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We have now accumulated a wealth of observations of the planet-formationenvironment and of mature planetary systems. These data allow us to test andrefine theories of gas-giant planet formation by placing constraints on theconditions and timescale of this process. Yet a number of fundamental questionsremain unanswered about how protoplanets accumulate material, theirphotospheric properties and compositions, and how they interact withprotoplanetary disks. While we have begun to detect protoplanet candidatesduring the last several years, we are presently only sensitive to the widestseparation, highest mass / accretion rate cases. Current observing facilitieslack the angular resolution and inner working angle to probe the few-AU orbitalseparations where giant planet formation is thought to be most efficient. Theyalso lack the contrast to detect accretion rates that would form lower mass gasgiants and ice giants. Instruments and telescopes coming online over the nextdecade will provide high contrast in the inner giant-planet-forming regionsaround young stars, allowing us to build a protoplanet census and tocharacterize planet formation in detail for the first time.

Imaging Giant Protoplanets with the ELTs