  We observed the galactic microquasar GRS1915+105 in the K ($2.2 \mu$m) band
on October 16 and 17, 1995 UTC using the COB infrared (IR) imager on the Kitt
Peak National Observatory 2.1-m telescope with a 0.2-arcsec/pixel plate scale
and under good ($\sim 0.7$-arcsec) seeing conditions. Using a neighboring star
in the image frames to determine the point spread function (PSF), we
PSF-subtract the images of GRS1915+105. We find no evidence of extended
emission such as the apparent near-IR jets seen by Sams et al. (1996) in July,
1995. Simple modelling of the star + jet structure allows us to place an upper
limit on any similar emission at that position of $K>16.4$ at the 95%
confidence level, as compared to $K=13.9$ as seen by Sams et al. (1996). This
lack of extended IR flux during continued hard X-ray flaring activity confirms
the hypothesis that the extended IR emission arises from the superluminal
radio-emitting jets rather than reprocessing of the X-ray emission on other
structures around the compact central object. Given the large apparent velocity
of the radio-emitting jets, by the time of our observations the Sams et al.
feature would have moved $>1$ arcsec from GRS1915+105, and we can place a limit
of $K>17.7$ (95% confidence level) on any infrared emission in this region. We
can thus place an upper limit on the radiative timescale of the feature of
$\tau < 25$ days, which is consistent with synchrotron jet emission.
