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Understanding the origin of the astonishing diversity of exoplanets is a keyquestion for the coming decades. ALMA has revolutionized our view of the dustemission from protoplanetary disks, demonstrating the prevalence of ring andspiral structures that are likely sculpted by young planets in formation. Todetect kinematic signatures of these protoplanets and to probe the chemistry oftheir gas accretion reservoir will require the imaging of molecular spectralline emission at high angular and spectral resolution. However, the currentsensitivity of ALMA limits these important spectral studies to only the nearestprotoplanetary disks. Although some promising results are emerging, includingthe identification of the snowlines of a few key molecules and the firstattempt at detecting a protoplanet's spiral wake, it is not yet possible tosearch for these important signatures in a population of disks in diverseenvironments and ages. Harnessing the tremendous power of (sub)mm observationsto pinpoint and characterize the chemistry of planets in formation will requirea major increase of ALMA's spectral sensitivity (5-10x), increase ininstantaneous bandwidth (2x) at high spectral resolution, and improved angularresolution (2x) in the 2030 era.

Realizing the Unique Potential of ALMA to Probe the Gas Reservoir of Planet Formation