3d Straight Shota 30
LINK ::: https://urlin.us/2td5sr
The Sagitta detectors of the Pierre Auger Observatory, the largest cosmic-ray instrument, have recently seen the culmination of years of effort and multiple funding cycles. The results presented here give an overview of the overall performance characteristics of the detector.
The detector technologies used in the two components of the detector are discussed. The individual sensors are critically analyzed with respect to dynodes used, signal amplifiers, pulse shaping filters, and power supplies. The results on the timing properties of the wires of the array are presented. The cross calibration of the two components of the detector is discussed. Finally, the resolution of the individual sensors is shown by using track-finding efficiencies, and it is shown that this can be used to distinguish reconstructed tracks from noise of different origins. The statistical aspects of the analysis are mentioned, particularly with respect to the very large data base obtained while the detectors were operating in 2004-2006. A Conclusion is given, and the prospects for future work within the Pierre Auger Observatory are discussed.« less
Ionizing radiation, caused by either solar or cosmic rays, is the most likely source of the damage that has been observed in the detectors of the Pierre Auger Observatory. To completely eliminate the contribution of solar radiation, the Observatory is located in 4100 m altitude, the edge of the earth's atmosphere, at 54.5°S. For cosmic rays, the atmosphere reduces the number of particles that reach the ground by a factor of one million/km, but the particles that do reach the ground can be much more energetic than the particles of galactic cosmic rays. At this altitude, the median energy of the particles entering a sensor is about 5 GeV. The Pierre Auger Collaboration has recently completed the most advanced study of the energy deposition by cosmic rays in a detector that can be operated at high altitudes, the Surface Detector (SD) in its version 30. The energy deposited in the crystals is related to the charge produced in the pixels, allowing particle detection not only in the SD, but also in the fluorescence lights of the Surface Detector Array (SDA), where the energy deposit in the scintillator is related to the energy loss in the tracking chambers (in these latter both Auger experiments are using a combination of optical and hadronic tracking). d2c66b5586