  We investigated the possible cause-effect relation between the wiggling shape
of two stellar jets, MHO 1502 and MHO 2147, and the potential binarity of the
respective driving stars.
  We present high-angular-resolution H$_2$ (2.122 $\mu$m) and K-band images
obtained with the Gemini South Adaptive Optics Imager (GSAOI) and the Gemini
Multi-conjugate Adaptive Optics System (GeMS). The profiles of the jets are
depicted in detail by the H$_2$ images. We used K-band data to search for
potential close companions to the previously suggested exciting sources, and
used archive data to investigate these sources and the environments in which
the jets are located. We also applied a model to reproduce the wiggling
profiles of the jets.
  MHO~1502 is composed of a chain of knots delineating the wiggling jet,
suggesting that the driving source emitted them in an intermittent manner. Our
K-band image of the previously proposed exciting star, IRAC 18064, shows two
sources separated by $\sim240$ AU, hinting at its binarity. However, as IRAC
18064 is located off the jet axis at $\sim2064$ AU, it is questionable as to
whether this source is the true exciting star. Moreover, the orbital model
centred on IRAC 18064 suggests a binary companion at a much greater distance
($\sim2200$ AU) than the nearby star (at $\sim$240 AU). On the other hand, the
orbital model centred on the axis provides the best fits. Nevertheless, the
precession model centred on the axis cannot be discarded, despite having larger
residuals and $\chi^2$. MHO 2147 displays an S-shaped gentle continuous
emission in H$_2$. We identify two other jets in the field of MHO 2147: a
previously reported quasi-perpendicular jet, MHO 2148, and a third jet adjacent
to MHO 2147. The model that best fits the morphology of the MHO 2147 jet and
that of its adjacent jet is precession. The exciting source of MHO 2147 may be
a triple system.
