Nuisances of SiPMs and how to deal with them in ... - KICP Workshops

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... or shape output signal with high pass 3x3 mm 2 MPPC before Pole zero cancellation not really needed 3 kΩ ~24 pF Nepomuk Otte 50 Ω after Use input impedance of next stage 18
Temperature Dependencies Critical E-field for breakdown depends on temperature Temperature dependent breakdown voltage Temperature dependent gain and PDE Intrinsic dark rates are high but not an issue for Cherenkov telescopes NSB rates are generally higher -> no cooling needed For example in the SCT we expect ~40 MHz NSB in a 6x6 mm 2 pixel -> about 1 MHz NSB per mm 2 sensor area Compare to typical intrinsic dark rates of MPPCs of a few 100 kHz per mm 2 Nepomuk Otte 19
Page 1 and 2: Nuisances of SiPMs and how to deal
Page 3 and 4: CTA-US SC telescope Schwarzschild C
Page 5 and 6: Module Conceptional Design Cold fin
Page 7 and 8: Night Sky Background Light From sta
Page 9 and 10: Intensities are not to scale Nepomu
Page 11 and 12: P(n) = λ n /n! exp(-λ) Non-Poisso
Page 13 and 14: Operational Requirements Purpose of
Page 15 and 16: Output signals
Page 17: Faster output pulses by adding one
Page 21 and 22: PDE Different effects contribute to
Page 23 and 24: Conceptual Design Primary goal for
Page 25 and 26: Photon Emission during Breakdown Av
Page 27 and 28: Non-Poisson tails due to optical cr
Page 29 and 30: Dependency of gain on NSB rate Larg

Nuisances of SiPMs and how to deal with them in ... - KICP Workshops

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