Ices play a crucial role in planet formation and the delivery of volatiles to terrestrial planets, yet direct observations of ices in protoplanetary disks have, to date, been limited. Upcoming observational facilities—including JWST, large ground-based telescopes, SPHEREx, new SOFIA instrumentation, and future far-IR missions—will greatly enhance our view of disk ices by measuring their infrared spectral features. I will present a suite of models designed to complement these upcoming observations. The models use a kinetics-based gas-grain chemical evolution code to simulate the distribution of ices in a disk, followed by radiative transfer code using a subset of key ice species to simulate the observations. I will discuss which ice species are readily detectable and how the observable features vary with disk inclination, initial chemical composition (inheritance vs. reset scenarios), and subsequent chemical evolution. I will also highlight the value of obtaining spatially resolved spectra of edge-on disks (possible with JWST's integral field units) to constrain the vertical distribution of ices and isolate features from ices closer to the disk midplane.
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