  We present the analysis of high resolution follow-up observations of
OGLE-2016-BLG-1195 using Keck, four years after the event's peak. We find the
lens 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, $M_{\rm L} = 0.57\pm
0.06\ M_{\odot}$, 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-distance
constraint from finite source effects. However, both the discovery paper and
our follow-up results disagree with the analysis of a different group that also
present the planetary signal detection. The latter utilizes Spitzer photometry
to measure a parallax signal. Combined with finite source effects, they claim
to measure the mass and distance of the system to much greater accuracy,
suggesting that it is composed of an Earth-mass planet orbiting an ultracool
dwarf. Their parallax signal though is improbable since it suggests a lens star
in the disk moving perpendicular to disk rotation. Moreover, parallaxes are
known to be affected by systematic errors in the photometry. Therefore, we
reanalyze the Spitzer photometry for this event and conclude that the parallax
signal is not significantly greater than the instrumental noise, and is likely
affected by systematic errors in the photometric data. The results of this
paper act as a cautionary tale that conclusions of analyses that rely heavily
on low signal-to-noise Spitzer photometric data, can be misleading.
