Computer-aided design (CAD) model for silicon avalanche Geiger mode systems design: Application to high sensitivity imaging systems

Avalanche Process in Semiconductor Photo Detectors in the Context of the Feedback Theory

“…In other words, the avalanche suppression processes in APD define the multiplication factor. As such requirements correspond to the operation principle by convention Geiger Mode Avalanche Photo Diode (GAPD) [4], the probability interpretation of multiplication coefficient has quite a definite meaning. Namely, as GAPD operates in the region where the field intensity is critical and P~1, the avalanche suppressing should be defined with a certain internal process whose probability should be practically constant to provide for low noise of the detector.…”

The use of silicon photomultipliers for very high energy gamma ray astronomy: the optical issues

“…In recent years, however, an alternative technology based on solid state detectors has emerged [3,4] which has the potential to overcome some of the drawbacks of PMTs, such as their relatively large weight and size, the need for high voltage supplies and their limited quantum efficiency in terms of amplitude and of spectral width. These solid state detectors are based on single APD's and are realized by silicon doped P/N junctions.…”

“…These solid state detectors are based on single APD's and are realized by silicon doped P/N junctions. Their operating principle is rather simple [4,5]. A photon arrives in the depletion region -or space charge region-causes the ejection of an electron from the valence band to the conduction band with the subsequent appearance of an electron / hole pair in the crystal lattice.…”

“…However, these detectors are still too small -from one to three millimeters for commercial MPPC's-to be fully exploited in Imaging Atmospheric Cerenkov Telescope (IACT) experiments. Moreover, they have large and unavoidable dark noise [4], created by photon emissions inside the silicon lattice, which mainly depend on temperature and detector dimensions. For instance, the trigger frequency is typically of the order of 1 MHz/mm 2 , placed in complete darkness with a room temperature of 20 • C. For Cerenkov astronomy, dark noise is absolutely critical because of sky background which can reach several photons per pixel during a two nanoseconds acquisition.…”