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Figure 8: (a) The noise rate for all the SiPMs at 0.5 pe threshold for V,,,=3 V, (b) Correlation plot of noise rate (at 1.5 pe threshold) versus dG/dV and (c) Correlation plot of noise rate (at 1.5 pe) versus dG/dV Figure 8: (a) The noise rate for all the SiPMs at 0.5 pe threshold for V,,,=3 V, (b) Correlation plot of noise Vpr respectively, but it is clear that there is no correlation of noise rate with dG/dV and Vp,.

Figure 8 (a) The noise rate for all the SiPMs at 0.5 pe threshold for V,,,=3 V, (b) Correlation plot of noise rate (at 1.5 pe threshold) versus dG/dV and (c) Correlation plot of noise rate (at 1.5 pe) versus dG/dV Figure 8: (a) The noise rate for all the SiPMs at 0.5 pe threshold for V,,,=3 V, (b) Correlation plot of noise Vpr respectively, but it is clear that there is no correlation of noise rate with dG/dV and Vp,.

Related Figures (6)

Figure 1: A schematic of the Cosmic Muon Veto Detector around mini-ICAL The flux of the cosmic ray muons on the earth’s surface constitutes a huge background for the experiments searching for the rare neutrino interactions. The cosmic muon flux reduces by a factor of 10° against a depth of ~ 1 km and 10? against shallow depth of ~ 100m. An active cosmic muon veto (CMV) detector with veto efficiency >99.99% will be required for a rejection factor of 10° at depth of 100m. The prototype of Iron CALorimeter (ICAL) i.e. mini-ICAL, consists of 11 layers of 5.6 cm thick soft iron plates and 10 layers of 2m x 2m glass Resistive Plate Chambers (RPCs), an 85-ton magnet and is operational at Madurai, India. A CMV detector is being built on top of mini-ICAL (as shown in Fig. 1) with extruded plastic scintillators with embedded WLS fibres to propagate light and SiPM to detect scintillation photons. The SiPM model S13360-2050VE from Hamamatsu is used for CMVD experiment. This particular model of SiPM has a total photosensitive area of 2mmx2 mm, 1584 microcells, microcell pitch of 50 um, fill factor of 74%, Vz, of (53 + 5) V at room temperature. The SiPMs are available on panels, with each panel containing 16 SiPMs, as shown in Fig. 2. the faces of the black box as shown in the Fig. 3. An ultrafast LED driver (CAEN SP5601) is used
Figure 1: A schematic of the Cosmic Muon Veto Detector around mini-ICAL The flux of the cosmic ray muons on the earth’s surface constitutes a huge background for the experiments searching for the rare neutrino interactions. The cosmic muon flux reduces by a factor of 10° against a depth of ~ 1 km and 10? against shallow depth of ~ 100m. An active cosmic muon veto (CMV) detector with veto efficiency >99.99% will be required for a rejection factor of 10° at depth of 100m. The prototype of Iron CALorimeter (ICAL) i.e. mini-ICAL, consists of 11 layers of 5.6 cm thick soft iron plates and 10 layers of 2m x 2m glass Resistive Plate Chambers (RPCs), an 85-ton magnet and is operational at Madurai, India. A CMV detector is being built on top of mini-ICAL (as shown in Fig. 1) with extruded plastic scintillators with embedded WLS fibres to propagate light and SiPM to detect scintillation photons. The SiPM model S13360-2050VE from Hamamatsu is used for CMVD experiment. This particular model of SiPM has a total photosensitive area of 2mmx2 mm, 1584 microcells, microcell pitch of 50 um, fill factor of 74%, Vz, of (53 + 5) V at room temperature. The SiPMs are available on panels, with each panel containing 16 SiPMs, as shown in Fig. 2. the faces of the black box as shown in the Fig. 3. An ultrafast LED driver (CAEN SP5601) is used
Figure 3: The SiPM mass testing experimental setup
Figure 3: The SiPM mass testing experimental setup
Figure 5: (a) Raw SiPM signal, (b) Charge distribution at Vig, =54 V and (c) Calibration plot for measuring Vp- and dG/dV for one of the SiPMs. The total collected charge is fitted with a function [1]:
Figure 5: (a) Raw SiPM signal, (b) Charge distribution at Vig, =54 V and (c) Calibration plot for measuring Vp- and dG/dV for one of the SiPMs. The total collected charge is fitted with a function [1]:
Figure 6: (a) The variation in the gain with respect to bias voltage (dG/dV) versus SiPM number and (b) Vp, versus SiPM number at room temperature (25 ° C). to the slope will determine V,, and both the parameters are estimated for each of these SiPMs as
Figure 6: (a) The variation in the gain with respect to bias voltage (dG/dV) versus SiPM number and (b) Vp, versus SiPM number at room temperature (25 ° C). to the slope will determine V,, and both the parameters are estimated for each of these SiPMs as
Figure 7: (a) The integerated charge distribution from the noise data at different V,, and (b) Variation in the noise rate at different g;;, for different V,,,
Figure 7: (a) The integerated charge distribution from the noise data at different V,, and (b) Variation in the noise rate at different g;;, for different V,,,
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