, wereanalyze the Spitzer photometry for this event and conclude that the parallaxsignal is not significantly greater than the instrumental noise, and is likelyaffected by systematic errors in the photometric data. The results of thispaper act as a cautionary tale that conclusions of analyses that rely heavilyon low signal-to-noise Spitzer photometric data, can be misleading.

OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck AO