Author/Authors :
Argirٍ، نويسنده , , S and Camin، نويسنده , , D.V and Cattaneo، نويسنده , , P and Destro، نويسنده , , M and Fonte، نويسنده , , R and Gariboldi، نويسنده , , R and Grassi، نويسنده , , V and Lapolla، نويسنده , , M and Manfredi، نويسنده , , P.F and Menichetti، نويسنده , , E and Nicotra، نويسنده , , M and Privitera، نويسنده , , P and Ratti، نويسنده , , L and Re، نويسنده , , V and Speziali، نويسنده , , V and Trapani، نويسنده , , P، نويسنده ,
Abstract :
The Auger Fluorescence Detector will allow to determine the longitudinal development of atmospheric showers in the range 1019–1021 eV. A detector module comprises an array of 20×22 PMTs at the focal surface of a large-aperture telescope. Thirty such modules will be used. The PMTs pixel signal is variable in shape depending on the shower-eye geometry. The sky background light (BL) is also variable. We have developed an analog signal processor to obtain best energy and timing resolution despite those constrains. The Head Electronics (HE) bias the PMTs and keeps its pulse-gain constant even for large BL. This is measured using a current-monitor of novel design. Both the signal pulse and the BL DC level are sent via a single twisted pair to the Analog Board (AB). The AB performs the compression of the 15–16 bit signal dynamic range into 12 bits of the FADC which follows the AB. A three-pole Bessel filter was adopted for antialiasing. The AB includes 16 bit sigma-delta chips to readout the BL DC level, and a test-pulse distribution system.
