The role of the pre-solar chemistry in the present chemical composition of the Solar System bodies is far to be understood. The molecular complexity builds up at each step of the process leading to star formation, starting from simple molecules and ending up in interstellar Complex Organic Molecules (iCOMs). It is of paramount importance to image the spatial distribution of iCOMs in order to investigate their association with different ingredients of the Sun-like star formation recipe (warm envelopes and cavities opened from hot jets, accretion disks and shocks). Thanks to the combination of the high-sensitivities and high-angular resolutions provided by the advent of new telescopes such as ALMA and NOEMA, it is now possible to image in details the earliest stages of the Sun-like star formation, thus inspecting the inner (less than 20-50 au from the driving protostar) jet. At these spatial scales a proper study of jets has to take into account also the effects connected with the accreting disk. In other words, it is time to study the protostellar jet-disk system as a whole. Shocks are precious diagnostic tools, given they enrich the gas phase with the species deposited onto the dust mantles and/or locked in the refractory dust cores. Basically, we have to deal with two kind of shocks: (i) high-velocity shocks produced by protostellar jets, and (ii) slow accretion shocks located close to the centrifugal barrier of the accretion disks. Both shocks are factories of iCOMs, which can be then efficiently used to follow both the kinematics and the chemistry of the inner protostellar systems. With this in mind, we will discuss recent results obtained in the framework of different large programs at mm and sub-mm wavelengths, such as SOLIS.