How to detect gamma-rays from ground: an introduction to the detection concepts

Abstract

Indirect detection of gamma rays with ground-based observatories is currently the most sensitive experimental approach to characterize the gamma-ray sky at energies $>0.1$\,TeV. Ground-based detection of gamma-rays relies on the electromagnetic showers that gamma rays initiate in the Earth's atmosphere. In this chapter we will review the properties of electromagnetic air showers as well as the differences with respect to cosmic-ray showers that enable the rejection of the cosmic ray background. The experimental techniques that have been developed for ground-based detection of gamma rays will be introduced. These fall onto three main categories: air shower particle detectors, sampling Cherenkov arrays, and imaging atmospheric Cherenkov telescopes. Hybrid concepts as well as other experimental approaches are also discussed.

24 pages, 11 figures, invited chapter in Handbook of X-ray and Gamma-ray Astrophysics (eds. Cosimo Bambi and Andrea Santangelo)

References in corpus (13)

• Observations of the Crab Nebula with H.E.S.S
• Teraelectronvolt Astronomy
• The major upgrade of the MAGIC telescopes, Part I: The hardware improvements and the commissioning of the system
• Discovery of TeV Gamma-Ray Emission from the Cygnus Region of the Galaxy
• Detection of the Geminga pulsar with MAGIC hints at a power-law tail emission beyond 15 GeV
• Detection of the Crab Nebula with the 9.7 m Prototype Schwarzschild-Couder Telescope
• FACT - Monitoring Blazars at Very High Energies
• A luminous and isolated gamma-ray flare from the blazar B2 1215+30
• Monte Carlo Studies of Geomagnetic Field Effects on the Imaging Air Cherenkov Technique for the MAGIC Telescope Site
• A method to correct IACT data for atmospheric absorption due to the Saharan Air Layer
• Design and Performance of the Prototype Schwarzschild-Couder Telescope Camera
• Panoramic SETI: Program Update and High-Energy Astrophysics Applications
• Very high-energy observations of the two high-frequency peaked BL Lac objects 1ES 1218+304 and H 1426+428