Gamma-ray astronomy by the air shower technique: Performance and perspectives

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References to the arrays discussed in this paper are as follows:Cygnus Alexandreas D. E. et al.),Nucl. Instrum. Methods. A,311 (1992) 350; CASA-MIA (Borione A. et al.),Nucl. Instrum. Methods. A,346 (1994) 329; HEGRA (Aharonian F. et al.),Proc. XXIII ICRC, Calgary,4 (1993) 291;Tibet (Amenomori M. et al.),Proc. XXII ICRC, Dublin,2 (1991) 704; SPASE (Beaman J. et al.),Phys. Rev. D,48 (1993) 4495; EAS-TOP (Aglietta M. et al.),Nucl. Instrum. Methods. A,336 (1993) 310; JANZOS (Allen W. H. et al.),Phys. Rev. D,48 (1993) 466.

Bloomer S. D., Linsley J. andWatson A. A.,J. Phys. G,14 (1988) 645.

Borione A. et al., Nucl. Instrum. Methods. A,346 (1994) 329.

This technique to estimate the energy threshold of an array was suggested to the author by René Ong, University of Chicago.

Amenomori M. et al., Proceedings XXIV ICRC, Rome,2 (1995) 736.

Li T. andMa Y.,Astrophys. J.,272 (1983) 317.

Borione A. et al., Proc. XXIV ICRC, Rome,2 (1995) 430.

References for the integral flux limits for the Crab Nebula or SN1987a are the following:Tibet Amenomori M. et al.),Proc. XXIV ICRC, Rome,2 (1995) 346; CASA-MIA (Borione A. et al.),Proc. XXIV ICRC, Rome,2 (1995) 350; HEGRA (Willmer M. et al.),Proc. XXIV ICRC, Rome,2 (1995) 409 andFonseca V., private communication; EAS-TOP (Ghia P. L. et al.),Proc. XXIV ICRC, Rome,2 (1995) 421; GREX (Blake P. R., Luxton S. J. andNash W. F.,Proc. XXIV ICRC, Rome,2 (1995) 413;Cygnus (Alexandreas D. E. et al.),Proc. XXIII ICRC, Calgary,1 (1993) 353; SPASE (Beaman J. et al.),Proc. XXIII ICRC, Calgary,1 (1993) 346; JANZOS (Allen W. H. et al.),Proc. XXIII ICRC, Calgary,1 (1993) 348.

References to the atmospheric Cherenkov measurements of the Crab Nebula are:Whipple Lewis D. A. et al.),Proc. XIII ICRC, Rome,2 (1993) 279;Themistocle (Djannati-Ataï A. et al.),Proc. XXIV ICRC, Rome,2 (1995) 315;Cangaroo (Ca) (Tanimori T. et al.),Astrophys. J.,429 (1994) L61.

de Jager O. C. andHarding A. K.,Astrophys. J.,396 (1992) 161.

References for upper limits on the γ-ray flux from Cygnus X-3 are CASA-MIA, ref. [14] ;Kiel, ref. [2];Samorski M. andStamm W.,Astrophys. J.,268 (1983) L17;H. Park, ref. [3];Lloyd-Evans J. et al., Nature,305 (1983) 784. EAS-TOP (Ghia P. L. et al.),Proc. XXIV ICRC, Rome,2 (1995) 421;Cygnus (Alexandreas D. E. et al.),Proc. XXIII ICRC, Calgary,1 (1993) 373;Tibert (Amenomori M. et al.),Proc. XXIII ICRC, Calgary,1 (1993) 342; HEGRA (Merck M. et al.),Proc. XXIII ICRC, Calgary,1 (1993) 361.

Covault C. et al., Proc. XXIV ICRC, Rome,2 (1995) 463.

Amenomori M. et al., Proc. XXIV ICRC, Rome,4 (1995) 840.

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Drury L. O'C. et al., Astron. Astrophys.,287 (1994) 959.

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