Planetary systems form out of disks of dust and gas that are an integral part of the star formation process. The structure of inner regions of these protoplanetary disks has important implications for terrestrial planet formation, giant planet migration, and disk accretion. I present spectrally dispersed infrared interferometric observations that spatially resolve dust and gas within 1 AU of young stars, and I discuss new insights into star and planet formation processes that are enabled with these data. I also describe a program of upgrades to the Keck Interferometer that has enabled these observations and will yield a range of new scientific opportunities in the near future.