Direct detection of young giant planets can probe formation processes near the snow line, which is thought to be where giant planet formation is most likely. I will outline the scientific requirements for observational constraints on this process, and show that the minimum requirements from the ground can be achieved by a high contrast VLTI instrument (Hi-5/VIKiNG) operating within the 2-5 micron range, nulling starlight in a highly calibratable manner with a "Kernel Nuller". Understanding these processes in more depth will eventually require an instrument more sensitive than is possible from the ground, requiring a cooled space mission. I will describe a pathway for such a mission.
