Gamma-ray astronomy

Gamma-ray astronomy is a subfield of <a href="/facts/Astronomy/0ArJVM1p">astronomy</a> where scientists <a href="/facts/Astronomical_observation/PKgYt9PX">observe</a> and study <a href="/facts/Celestial_object/BCHLa0Q2">celestial objects</a> and phenomena in <a href="/facts/Outer_space/R3LRKyFs">outer space</a> which emit cosmic <a href="/facts/Electromagnetic_radiation/Ynx7ujCW">electromagnetic radiation</a> in the form of <a href="/facts/Gamma_ray/5Drf913J">gamma rays</a>, i.e. <a href="/facts/Photon/mFNhAEzA">photons</a> with the highest <a href="/facts/Photon_energy/Gy4zEAaE">energies</a> (above 100 <a href="/facts/Electronvolt/YMT1fqX9">keV</a>) at the very shortest wavelengths. Radiation below 100 keV is classified as <a href="/facts/X-ray/wseP79cN">X-rays</a> and is the subject of <a href="/facts/X-ray_astronomy/KAQ6WxgQ">X-ray astronomy</a>.
In most cases, gamma rays from <a href="/facts/Solar_flare/6kCvPKxD">solar flares</a> and <a href="/facts/Terrestrial_gamma-ray_flash/6WykoU8y">Earth's atmosphere</a> fall in the MeV range, but it's now known that solar flares can also produce gamma rays in the GeV range, contrary to previous beliefs. Much of the detected gamma radiation stems from collisions between <a href="/facts/Hydrogen/BoYHjl0J">hydrogen</a> gas and <a href="/facts/Cosmic_ray/uxCVdTKd">cosmic rays</a> within our <a href="/facts/Galaxy/zCyUvEf7">galaxy</a>. These gamma rays, originating from diverse mechanisms such as <a href="/facts/Electron-positron_annihilation/ca6HdHfu">electron-positron annihilation</a>, the <a href="/facts/Inverse_Compton_effect/Q98Ty8rz">inverse Compton effect</a> and in some cases <a href="/facts/Gamma_decay/5Drf913J">gamma decay</a>, occur in regions of extreme temperature, density, and magnetic fields, reflecting violent astrophysical processes like the decay of neutral <a href="/facts/Pion/x5HamzG3">pions</a>. They provide insights into extreme events like <a href="/facts/Supernova/Pfo2J23l">supernovae</a>, <a href="/facts/Hypernova/7f0l3sQB">hypernovae</a>, and the behavior of matter in environments such as <a href="/facts/Pulsar/f8c7S5LQ">pulsars</a> and <a href="/facts/Blazar/gtIlQjQ5">blazars</a>. A huge number of gamma ray emitting high-energy systems like <a href="/facts/Black_hole/1r2lmkcF">black holes</a>, <a href="/facts/Stellar_corona/W4WNqV9u">stellar coronas</a>, <a href="/facts/Neutron_star/4enfoxBA">neutron stars</a>, <a href="/facts/White_dwarf/gIYlTtrC">white dwarf</a> stars, remnants of supernova, clusters of galaxies, including the <a href="/facts/Crab_Nebula/HmAndxQX">Crab Nebula</a> and the <a href="/facts/Vela_pulsar/qMAAg0Et">Vela pulsar</a> (the most powerful source so far), have been identified, alongside an overall diffuse <a href="/facts/Gamma_ray/5Drf913J">gamma-ray background</a> along the plane of the <a href="/facts/Milky_Way/ulF6lccN">Milky Way</a> galaxy. Cosmic radiation with the highest energy triggers electron-photon cascades in the atmosphere, while lower-energy gamma rays are only detectable above it. <a href="/facts/Gamma-ray_burst/oRRU6Fhn">Gamma-ray bursts</a>, like <a href="/facts/GRB_190114C/h2wFr865">GRB 190114C</a>, are transient phenomena challenging our understanding of high-energy <a href="/facts/Astrophysics/krFPRWLA">astrophysical processes</a>, ranging from microseconds to several hundred seconds.
Gamma rays are difficult to detect due to their high energy and their blocking by the Earth’s atmosphere, necessitating balloon-borne detectors and artificial satellites in space. Early experiments in the 1950s and 1960s used balloons to carry instruments to access altitudes where the atmospheric absorption of gamma rays is low, followed by the launch of the first gamma-ray satellites: <a href="/facts/Small_Astronomy_Satellite_2/W5d1rjbJ">SAS 2</a> (1972) and <a href="/facts/COS-B/FzjRbfyd">COS-B</a> (1975). These were defense satellites originally designed to detect gamma rays from secret nuclear testing, but they discovered puzzling gamma-ray bursts coming from deep space. In the 1970s, satellite observatories found several gamma-ray sources, among which a very strong source called <a href="/facts/Geminga/Mh2ctXRa">Geminga</a> was later identified as a pulsar in proximity. The <a href="/facts/Compton_Gamma_Ray_Observatory/XrhShxVh">Compton Gamma Ray Observatory</a> (launched in 1991) revealed numerous gamma-ray sources in space. Today, both ground-based observatories like the <a href="/facts/VERITAS/xylTuCUT">VERITAS</a> array and space-based telescopes like the <a href="/facts/Fermi_Gamma-ray_Space_Telescope/rwKktSFn">Fermi Gamma-ray Space Telescope</a> (launched in 2008) contribute significantly to gamma-ray astronomy. This interdisciplinary field involves collaboration among physicists, astrophysicists, and engineers in projects like the <a href="/facts/High_Energy_Stereoscopic_System/Tw9ovaIw">High Energy Stereoscopic System</a> (H.E.S.S.), which explores extreme astrophysical environments like the vicinity of <a href="/facts/Black_hole/1r2lmkcF">black holes</a> in <a href="/facts/Active_galactic_nuclei/qT1owvXz">active galactic nuclei</a>.
Studying gamma rays provides valuable insights into extreme astrophysical environments, as observed by the H.E.S.S. Observatory. Ongoing research aims to expand our understanding of gamma-ray sources, such as blazars, and their implications for cosmology. As GeV gamma rays are important in the study of extra-solar, and especially <a href="/facts/Extragalactic_astronomy/WtKKEWru">extragalactic</a>, astronomy, new observations may complicate some prior models and findings. 
Future developments in gamma-ray astronomy will integrate data from <a href="/facts/Gravitational_wave/4XWN3NtG">gravitational wave</a> and <a href="/facts/Neutrino/yGWVfSg2">neutrino</a> observatories (<a href="/facts/Multi-messenger_astronomy/7pvCx4PL">Multi-messenger astronomy</a>), enriching our understanding of cosmic events like neutron star mergers. Technological advancements, including advanced <a href="/facts/Mirror/wMu4u6BB">mirror</a> designs, better <a href="/facts/Camera/j4uqsfJQ">camera</a> technologies, improved trigger systems, faster <a href="/facts/Readout_integrated_circuit/4kfWtmcL">readout electronics</a>, high-performance photon detectors like <a href="/facts/Silicon_photomultiplier/fg5Mx48B">Silicon photomultipliers</a> (SiPMs), alongside innovative data processing algorithms like time-tagging techniques and <a href="/facts/Event_reconstruction/URwQSDJt">event reconstruction</a> methods, will enhance <a href="/facts/Spatial_resolution/ll8LNYxN">spatial</a> and <a href="/facts/Temporal_resolution/9wp61G97">temporal resolution</a>. <a href="/facts/Machine_learning/e0w0XJTu">Machine learning</a> algorithms and <a href="/facts/Big_data/XGtrVg4z">big data</a> analytics will facilitate the extraction of meaningful insights from vast datasets, leading to discoveries of new gamma-ray sources, identification of specific gamma-ray signatures, and improved modeling of gamma-ray emission mechanisms. Future missions may include space telescopes and lunar gamma-ray observatories (taking advantage of the <a href="/facts/Moon/zKHqEMPb">Moon</a>'s lack of atmosphere and stable environment for prolonged observations), enabling observations in previously inaccessible regions. The ground-based <a href="/facts/Cherenkov_Telescope_Array/q6QmtgFG">Cherenkov Telescope Array</a> project, a next-generation gamma ray observatory which will incorporate many of these improvements and will be ten times more sensitive, is planned to be fully operational by 2025.

Gamma-ray astronomy open-in-new

Gamma-ray astronomy