D5 High Energy

Topic

Central to this model is the suite of instruments that survey the high-energy sky.

Each high-energy radiation band requires its own specific detector technology, meaning no single instrument covers the entire landscape: soft and hard X-ray telescopes directly reveal accretion-powered sources and the temperatures of their surrounding disks.

Meanwhile, gamma-ray satellites capture the most energetic end of the synchrotron and inverse Compton emissions originating from jets and pulsars.

Ground-based Cherenkov telescope arrays extend this reach even further—up to the highest known gamma-ray energies—by detecting the secondary flash of light produced when a gamma ray strikes Earth's upper atmosphere.

Combining measurements from this entire chain of instruments—spanning from soft X-rays to very-high-energy gamma rays—allows for the reconstruction of a single high-energy source's complete radiative history, as no single instrument can observe more than one segment of that chain. Thus, from the instrument suite that opens this document to the complete radiative history that concludes it—taking in X-ray telescopes, gamma-ray satellites, and Cherenkov arrays along the way—high-energy observational astrophysics ensures that no violent source in the universe can hide its full history behind just one band of the spectrum.

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