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. GHIA; C. GRUNFELD; I. LHENRY-YVON; M. C. MEDINA; E. MORENO; G. NAVARRA; D. NITZ; T. OHNUKI; S. RANCHON; H. SALAZAR; T. SUOMIJARVI; D. SUPANITSKY; A. K. TRIPATHI; M. URBAN; L. VILLASENOR

Pune

Conferencia; 29th International Cosmic Ray Conference; 2005

The ground array of the Pierre Auger Observatory will consist of 1600 water Cherenkov detectors, deployed cover 3000 km^2. 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.