Measurement of the cosmic ray hadron spectrum up to 30 TeV at mountain altitude: The primary proton spectrum

M. Aglietta; B. Alessandro; P. Antonioli; F. Arneodo; L. Bergamasco; M. Bertaina; C. Castagnoli; A. Castellina; A. Chiavassa; G. Cini Castagnoli; B. D'Ettorre Piazzoli; G. Di Sciascio; W. Fulgione; P. Galeotti; P. L. Ghia; M. Iacovacci; G. Mannocchi; C. Morello; G. Navarra; L. Riccati; O. Saavedra; G. C. Trinchero; S. Valchierotti; P. Vallania; S. Vernetto; C. Vigorito

doi:10.1016/S0927-6505(03)00103-8

Measurement of the cosmic ray hadron spectrum up to 30 TeV at mountain altitude: The primary proton spectrum

M. Aglietta, B. Alessandro, P. Antonioli, F. Arneodo, L. Bergamasco, M. Bertaina, C. Castagnoli, A. Castellina, A. Chiavassa, G. Cini Castagnoli, B. D'Ettorre Piazzoli, G. Di Sciascio, W. Fulgione, P. Galeotti, P. L. Ghia, M. Iacovacci, G. Mannocchi, C. Morello, G. Navarra, L. RiccatiO. Saavedra, G. C. Trinchero, S. Valchierotti, P. Vallania, S. Vernetto, C. Vigorito

Physics

Research output: Contribution to journal › Article › peer-review

Abstract

The flux of cosmic ray hadrons at the atmospheric depth of 820 g cm^-2 has been measured by means of the EAS-TOP hadron calorimeter (Campo Imperatore, National Gran Sasso Laboratories, 2005 m a.s.l.).The hadron spectrum is well described by a single power law:S_h(E_h)= (2.25±0.21±0.34^sys)×10^-7 E_h/1000 ^{(-2.79±0.05)} m^-2 s^-1 sr^-1 GeV^-1 overthe energy range 30 GeV-30 TeV. The procedure and the accuracy of the measurement are discussed.The primary proton spectrum is derived from the data by using the CORSIKA/QGSJET code to compute the local hadron flux as a function of the primary proton spectrum and to calculate and subtract the heavy nuclei contribution (basing on direct measurements). Over a wide energy range E₀=0.5-50 TeV its best fit is given by a single power law: S(E₀)= (9.8±1.1±1.6^sys)×10^-5 E₀/1000 ^{(-2.80±0.06)} m^-2 s^-1 sr^-1 GeV^-1. The validity of the CORSIKA/QGSJET code for such application has been checked using the EAS-TOP and KASCADE experimental data by reproducing the ratio of the measured hadron fluxes at the two experimental depths (820 and 1030 gcm^-2 respectively) at better than 10% in the considered energy range.

Original language	English (US)
Pages (from-to)	329-338
Number of pages	10
Journal	Astroparticle Physics
Volume	19
Issue number	3
DOIs	https://doi.org/10.1016/S0927-6505(03)00103-8
State	Published - Jun 2003

Keywords

Cosmic rays
Hadrons
High energy calorimetry
Primary protons

ASJC Scopus subject areas

Astronomy and Astrophysics

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10.1016/S0927-6505(03)00103-8

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Aglietta, M., Alessandro, B., Antonioli, P., Arneodo, F., Bergamasco, L., Bertaina, M., Castagnoli, C., Castellina, A., Chiavassa, A., Cini Castagnoli, G., D'Ettorre Piazzoli, B., Di Sciascio, G., Fulgione, W., Galeotti, P., Ghia, P. L., Iacovacci, M., Mannocchi, G., Morello, C., Navarra, G., ... Vigorito, C. (2003). Measurement of the cosmic ray hadron spectrum up to 30 TeV at mountain altitude: The primary proton spectrum. Astroparticle Physics, 19(3), 329-338. https://doi.org/10.1016/S0927-6505(03)00103-8

Aglietta, M, Alessandro, B, Antonioli, P, Arneodo, F, Bergamasco, L, Bertaina, M, Castagnoli, C, Castellina, A, Chiavassa, A, Cini Castagnoli, G, D'Ettorre Piazzoli, B, Di Sciascio, G, Fulgione, W, Galeotti, P, Ghia, PL, Iacovacci, M, Mannocchi, G, Morello, C, Navarra, G, Riccati, L, Saavedra, O, Trinchero, GC, Valchierotti, S, Vallania, P, Vernetto, S & Vigorito, C 2003, 'Measurement of the cosmic ray hadron spectrum up to 30 TeV at mountain altitude: The primary proton spectrum', Astroparticle Physics, vol. 19, no. 3, pp. 329-338. https://doi.org/10.1016/S0927-6505(03)00103-8

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title = "Measurement of the cosmic ray hadron spectrum up to 30 TeV at mountain altitude: The primary proton spectrum",

abstract = "The flux of cosmic ray hadrons at the atmospheric depth of 820 g cm-2 has been measured by means of the EAS-TOP hadron calorimeter (Campo Imperatore, National Gran Sasso Laboratories, 2005 m a.s.l.).The hadron spectrum is well described by a single power law:Sh(Eh)= (2.25±0.21±0.34sys)×10-7 Eh/1000 (-2.79±0.05) m-2 s-1 sr-1 GeV-1 overthe energy range 30 GeV-30 TeV. The procedure and the accuracy of the measurement are discussed.The primary proton spectrum is derived from the data by using the CORSIKA/QGSJET code to compute the local hadron flux as a function of the primary proton spectrum and to calculate and subtract the heavy nuclei contribution (basing on direct measurements). Over a wide energy range E0=0.5-50 TeV its best fit is given by a single power law: S(E0)= (9.8±1.1±1.6sys)×10-5 E0/1000 (-2.80±0.06) m-2 s-1 sr-1 GeV-1. The validity of the CORSIKA/QGSJET code for such application has been checked using the EAS-TOP and KASCADE experimental data by reproducing the ratio of the measured hadron fluxes at the two experimental depths (820 and 1030 gcm-2 respectively) at better than 10% in the considered energy range.",

keywords = "Cosmic rays, Hadrons, High energy calorimetry, Primary protons",

author = "M. Aglietta and B. Alessandro and P. Antonioli and F. Arneodo and L. Bergamasco and M. Bertaina and C. Castagnoli and A. Castellina and A. Chiavassa and {Cini Castagnoli}, G. and {D'Ettorre Piazzoli}, B. and {Di Sciascio}, G. and W. Fulgione and P. Galeotti and Ghia, {P. L.} and M. Iacovacci and G. Mannocchi and C. Morello and G. Navarra and L. Riccati and O. Saavedra and Trinchero, {G. C.} and S. Valchierotti and P. Vallania and S. Vernetto and C. Vigorito",

year = "2003",

month = jun,

doi = "10.1016/S0927-6505(03)00103-8",

language = "English (US)",

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issn = "0927-6505",

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TY - JOUR

T1 - Measurement of the cosmic ray hadron spectrum up to 30 TeV at mountain altitude

T2 - The primary proton spectrum

AU - Aglietta, M.

AU - Alessandro, B.

AU - Antonioli, P.

AU - Arneodo, F.

AU - Bergamasco, L.

AU - Bertaina, M.

AU - Castagnoli, C.

AU - Castellina, A.

AU - Chiavassa, A.

AU - Cini Castagnoli, G.

AU - D'Ettorre Piazzoli, B.

AU - Di Sciascio, G.

AU - Fulgione, W.

AU - Galeotti, P.

AU - Ghia, P. L.

AU - Iacovacci, M.

AU - Mannocchi, G.

AU - Morello, C.

AU - Navarra, G.

AU - Riccati, L.

AU - Saavedra, O.

AU - Trinchero, G. C.

AU - Valchierotti, S.

AU - Vallania, P.

AU - Vernetto, S.

AU - Vigorito, C.

PY - 2003/6

Y1 - 2003/6

N2 - The flux of cosmic ray hadrons at the atmospheric depth of 820 g cm-2 has been measured by means of the EAS-TOP hadron calorimeter (Campo Imperatore, National Gran Sasso Laboratories, 2005 m a.s.l.).The hadron spectrum is well described by a single power law:Sh(Eh)= (2.25±0.21±0.34sys)×10-7 Eh/1000 (-2.79±0.05) m-2 s-1 sr-1 GeV-1 overthe energy range 30 GeV-30 TeV. The procedure and the accuracy of the measurement are discussed.The primary proton spectrum is derived from the data by using the CORSIKA/QGSJET code to compute the local hadron flux as a function of the primary proton spectrum and to calculate and subtract the heavy nuclei contribution (basing on direct measurements). Over a wide energy range E0=0.5-50 TeV its best fit is given by a single power law: S(E0)= (9.8±1.1±1.6sys)×10-5 E0/1000 (-2.80±0.06) m-2 s-1 sr-1 GeV-1. The validity of the CORSIKA/QGSJET code for such application has been checked using the EAS-TOP and KASCADE experimental data by reproducing the ratio of the measured hadron fluxes at the two experimental depths (820 and 1030 gcm-2 respectively) at better than 10% in the considered energy range.

AB - The flux of cosmic ray hadrons at the atmospheric depth of 820 g cm-2 has been measured by means of the EAS-TOP hadron calorimeter (Campo Imperatore, National Gran Sasso Laboratories, 2005 m a.s.l.).The hadron spectrum is well described by a single power law:Sh(Eh)= (2.25±0.21±0.34sys)×10-7 Eh/1000 (-2.79±0.05) m-2 s-1 sr-1 GeV-1 overthe energy range 30 GeV-30 TeV. The procedure and the accuracy of the measurement are discussed.The primary proton spectrum is derived from the data by using the CORSIKA/QGSJET code to compute the local hadron flux as a function of the primary proton spectrum and to calculate and subtract the heavy nuclei contribution (basing on direct measurements). Over a wide energy range E0=0.5-50 TeV its best fit is given by a single power law: S(E0)= (9.8±1.1±1.6sys)×10-5 E0/1000 (-2.80±0.06) m-2 s-1 sr-1 GeV-1. The validity of the CORSIKA/QGSJET code for such application has been checked using the EAS-TOP and KASCADE experimental data by reproducing the ratio of the measured hadron fluxes at the two experimental depths (820 and 1030 gcm-2 respectively) at better than 10% in the considered energy range.

KW - Cosmic rays

KW - Hadrons

KW - High energy calorimetry

KW - Primary protons

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JO - Astroparticle Physics

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ER -

Measurement of the cosmic ray hadron spectrum up to 30 TeV at mountain altitude: The primary proton spectrum

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Keywords

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