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Star formation feedback is mapped around the local environments of protostars and from multiple chemical tracers (ices, gas-phase molecules, and ionized species). Using near- to mid-infrared integral field unit (IFU) observations, the James Webb Space Telescope (JWST) traces the masses and temperatures of gaseous CO and H2 on Solar System scales (<1000 au) from five protostars at their inception. The same JWST data also reveal the first evidence of momentum-driving wide-angle winds emanating from shocks that produce [Fe II] and other ionic emission lines at 1000 to 2500 au in the outflow cavity of an intermediate-mass protostar. Combining near-infrared imaging of [Fe II] and H I from the Hubble Space Telescope (HST) with far-infrared [O I] spectra from the Stratospheric Observatory for Infrared Astronomy (SOFIA), a more mature protostar's outflowing gas opens a cavity in its immediate surrounding, and the protostellar winds lose energy on 10000 au scales. Finally, using the same HST+SOFIA dataset, the remnants of a protostellar jet precesses through a cloud on parsec-scales and locally quenches star formation.
