Abstract
TeV \(\upgamma \)-ray astronomy is outside the possibility of space-based experiments and can be at present studied only through ground-based experiments. However, because of the high background induced by CR showers, the large collection areas alone cannot provide adequate sensitivities for effective studies of cosmic \(\upgamma \)-rays. The capability to suppress the events induced by charged CRs was made possible with the advent of the Imaging Air Cherenkov Technique (IACT), Sect. 9.1 and with some dedicated air shower particle arrays, Sect. 9.2.
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Notes
- 1.
Note that a source with a flux equal to 1 % of the Crab is not detected in 100 min. The statistical significance of a signal excess depends on the background level, and this increases linearly with the observation time.
- 2.
Quasar is also the contraction of quasi-stellar object because in optical images they have optical luminosities greater than that of their host galaxy. Some astronomers use the term quasi-stellar object (QSO) to indicate radio-quiet quasars, reserving that of quasars for radio-loud objects.
- 3.
As an exercise, try to estimate the peak luminosity for the three considered objects using the redshift-distance relation.
- 4.
As an exercise, demonstrate that the CMB contribution in Fig. 9.20 would be represented by a parabola with negative concavity and vertex at about \(5\times 10^{-13}\) erg cm\(^{-3}\) at \(E_\upgamma \sim 10^{-3}\) eV.
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Spurio, M. (2015). The TeV Sky and Multiwavelength Astrophysics. In: Particles and Astrophysics. Astronomy and Astrophysics Library. Springer, Cham. https://doi.org/10.1007/978-3-319-08051-2_9
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