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Through its ability to measure the energetics and dynamics of the atomic and molecular gas and dust in and around galaxies, Origins can probe nearly all aspects of the galactic ecosystem: star formation and AGN growth stellar death AGN-and starburst-driven outflows and gas cooling and accretion. Energetic processes that shape galaxies and the circumgalactic medium together define this ecosystem. Origins studies the baryon cycle in galactic ecosystems. However, we do not know how terrestrial planets get their water, since rocky planets with liquid water exist in regions where water in icy, protoplanetary dust Figure ES-3: Water provides the liquid medium for life's chemistry and plays an essential biochemical role. Water is essential to all life on our planet. How do the conditions for habitability develop during the process of planet formation? Origins studies the role of feedback processes in galaxies over a wide range of environments and redshifts by investigating the processes that drive powerful outflows and surveying the demographics of galactic feedback. The reason is thought to be 'feedback' from star formation or black hole growth, because supernovae or quasar winds can disrupt star-forming gas. How do the relative energetics from supernovae and quasars influence the interstellar medium of galaxies? Galaxies are made of billions of stars, yet star formation is extremely inefficient on all scales, from single molecular clouds to galaxy clusters. Sensitive metallicity indicators in the infrared can be used to track the growth of heavy elements in even the densest optically-obscured regions inside galaxies. How do galaxies make metals, dust, and organic molecules? Galaxies are the metal factories of the Universe, and Origins studies how heavy elements and dust were made and dispersed throughout the cosmic web over the past 12 billion years.
These observations probe the physics of the interstellar medium, characterize the atomic and molecular gas that drives star-formation, measure the buildup of metals from dying stars, and track the growth of SMBHs and their influence, as they drive energetic outflows into the surrounding interstellar medium (. How do the stars and supermassive black holes in galaxies evolve with time? Origins uses atomic and molecular emission lines and emission from dust grains to measure the density, temperature, and ionization state of the gas where stars are forming and in galactic nuclei. With 1000 times better sensitivity, Origins gives us a clear view of galaxy and metal growth across cosmic time, through a deep-and-wide spectroscopic survey in a wavelength regime inaccessible from the ground and that will remain unexplored by JWST. ES-3įrom First Light to Life which provided our first glimpses of dusty galaxies in the infrared during the peak epoch of star formation, when the Universe was only 3 Gyr old. Infrared photons between 2.8 and 588 μm in Origins' wavelength range capture emission from stars, molecules, dust, and ions/atoms, enabling a multi-pronged probe into key physical processes in galaxies. Origins studies the universe at a wavelength range that is inaccessible from the ground. Origins is agile, enabling >80% observing efficiency, in line with the 90% efficiency achieved with Herschel. The Origins design has very few critical deployments and builds upon the technical heritage of Spitzer, with passive cooling from a two-layer Sun shield and advanced cryocoolers maintaining the telescope at 4.5 K. Origins, with an aperture diameter of 5.9 m and a suite of powerful instruments, operates with spectral resolving power from 3 to 3x10 5 over the wavelength range from 2.8 to 588 μm. The Origins concept is low-risk and powerful: 1000 times more sensitive than prior far-IR missions.