The cosmic ray proton, helium and CNO fluxes in the 100 TeV energy region from TeV muons and EAS atmospheric Cherenkov light observations of MACRO and EAS-TOP

M. Aglietta; B. Alessandro; P. Antonioli; F. Arneodo; L. Bergamasco; M. Bertaina; C. Castagnoli; A. Castellina; A. Chiavassa; G. Cini; B. D'Ettorre Piazzoli; G. di Sciascio; W. Fulgione; P. Galeotti; P. L. Ghia; M. Iacovacci; G. Mannocchi; C. Morello; G. Navarra; O. Saavedra; A. Stamerra; G. C. Trinchero; S. Valchierotti; P. Vallania; S. Vernetto; C. Vigorito; M. Ambrosio; R. Antolini; A. Baldini; G. C. Barbarino; B. C. Barish; G. Battistoni; Y. Becherini; R. Bellotti; C. Bemporad; P. Bernardini; H. Bilokon; C. Bower; M. Brigida; S. Bussino; F. Cafagna; M. Calicchio; D. Campana; M. Carboni; R. Caruso; S. Cecchini; F. Cei; V. Chiarella; T. Chiarusi; B. C. Choudhary; S. Coutu; M. Cozzi; G. de Cataldo; H. Dekhissi; C. de Marzo; I. de Mitri; J. Derkaoui; M. de Vincenzi; A. di Credico; O. Erriquez; C. Favuzzi; C. Forti; P. Fusco; G. Giacomelli; G. Giannini; N. Giglietto; M. Giorgini; M. Grassi; A. Grillo; F. Guarino; C. Gustavino; A. Habig; K. Hanson; R. Heinz; E. Iarocci; E. Katsavounidis; I. Katsavounidis; E. Kearns; H. Kim; S. Kyriazopoulou; E. Lamanna; C. Lane; D. S. Levin; P. Lipari; N. P. Longley; M. J. Longo; F. Loparco; F. Maaroufi; G. Mancarella; G. Mandrioli; A. Margiotta; A. Marini; D. Martello; A. Marzari-Chiesa; M. N. Mazziotta; D. G. Michael; P. Monacelli; T. Montaruli; M. Monteno; S. Mufson; J. Musser; D. Nicolò; R. Nolty; C. Orth; G. Osteria; O. Palamara; V. Patera; L. Patrizii; R. Pazzi; C. W. Peck; L. Perrone; S. Petrera; V. Popa; A. Rainò; J. Reynoldson; F. Ronga; C. Satriano; E. Scapparone; K. Scholberg; A. Sciubba; M. Sioli; G. Sirri; M. Sitta; P. Spinelli; M. Spinetti; M. Spurio; R. Steinberg; J. L. Stone; L. R. Sulak; A. Surdo; G. Tarlé; V. Togo; M. Vakili; C. W. Walter; R. Webb

doi:10.1016/j.astropartphys.2004.01.005

The cosmic ray proton, helium and CNO fluxes in the 100 TeV energy region from TeV muons and EAS atmospheric Cherenkov light observations of MACRO and EAS-TOP

M. Aglietta, B. Alessandro, P. Antonioli, F. Arneodo, L. Bergamasco, M. Bertaina, C. Castagnoli, A. Castellina, A. Chiavassa, G. Cini, B. D'Ettorre Piazzoli, G. di Sciascio, W. Fulgione, P. Galeotti, P. L. Ghia, M. Iacovacci, G. Mannocchi, C. Morello, G. Navarra, O. SaavedraA. Stamerra, G. C. Trinchero, S. Valchierotti, P. Vallania, S. Vernetto, C. Vigorito, M. Ambrosio, R. Antolini, A. Baldini, G. C. Barbarino, B. C. Barish, G. Battistoni, Y. Becherini, R. Bellotti, C. Bemporad, P. Bernardini, H. Bilokon, C. Bower, M. Brigida, S. Bussino, F. Cafagna, M. Calicchio, D. Campana, M. Carboni, R. Caruso, S. Cecchini, F. Cei, V. Chiarella, T. Chiarusi, B. C. Choudhary, S. Coutu, M. Cozzi, G. de Cataldo, H. Dekhissi, C. de Marzo, I. de Mitri, J. Derkaoui, M. de Vincenzi, A. di Credico, O. Erriquez, C. Favuzzi, C. Forti, P. Fusco, G. Giacomelli, G. Giannini, N. Giglietto, M. Giorgini, M. Grassi, A. Grillo, F. Guarino, C. Gustavino, A. Habig, K. Hanson, R. Heinz, E. Iarocci, E. Katsavounidis, I. Katsavounidis, E. Kearns, H. Kim, S. Kyriazopoulou, E. Lamanna, C. Lane, D. S. Levin, P. Lipari, N. P. Longley, M. J. Longo, F. Loparco, F. Maaroufi, G. Mancarella, G. Mandrioli, A. Margiotta, A. Marini, D. Martello, A. Marzari-Chiesa, M. N. Mazziotta, D. G. Michael, P. Monacelli, T. Montaruli, M. Monteno, S. Mufson, J. Musser, D. Nicolò, R. Nolty, C. Orth, G. Osteria, O. Palamara, V. Patera, L. Patrizii, R. Pazzi, C. W. Peck, L. Perrone, S. Petrera, V. Popa, A. Rainò, J. Reynoldson, F. Ronga, C. Satriano, E. Scapparone, K. Scholberg, A. Sciubba, M. Sioli, G. Sirri, M. Sitta, P. Spinelli, M. Spinetti, M. Spurio, R. Steinberg, J. L. Stone, L. R. Sulak, A. Surdo, G. Tarlé, V. Togo, M. Vakili, C. W. Walter, R. Webb

Dipartimento di Scienze e Innovazione Tecnologica

Risultato della ricerca: Contributo su rivista › Articolo in rivista › peer review

Abstract

The primary cosmic ray (CR) proton, helium and CNO fluxes in the energy range 80-300 TeV are studied at the National Gran Sasso Laboratories by means of EAS-TOP (Campo Imperatore, 2005 m a.s.l.) and MACRO (deep underground, 3100 m w.e., the surface energy threshold for a muon reaching the detector being E_μ^th≈1.3 TeV). The measurement is based on: (a) the selection of primaries based on their energy/nucleon (i.e., with energy/nucleon sufficient to produce a muon with energy larger than 1.3 TeV) and the reconstruction of the shower geometry by means of the muons recorded by MACRO in the deep underground laboratories; (b) the detection of the associated atmospheric Cherenkov light (C.l.) signals by means of the C.l. detector of EAS-TOP. The C.l. density at core distance r>100 m is directly related to the total primary energy E₀. Proton and helium ("p + He") and proton, helium and CNO ("p + He + CNO") primaries are thus selected at E₀≃80 TeV, and at E₀≃250 TeV, respectively. Their flux is measured: J_p+He(80 Tev= (1.8±0.4)×10^-6 m^-2 s^-1 sr^-1 TeV^-1, and J_p+He+CNO(250 TeV)=(1.1±0.3)×10^-7 m^-2 s^-1 sr^-1 TeV^-1, their relative weights being: J_p+He/J_p+He+CNO (250 TeV)=0.78±0.17. By using the measurements of the proton spectrum obtained from the direct experiments and hadron flux data in the atmosphere, we obtain for the relative weights of the three components at 250 TeV: J_p:J_He:J_CNO =(0.20±0.08): (0.58±0.19):(0.22±0.17). This corresponds to the dominance of helium over proton primaries at 100-1000 TeV, and a possible non-negligible contribution from CNO.The lateral distribution of Cherenkov light in Extensive Air Showers (EASs), which is related to the rate of energy deposit of the primary in the atmosphere, is measured for a selected proton and helium primary beam, and good agreement is found when compared with the one calculated with the CORSIKA/QGSJET simulation model.

Lingua originale	Inglese
pagine (da-a)	223-240
Numero di pagine	18
Rivista	Astroparticle Physics
Volume	21
Numero di pubblicazione	3
DOI	https://doi.org/10.1016/j.astropartphys.2004.01.005
Stato di pubblicazione	Pubblicato - giu 2004

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10.1016/j.astropartphys.2004.01.005

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Aglietta, M., Alessandro, B., Antonioli, P., Arneodo, F., Bergamasco, L., Bertaina, M., Castagnoli, C., Castellina, A., Chiavassa, A., Cini, G., D'Ettorre Piazzoli, B., di Sciascio, G., Fulgione, W., Galeotti, P., Ghia, P. L., Iacovacci, M., Mannocchi, G., Morello, C., Navarra, G., ... Webb, R. (2004). The cosmic ray proton, helium and CNO fluxes in the 100 TeV energy region from TeV muons and EAS atmospheric Cherenkov light observations of MACRO and EAS-TOP. Astroparticle Physics, 21(3), 223-240. https://doi.org/10.1016/j.astropartphys.2004.01.005

@article{3357623d563b447b83e81d4a6787e03e,

title = "The cosmic ray proton, helium and CNO fluxes in the 100 TeV energy region from TeV muons and EAS atmospheric Cherenkov light observations of MACRO and EAS-TOP",

abstract = "The primary cosmic ray (CR) proton, helium and CNO fluxes in the energy range 80-300 TeV are studied at the National Gran Sasso Laboratories by means of EAS-TOP (Campo Imperatore, 2005 m a.s.l.) and MACRO (deep underground, 3100 m w.e., the surface energy threshold for a muon reaching the detector being Eμth≈1.3 TeV). The measurement is based on: (a) the selection of primaries based on their energy/nucleon (i.e., with energy/nucleon sufficient to produce a muon with energy larger than 1.3 TeV) and the reconstruction of the shower geometry by means of the muons recorded by MACRO in the deep underground laboratories; (b) the detection of the associated atmospheric Cherenkov light (C.l.) signals by means of the C.l. detector of EAS-TOP. The C.l. density at core distance r>100 m is directly related to the total primary energy E0. Proton and helium ({"}p + He{"}) and proton, helium and CNO ({"}p + He + CNO{"}) primaries are thus selected at E0≃80 TeV, and at E0≃250 TeV, respectively. Their flux is measured: Jp+He(80 Tev= (1.8±0.4)×10-6 m-2 s-1 sr-1 TeV-1, and Jp+He+CNO(250 TeV)=(1.1±0.3)×10-7 m-2 s-1 sr-1 TeV-1, their relative weights being: Jp+He/Jp+He+CNO (250 TeV)=0.78±0.17. By using the measurements of the proton spectrum obtained from the direct experiments and hadron flux data in the atmosphere, we obtain for the relative weights of the three components at 250 TeV: Jp:JHe:JCNO =(0.20±0.08): (0.58±0.19):(0.22±0.17). This corresponds to the dominance of helium over proton primaries at 100-1000 TeV, and a possible non-negligible contribution from CNO.The lateral distribution of Cherenkov light in Extensive Air Showers (EASs), which is related to the rate of energy deposit of the primary in the atmosphere, is measured for a selected proton and helium primary beam, and good agreement is found when compared with the one calculated with the CORSIKA/QGSJET simulation model.",

keywords = "Composition, Cosmic rays, Extensive air showers, High energies, Underground muons",

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 G. Cini 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 O. Saavedra and A. Stamerra and Trinchero, \{G. C.\} and S. Valchierotti and P. Vallania and S. Vernetto and C. Vigorito and M. Ambrosio and R. Antolini and A. Baldini and Barbarino, \{G. C.\} and Barish, \{B. C.\} and G. Battistoni and Y. Becherini and R. Bellotti and C. Bemporad and P. Bernardini and H. Bilokon and C. Bower and M. Brigida and S. Bussino and F. Cafagna and M. Calicchio and D. Campana and M. Carboni and R. Caruso and S. Cecchini and F. Cei and V. Chiarella and T. Chiarusi and Choudhary, \{B. C.\} and S. Coutu and M. Cozzi and \{de Cataldo\}, G. and H. Dekhissi and \{de Marzo\}, C. and \{de Mitri\}, I. and J. Derkaoui and \{de Vincenzi\}, M. and \{di Credico\}, A. and O. Erriquez and C. Favuzzi and C. Forti and P. Fusco and G. Giacomelli and G. Giannini and N. Giglietto and M. Giorgini and M. Grassi and A. Grillo and F. Guarino and C. Gustavino and A. Habig and K. Hanson and R. Heinz and E. Iarocci and E. Katsavounidis and I. Katsavounidis and E. Kearns and H. Kim and S. Kyriazopoulou and E. Lamanna and C. Lane and Levin, \{D. S.\} and P. Lipari and Longley, \{N. P.\} and Longo, \{M. J.\} and F. Loparco and F. Maaroufi and G. Mancarella and G. Mandrioli and A. Margiotta and A. Marini and D. Martello and A. Marzari-Chiesa and Mazziotta, \{M. N.\} and Michael, \{D. G.\} and P. Monacelli and T. Montaruli and M. Monteno and S. Mufson and J. Musser and D. Nicol{\`o} and R. Nolty and C. Orth and G. Osteria and O. Palamara and V. Patera and L. Patrizii and R. Pazzi and Peck, \{C. W.\} and L. Perrone and S. Petrera and V. Popa and A. Rain{\`o} and J. Reynoldson and F. Ronga and C. Satriano and E. Scapparone and K. Scholberg and A. Sciubba and M. Sioli and G. Sirri and M. Sitta and P. Spinelli and M. Spinetti and M. Spurio and R. Steinberg and Stone, \{J. L.\} and Sulak, \{L. R.\} and A. Surdo and G. Tarl{\'e} and V. Togo and M. Vakili and Walter, \{C. W.\} and R. Webb",

note = "Funding Information: We gratefully acknowledge the support of the Gran Sasso National Laboratories and the assistance of the technical staff of the Institutions participating in the experiments. We thank Istituto Nazionale di Fisica Nucleare (INFN), the Consiglio Nazionale delle Ricerche (CNR) and the US Department of Energy and the US National Science Foundation for their support to the experiments. We also thank INFN, ICTP (Trieste), WorldLab and NATO for providing fellowships and grants (FAI) for non-Italian citizens. ",

year = "2004",

month = jun,

doi = "10.1016/j.astropartphys.2004.01.005",

language = "English",

volume = "21",

pages = "223--240",

journal = "Astroparticle Physics",

issn = "0927-6505",

publisher = "Elsevier B.V.",

number = "3",

}

Aglietta, M, Alessandro, B, Antonioli, P, Arneodo, F, Bergamasco, L, Bertaina, M, Castagnoli, C, Castellina, A, Chiavassa, A, Cini, G, D'Ettorre Piazzoli, B, di Sciascio, G, Fulgione, W, Galeotti, P, Ghia, PL, Iacovacci, M, Mannocchi, G, Morello, C, Navarra, G, Saavedra, O, Stamerra, A, Trinchero, GC, Valchierotti, S, Vallania, P, Vernetto, S, Vigorito, C, Ambrosio, M, Antolini, R, Baldini, A, Barbarino, GC, Barish, BC, Battistoni, G, Becherini, Y, Bellotti, R, Bemporad, C, Bernardini, P, Bilokon, H, Bower, C, Brigida, M, Bussino, S, Cafagna, F, Calicchio, M, Campana, D, Carboni, M, Caruso, R, Cecchini, S, Cei, F, Chiarella, V, Chiarusi, T, Choudhary, BC, Coutu, S, Cozzi, M, de Cataldo, G, Dekhissi, H, de Marzo, C, de Mitri, I, Derkaoui, J, de Vincenzi, M, di Credico, A, Erriquez, O, Favuzzi, C, Forti, C, Fusco, P, Giacomelli, G, Giannini, G, Giglietto, N, Giorgini, M, Grassi, M, Grillo, A, Guarino, F, Gustavino, C, Habig, A, Hanson, K, Heinz, R, Iarocci, E, Katsavounidis, E, Katsavounidis, I, Kearns, E, Kim, H, Kyriazopoulou, S, Lamanna, E, Lane, C, Levin, DS, Lipari, P, Longley, NP, Longo, MJ, Loparco, F, Maaroufi, F, Mancarella, G, Mandrioli, G, Margiotta, A, Marini, A, Martello, D, Marzari-Chiesa, A, Mazziotta, MN, Michael, DG, Monacelli, P, Montaruli, T, Monteno, M, Mufson, S, Musser, J, Nicolò, D, Nolty, R, Orth, C, Osteria, G, Palamara, O, Patera, V, Patrizii, L, Pazzi, R, Peck, CW, Perrone, L, Petrera, S, Popa, V, Rainò, A, Reynoldson, J, Ronga, F, Satriano, C, Scapparone, E, Scholberg, K, Sciubba, A, Sioli, M, Sirri, G, Sitta, M, Spinelli, P, Spinetti, M, Spurio, M, Steinberg, R, Stone, JL, Sulak, LR, Surdo, A, Tarlé, G, Togo, V, Vakili, M, Walter, CW & Webb, R 2004, 'The cosmic ray proton, helium and CNO fluxes in the 100 TeV energy region from TeV muons and EAS atmospheric Cherenkov light observations of MACRO and EAS-TOP', Astroparticle Physics, vol. 21, n. 3, pagg. 223-240. https://doi.org/10.1016/j.astropartphys.2004.01.005

TY - JOUR

T1 - The cosmic ray proton, helium and CNO fluxes in the 100 TeV energy region from TeV muons and EAS atmospheric Cherenkov light observations of MACRO and EAS-TOP

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, 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 - Saavedra, O.

AU - Stamerra, A.

AU - Trinchero, G. C.

AU - Valchierotti, S.

AU - Vallania, P.

AU - Vernetto, S.

AU - Vigorito, C.

AU - Ambrosio, M.

AU - Antolini, R.

AU - Baldini, A.

AU - Barbarino, G. C.

AU - Barish, B. C.

AU - Battistoni, G.

AU - Becherini, Y.

AU - Bellotti, R.

AU - Bemporad, C.

AU - Bernardini, P.

AU - Bilokon, H.

AU - Bower, C.

AU - Brigida, M.

AU - Bussino, S.

AU - Cafagna, F.

AU - Calicchio, M.

AU - Campana, D.

AU - Carboni, M.

AU - Caruso, R.

AU - Cecchini, S.

AU - Cei, F.

AU - Chiarella, V.

AU - Chiarusi, T.

AU - Choudhary, B. C.

AU - Coutu, S.

AU - Cozzi, M.

AU - de Cataldo, G.

AU - Dekhissi, H.

AU - de Marzo, C.

AU - de Mitri, I.

AU - Derkaoui, J.

AU - de Vincenzi, M.

AU - di Credico, A.

AU - Erriquez, O.

AU - Favuzzi, C.

AU - Forti, C.

AU - Fusco, P.

AU - Giacomelli, G.

AU - Giannini, G.

AU - Giglietto, N.

AU - Giorgini, M.

AU - Grassi, M.

AU - Grillo, A.

AU - Guarino, F.

AU - Gustavino, C.

AU - Habig, A.

AU - Hanson, K.

AU - Heinz, R.

AU - Iarocci, E.

AU - Katsavounidis, E.

AU - Katsavounidis, I.

AU - Kearns, E.

AU - Kim, H.

AU - Kyriazopoulou, S.

AU - Lamanna, E.

AU - Lane, C.

AU - Levin, D. S.

AU - Lipari, P.

AU - Longley, N. P.

AU - Longo, M. J.

AU - Loparco, F.

AU - Maaroufi, F.

AU - Mancarella, G.

AU - Mandrioli, G.

AU - Margiotta, A.

AU - Marini, A.

AU - Martello, D.

AU - Marzari-Chiesa, A.

AU - Mazziotta, M. N.

AU - Michael, D. G.

AU - Monacelli, P.

AU - Montaruli, T.

AU - Monteno, M.

AU - Mufson, S.

AU - Musser, J.

AU - Nicolò, D.

AU - Nolty, R.

AU - Orth, C.

AU - Osteria, G.

AU - Palamara, O.

AU - Patera, V.

AU - Patrizii, L.

AU - Pazzi, R.

AU - Peck, C. W.

AU - Perrone, L.

AU - Petrera, S.

AU - Popa, V.

AU - Rainò, A.

AU - Reynoldson, J.

AU - Ronga, F.

AU - Satriano, C.

AU - Scapparone, E.

AU - Scholberg, K.

AU - Sciubba, A.

AU - Sioli, M.

AU - Sirri, G.

AU - Sitta, M.

AU - Spinelli, P.

AU - Spinetti, M.

AU - Spurio, M.

AU - Steinberg, R.

AU - Stone, J. L.

AU - Sulak, L. R.

AU - Surdo, A.

AU - Tarlé, G.

AU - Togo, V.

AU - Vakili, M.

AU - Walter, C. W.

AU - Webb, R.

N1 - Funding Information: We gratefully acknowledge the support of the Gran Sasso National Laboratories and the assistance of the technical staff of the Institutions participating in the experiments. We thank Istituto Nazionale di Fisica Nucleare (INFN), the Consiglio Nazionale delle Ricerche (CNR) and the US Department of Energy and the US National Science Foundation for their support to the experiments. We also thank INFN, ICTP (Trieste), WorldLab and NATO for providing fellowships and grants (FAI) for non-Italian citizens.

PY - 2004/6

Y1 - 2004/6

N2 - The primary cosmic ray (CR) proton, helium and CNO fluxes in the energy range 80-300 TeV are studied at the National Gran Sasso Laboratories by means of EAS-TOP (Campo Imperatore, 2005 m a.s.l.) and MACRO (deep underground, 3100 m w.e., the surface energy threshold for a muon reaching the detector being Eμth≈1.3 TeV). The measurement is based on: (a) the selection of primaries based on their energy/nucleon (i.e., with energy/nucleon sufficient to produce a muon with energy larger than 1.3 TeV) and the reconstruction of the shower geometry by means of the muons recorded by MACRO in the deep underground laboratories; (b) the detection of the associated atmospheric Cherenkov light (C.l.) signals by means of the C.l. detector of EAS-TOP. The C.l. density at core distance r>100 m is directly related to the total primary energy E0. Proton and helium ("p + He") and proton, helium and CNO ("p + He + CNO") primaries are thus selected at E0≃80 TeV, and at E0≃250 TeV, respectively. Their flux is measured: Jp+He(80 Tev= (1.8±0.4)×10-6 m-2 s-1 sr-1 TeV-1, and Jp+He+CNO(250 TeV)=(1.1±0.3)×10-7 m-2 s-1 sr-1 TeV-1, their relative weights being: Jp+He/Jp+He+CNO (250 TeV)=0.78±0.17. By using the measurements of the proton spectrum obtained from the direct experiments and hadron flux data in the atmosphere, we obtain for the relative weights of the three components at 250 TeV: Jp:JHe:JCNO =(0.20±0.08): (0.58±0.19):(0.22±0.17). This corresponds to the dominance of helium over proton primaries at 100-1000 TeV, and a possible non-negligible contribution from CNO.The lateral distribution of Cherenkov light in Extensive Air Showers (EASs), which is related to the rate of energy deposit of the primary in the atmosphere, is measured for a selected proton and helium primary beam, and good agreement is found when compared with the one calculated with the CORSIKA/QGSJET simulation model.

AB - The primary cosmic ray (CR) proton, helium and CNO fluxes in the energy range 80-300 TeV are studied at the National Gran Sasso Laboratories by means of EAS-TOP (Campo Imperatore, 2005 m a.s.l.) and MACRO (deep underground, 3100 m w.e., the surface energy threshold for a muon reaching the detector being Eμth≈1.3 TeV). The measurement is based on: (a) the selection of primaries based on their energy/nucleon (i.e., with energy/nucleon sufficient to produce a muon with energy larger than 1.3 TeV) and the reconstruction of the shower geometry by means of the muons recorded by MACRO in the deep underground laboratories; (b) the detection of the associated atmospheric Cherenkov light (C.l.) signals by means of the C.l. detector of EAS-TOP. The C.l. density at core distance r>100 m is directly related to the total primary energy E0. Proton and helium ("p + He") and proton, helium and CNO ("p + He + CNO") primaries are thus selected at E0≃80 TeV, and at E0≃250 TeV, respectively. Their flux is measured: Jp+He(80 Tev= (1.8±0.4)×10-6 m-2 s-1 sr-1 TeV-1, and Jp+He+CNO(250 TeV)=(1.1±0.3)×10-7 m-2 s-1 sr-1 TeV-1, their relative weights being: Jp+He/Jp+He+CNO (250 TeV)=0.78±0.17. By using the measurements of the proton spectrum obtained from the direct experiments and hadron flux data in the atmosphere, we obtain for the relative weights of the three components at 250 TeV: Jp:JHe:JCNO =(0.20±0.08): (0.58±0.19):(0.22±0.17). This corresponds to the dominance of helium over proton primaries at 100-1000 TeV, and a possible non-negligible contribution from CNO.The lateral distribution of Cherenkov light in Extensive Air Showers (EASs), which is related to the rate of energy deposit of the primary in the atmosphere, is measured for a selected proton and helium primary beam, and good agreement is found when compared with the one calculated with the CORSIKA/QGSJET simulation model.

KW - Composition

KW - Cosmic rays

KW - Extensive air showers

KW - High energies

KW - Underground muons

UR - https://www.scopus.com/pages/publications/2542483532

U2 - 10.1016/j.astropartphys.2004.01.005

DO - 10.1016/j.astropartphys.2004.01.005

M3 - Article

SN - 0927-6505

VL - 21

SP - 223

EP - 240

JO - Astroparticle Physics

JF - Astroparticle Physics

IS - 3

ER -

The cosmic ray proton, helium and CNO fluxes in the 100 TeV energy region from TeV muons and EAS atmospheric Cherenkov light observations of MACRO and EAS-TOP

Abstract

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