Abstract
The Italian National Institute for Nuclear Physics (INFN) is involved in the development of a prototype for a camera based on Silicon Photomultipliers (SiPMs) for the Cherenkov Telescope Array (CTA), a new generation of telescopes for ground-based gamma-ray astronomy. In this framework, an R&D program within the ‘Progetto Premiale TElescopi CHErenkov made in Italy (TECHE.it)’ for the development of SiPMs suitable for Cherenkov light detection in the Near-Ultraviolet (NUV) has been carried out. The developed device is a NUV High-Density (NUV-HD) SiPM based on a micro cell of 30 μ m × 30 μ m and an area of 6 mm × 6 mm, produced by Fondazione Bruno Kessler (FBK). A full characterization of the single NUV-HD SiPM will be presented. A matrix of 8 × 8 single NUV-HD SiPMs will be part of the focal plane of the Schwarzschild- Couder Telescope prototype (pSCT) for CTA. An update on recent tests on the detectors arranged in this matrix configuration and on the front-end electronics will be given.
Highlights
The Italian National Institute for Nuclear Physics (INFN) is involved in the development of a prototype for a camera based on Silicon Photomultipliers (SiPMs) for the Cherenkov Telescope Array (CTA), a new generation of telescopes for ground-based gamma-ray astronomy
Looking at the results shown in the left panel of figure 2, we can conclude that integration times in the interval 50 ns – 75 ns represent a good compromise for obtaining high gains with a good SNR
The right panel of figure 2 shows the gains versus OV calculated for different integration times and using all LEDs
Summary
A systematic study of the SiPM gain and of the first peak signal-to-noise ratio (SNR1) as a function of the integration time. Looking at the results shown in the left panel of figure 2, we can conclude that integration times in the interval 50 ns – 75 ns represent a good compromise for obtaining high gains with a good SNR. The right panel of figure 2 shows the gains versus OV calculated for different integration times and using all LEDs. The average of the slopes obtained for each wavelength is the gain g, expressed in fC/V. Small deviations among wavelengths are seen for long integration times and high biases. This effect is probably due to the fluctuations in the waveform tail.
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