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We investigated the possible cause-effect relation between the wiggling shapeof two stellar jets, MHO 1502 and MHO 2147, and the potential binarity of therespective driving stars.  We present high-angular-resolution H$_2$ (2.122 $\mu$m) and K-band imagesobtained with the Gemini South Adaptive Optics Imager (GSAOI) and the GeminiMulti-conjugate Adaptive Optics System (GeMS). The profiles of the jets aredepicted in detail by the H$_2$ images. We used K-band data to search forpotential close companions to the previously suggested exciting sources, andused archive data to investigate these sources and the environments in whichthe jets are located. We also applied a model to reproduce the wigglingprofiles 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. OurK-band image of the previously proposed exciting star, IRAC 18064, shows twosources separated by $\sim240$ AU, hinting at its binarity. However, as IRAC18064 is located off the jet axis at $\sim2064$ AU, it is questionable as towhether this source is the true exciting star. Moreover, the orbital modelcentred 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, theorbital model centred on the axis provides the best fits. Nevertheless, theprecession model centred on the axis cannot be discarded, despite having largerresiduals and $\chi^2$. MHO 2147 displays an S-shaped gentle continuousemission in H$_2$. We identify two other jets in the field of MHO 2147: apreviously reported quasi-perpendicular jet, MHO 2148, and a third jet adjacentto MHO 2147. The model that best fits the morphology of the MHO 2147 jet andthat of its adjacent jet is precession. The exciting source of MHO 2147 may bea triple system.

High-resolution images of two wiggling stellar jets, MHO 1502 and MHO 2147, obtained with GSAOI+GeMS