An upper limit to the flux of Ultra High Energy (UHE) gamma-rays in the primary cosmic radiation is obtained through the data of the electromagnetic and the muon detectors of the EAS-TOP Extensive Air Shower array (Campo Imperatore, National Gran Sasso Laboratories, atmospheric depth 810 g cm(-2)). The search is performed by selecting Extensive Air Showers (EAS) with low muon content, For EAS electron sizes N-e > 6.3 . 10(5), no showers are observed with the core located inside a fiducial area and no muons recorded in the 140 m(2) muon detector, during a live time of 8440 h. The 90% c.l. upper limit to the relative intensity of gamma-ray with respect to cosmic ray (c.r.) primaries is I-y/I-c.r. < 7.3 . 10(-5), at primary energy E(0) greater than or equal to 10(15) eV: this limit is lower than reported in previous measurements.

A limit to the rate of ultra high energy gamma-rays in the primary cosmic radiation

BERGAMASCO, Laura Maria;BERTAINA, Mario Edoardo;CASTAGNOLI, Carlo;CHIAVASSA, Andrea;GALEOTTI, Piero;NAVARRA, Gianni Maria;SAAVEDRA, Oscar;VIGORITO, Carlo Francesco
1996

Abstract

An upper limit to the flux of Ultra High Energy (UHE) gamma-rays in the primary cosmic radiation is obtained through the data of the electromagnetic and the muon detectors of the EAS-TOP Extensive Air Shower array (Campo Imperatore, National Gran Sasso Laboratories, atmospheric depth 810 g cm(-2)). The search is performed by selecting Extensive Air Showers (EAS) with low muon content, For EAS electron sizes N-e > 6.3 . 10(5), no showers are observed with the core located inside a fiducial area and no muons recorded in the 140 m(2) muon detector, during a live time of 8440 h. The 90% c.l. upper limit to the relative intensity of gamma-ray with respect to cosmic ray (c.r.) primaries is I-y/I-c.r. < 7.3 . 10(-5), at primary energy E(0) greater than or equal to 10(15) eV: this limit is lower than reported in previous measurements.
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M. Aglietta;B. Alessandro;P. Antonioli;F. Arneodo;L. Bergamasco;M. Bertaina;A. C. Fauth;C. Castagnoli;A. Castellina;A. Chiavassa;G. C. Castagnoli;B. D. Piazzoli;G. DiSciascio;W. Fulgione;P. Galeotti;P. L. Ghia;R. Granella;M. Jacovacci;A. L. deGodoi;G. Mannocchi;C. Melagrana;N. M. Silva;C. Morello;G. Navarra;H. Nogima;L. Ricatti;O. Saavedra;G. C. Trinchero;P. Vallania;S. Vernetto;C. Vigorito
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2318/108437
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