Calibration of the surface array of the Pierre Auger Observatory

M. Aglietta; P. S. Allison; F. Arneodo; D. Barnhill; P. Bauleo; J. J. Beatty; X. Bertou; C. Bonifazi; N. Busca; A. Creusot; D. Dornic; A. Etchegoyen; A. Filevitch; P. L. Ghia; C. M. Grunfeld; I. Lhenry-Yvon; M. C. Medina; E. Moreno; G. Navarra; D. Nitz; T. Ohnuki; S. Ranchon; H. Salazar; T. Suomijärvi; D. Supanitsky; A. Tripathi; M. Urban; L. Villasenor

Calibration of the surface array of the Pierre Auger Observatory

M. Aglietta, P. S. Allison, F. Arneodo, D. Barnhill, P. Bauleo, J. J. Beatty, X. Bertou, C. Bonifazi, N. Busca, A. Creusot, D. Dornic, A. Etchegoyen, A. Filevitch, P. L. Ghia, C. M. Grunfeld, I. Lhenry-Yvon, M. C. Medina, E. Moreno, G. Navarra, D. NitzT. Ohnuki, S. Ranchon, H. Salazar, T. Suomijärvi, D. Supanitsky, A. Tripathi, M. Urban, L. Villasenor

Physics

Research output: Contribution to conference › Paper › peer-review

Abstract

The ground array of the Pierre Auger Observatory will consist of 1600 water Cherenkov detectors, deployed over 3000 km2. The remoteness and large number of detectors required a simple, automatic remote calibration procedure. The primary physics calibration is based on the average charge deposited by a vertical and central throughgoing muon, determined with good precision at the detector via a novel rate-based technique and later with higher precision via charge histograms. This value is named the vertical-equivalent muon (VEM). The VEM and the other parameters needed to maintain this calibration over the full energy range and to assess the quality of the detector are measured every minute. This allows an accurate determination of the energy deposited in each detector when an atmospheric cosmic ray shower occurs.

Original language	English (US)
Pages	279-282
Number of pages	4
State	Published - 2005
Event	29th International Cosmic Ray Conference, ICRC 2005 - Pune, India Duration: Aug 3 2005 → Aug 10 2005

Other

Other	29th International Cosmic Ray Conference, ICRC 2005
Country/Territory	India
City	Pune
Period	8/3/05 → 8/10/05

ASJC Scopus subject areas

Nuclear and High Energy Physics

Cite this

Aglietta, M., Allison, P. S., Arneodo, F., Barnhill, D., Bauleo, P., Beatty, J. J., Bertou, X., Bonifazi, C., Busca, N., Creusot, A., Dornic, D., Etchegoyen, A., Filevitch, A., Ghia, P. L., Grunfeld, C. M., Lhenry-Yvon, I., Medina, M. C., Moreno, E., Navarra, G., ... Villasenor, L. (2005). Calibration of the surface array of the Pierre Auger Observatory. 279-282. Paper presented at 29th International Cosmic Ray Conference, ICRC 2005, Pune, India.

Aglietta, M, Allison, PS, Arneodo, F, Barnhill, D, Bauleo, P, Beatty, JJ, Bertou, X, Bonifazi, C, Busca, N, Creusot, A, Dornic, D, Etchegoyen, A, Filevitch, A, Ghia, PL, Grunfeld, CM, Lhenry-Yvon, I, Medina, MC, Moreno, E, Navarra, G, Nitz, D, Ohnuki, T, Ranchon, S, Salazar, H, Suomijärvi, T, Supanitsky, D, Tripathi, A, Urban, M & Villasenor, L 2005, 'Calibration of the surface array of the Pierre Auger Observatory', Paper presented at 29th International Cosmic Ray Conference, ICRC 2005, Pune, India, 8/3/05 - 8/10/05 pp. 279-282.

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title = "Calibration of the surface array of the Pierre Auger Observatory",

abstract = "The ground array of the Pierre Auger Observatory will consist of 1600 water Cherenkov detectors, deployed over 3000 km2. The remoteness and large number of detectors required a simple, automatic remote calibration procedure. The primary physics calibration is based on the average charge deposited by a vertical and central throughgoing muon, determined with good precision at the detector via a novel rate-based technique and later with higher precision via charge histograms. This value is named the vertical-equivalent muon (VEM). The VEM and the other parameters needed to maintain this calibration over the full energy range and to assess the quality of the detector are measured every minute. This allows an accurate determination of the energy deposited in each detector when an atmospheric cosmic ray shower occurs.",

author = "M. Aglietta and Allison, {P. S.} and F. Arneodo and D. Barnhill and P. Bauleo and Beatty, {J. J.} and X. Bertou and C. Bonifazi and N. Busca and A. Creusot and D. Dornic and A. Etchegoyen and A. Filevitch and Ghia, {P. L.} and Grunfeld, {C. M.} and I. Lhenry-Yvon and Medina, {M. C.} and E. Moreno and G. Navarra and D. Nitz and T. Ohnuki and S. Ranchon and H. Salazar and T. Suomij{\"a}rvi and D. Supanitsky and A. Tripathi and M. Urban and L. Villasenor",

year = "2005",

language = "English (US)",

pages = "279--282",

note = "29th International Cosmic Ray Conference, ICRC 2005 ; Conference date: 03-08-2005 Through 10-08-2005",

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TY - CONF

T1 - Calibration of the surface array of the Pierre Auger Observatory

AU - Aglietta, M.

AU - Allison, P. S.

AU - Arneodo, F.

AU - Barnhill, D.

AU - Bauleo, P.

AU - Beatty, J. J.

AU - Bertou, X.

AU - Bonifazi, C.

AU - Busca, N.

AU - Creusot, A.

AU - Dornic, D.

AU - Etchegoyen, A.

AU - Filevitch, A.

AU - Ghia, P. L.

AU - Grunfeld, C. M.

AU - Lhenry-Yvon, I.

AU - Medina, M. C.

AU - Moreno, E.

AU - Navarra, G.

AU - Nitz, D.

AU - Ohnuki, T.

AU - Ranchon, S.

AU - Salazar, H.

AU - Suomijärvi, T.

AU - Supanitsky, D.

AU - Tripathi, A.

AU - Urban, M.

AU - Villasenor, L.

PY - 2005

Y1 - 2005

N2 - The ground array of the Pierre Auger Observatory will consist of 1600 water Cherenkov detectors, deployed over 3000 km2. The remoteness and large number of detectors required a simple, automatic remote calibration procedure. The primary physics calibration is based on the average charge deposited by a vertical and central throughgoing muon, determined with good precision at the detector via a novel rate-based technique and later with higher precision via charge histograms. This value is named the vertical-equivalent muon (VEM). The VEM and the other parameters needed to maintain this calibration over the full energy range and to assess the quality of the detector are measured every minute. This allows an accurate determination of the energy deposited in each detector when an atmospheric cosmic ray shower occurs.

AB - The ground array of the Pierre Auger Observatory will consist of 1600 water Cherenkov detectors, deployed over 3000 km2. The remoteness and large number of detectors required a simple, automatic remote calibration procedure. The primary physics calibration is based on the average charge deposited by a vertical and central throughgoing muon, determined with good precision at the detector via a novel rate-based technique and later with higher precision via charge histograms. This value is named the vertical-equivalent muon (VEM). The VEM and the other parameters needed to maintain this calibration over the full energy range and to assess the quality of the detector are measured every minute. This allows an accurate determination of the energy deposited in each detector when an atmospheric cosmic ray shower occurs.

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M3 - Paper

AN - SCOPUS:34248353258

SP - 279

EP - 282

T2 - 29th International Cosmic Ray Conference, ICRC 2005

Y2 - 3 August 2005 through 10 August 2005

ER -

Calibration of the surface array of the Pierre Auger Observatory

Abstract

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ASJC Scopus subject areas

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