•Universe
COSI Fact Sheet
COSI is a wide field of view gamma-ray telescope that obtains high spectral resolution from 0.2 to 5 MeV, enabling sensitive narrow line imaging of the entire Galaxy.
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We use space-based and ground-based instrumentation to learn about the universe beyond our solar system. Our projects and missions make measurements across the electromagnetic (EM) spectrum and extend to multi-messenger astrophysics. Our science goals include understanding the history and structure of the universe, probing regions of extreme physics and element formation, and searching for habitable planets and potentially extraterrestrial life. We have scientists and engineers with many years of experience developing world class instrumentation such as specialized detectors for different parts of the EM spectrum as well as related technologies. Our specialty is to incorporate these technologies into complex systems and to use sophisticated instrument simulations to determine that the capabilities will achieve our science goals.
COSI is a wide field of view gamma-ray telescope that obtains high spectral resolution from 0.2 to 5 MeV, enabling sensitive narrow line imaging of the entire Galaxy.
Experiment to Detect the Global EoR Signature (EDGES). Detect the global 21-cm signal from the cosmic dawn. Characterize the diffuse synchrotron radiation from the Milky Way.
The origin and nature of Ultra-High Energy Cosmic Rays (UHECRs) and neutrinos (UHEN) remain unsolved in contemporary astroparticle physics. The Extreme Universe Space Observatory Super Pressure Balloon II Mission (EUSO-SPB2) is one of several precursor missions for a space mission (JEM-EUSO) that would be dedicated to UHECR research.
FUEGO’s scientific objective is to detect the very beginnings of wildfires, and to provide real-time information on a fire’s intensity, evolution and movement. The system is an imager operating in two IR bands (4 and 9 microns wavelength), with a visible context imager.
ISI is a three-telescope interferometric array that uses heterodyne detection at 11 microns wavelength (27 THz).
The Mapper of the IGM Spin Temperature (MIST) aim is to detect the global 21-cm signal from the cosmic dawn and the dark age.
