HIRMES will aim to study the evo-lution of protoplanetary systems. Shocks resulting in ionized gas emission lines due to mass accre-tion lead to star and planet forma-tion. Features of particular interest include water lines and ice, [OI] as a tracer of disk chemistry and radial structure, and HD as a tracer of disk mass. While Herschel and Spitzer focused on tracing intensity and spatial profiles, HIRMES will expand on this to yield spectral profiles by resolving these lines and determin-ing their origins from velocity pro-files, which are key components of shock models.