AMIGA, Auger Muons and Infill for the Ground Array

A. ETCHEGOYEN, FOR THE PIERRE AUGER COLLABORATION. (VER F. SUAREZ EN LISTA AUTORES ICRC2007 HTTP://WWW.AUGER.ORG/AUGER-AUTHORS.PDF)

Merida, Mexico.

Conferencia; 30th International Cosmic Ray Conference, ICRC2007; 2007

The Pierre Auger Observatory is planned to be upgraded so that the energy spectrum of cosmic rays can be studied down to 0.1EeV and the muon component of showers can be determined. The former will lead to a spectrum measured by one technique from 0.1 EeV to beyond 100EeV while the latter will aid identification of the primary particles. These enhancements consist of three high elevation telescopes (HEAT) and an infilled are a having both surface detectors and underground muon counters (AMIGA). The surface array of the Auger Observatory will be enhanced over a 23.5km2 area by 85 detector pairs laidout as a graded array of water-Cherenkov detectors and 30m2 buried muon scintillator counters. The spacings in the array will be 433 and 750m. The muon detectors will comprise highly segmented scintillators with optical fibres ending on multi-anode phototubes. The AMIGA complex will be centred 6.0km away from the fluorescence detector installation at Coihueco and will be overlooked by the HEAT telescopes. We describe the design features of the AMIGA enhancement.