Performance of the NOνA Data Acquisition and Trigger Systems for the full 14 kT Far Detector

Norman, A.; Davies, G. S.; Ding, P. F.; Dukes, E. C.; Duyan, H.; Frank, M. J.; Habig, A.; Henderson, William R.; Niner, E.; Mina, R. A.; Moren, A.; Mualem, L.; Oksuzian, Y.; Rebel, B.; Shanahan, P.; Sheshukov, A.; Tamsett, M. C.; Tomsen, K.; Vinton, L.; Wang, Z.; Zamorano, B.; Zirnstien, J.

doi:10.1088/1742-6596/664/8/082041

Cited by 10 publications

(10 citation statements)

References 5 publications

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“…Even though the electronics is permanently sending data, the high cosmic ray rate in the FD (148 kHz) and the big number of channels means that the volume of data produced is higher than 1 GB/s. To keep the most relevant data, the triggering system uses either i) external signals, ii) periodic (clock) triggers, or iii) the results of real-time algorithms, or"data driven trigger" [41], and builds events of a requested length based on the time stamps of the microslices. For this analysis, we are only interested in the NuMI beam spill signal and the independent minimum-bias cosmic trigger.…”

Section: Near Detector (Nd)mentioning

confidence: 99%

Constraints on neutrino oscillation parameters with the NOvA experiment

Mur

2018

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NOvA is a long-baseline neutrino oscillation experiment, which consists of two finely-segmented liquid-scintillator detectors operating 14 mrad off-axis from the NuMI muon neutrino beam. With an 810 km baseline, the combined measurements of muon neutrino disappearance and electron neutrino appearance allow the determination of neutrino oscillation unknowns, namely the mass hierarchy, the octant of the largest neutrino mixing angle, and the CP violating phase. In this dissertation I present the joint analysis of ν µ → ν µ and ν µ → ν e oscillation data with an exposure of 8.85 × 10 20 protons on target on the 14 kton detector. It includes the estimation of neutrino energy distributions in the far detector using near detector data constraints, details of the implementation of the simultaneous fit of ν µ and ν e samples, and the effect of systematic uncertainties on the measurement of oscillation parameters. I also discuss NOvA's projected sensitivity to determine the mass hierarchy and discover CP violation in future analyses with increased exposure and the addition of antineutrino datasets. With 66 electron neutrino and 126 muon neutrino candidates, the best fit to the data corresponds to the normal mass hierarchy, ∆m 2 32 =2.44×10 −3 eV 2 /c 4 , sin 2 θ 23 = 0.56, and δ CP = 1.21π, with the allowed regions ∆m 2 32 ∈ [2.37, 2.52] × 10 −3 eV 2 /c 4 , sin 2 θ 23 ∈ [0.43, 0.51] ∪ [0.52, 0.60] and δ CP ∈ [0, 0.12π] ∪ [0.91π, 2π] at the 68.3% C.L. Our data disfavor maximal mixing by 0.8σ, δ CP = π/2 in the inverted hierarchy at higher than 3σ, and the entire inverted mass hierarchy at the 95% confidence level. By increasing the size of the samples and adding anti-neutrino data, NOvA can potentially resolve the neutrino mass hierarchy at 4σ C.L. or higher for some combinations of oscillation parameters. Improvements to the sensitivity to the determination of the mass hierarchy and CP violation in the neutrino sector can be achieved through gains in the NuMI beam intensity, the inclusion of external data, and refinements in the analysis methodology.

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Section: Near Detector (Nd)mentioning

confidence: 99%

Constraints on neutrino oscillation parameters with the NOvA experiment

Mur

2018

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“…The remote sense feature can be run in fast, moderate, and slow modes: the moderate setting is used due to the lengths of the cables. 4 Input power to the supplies is single-phase, 240 V, 15 A. The 240 V input was chosen early in the system design in order to allow the 3.5 V and 24 V pods to be run at their maximum power.…”

Section: Low Voltage Power Suppliesmentioning

confidence: 99%

“…The DCMs, powered by 24 V, accumulate 50 µs data fragments into 5 ms blocks from the 2048 cells served by 64 APDs/FEBs. The DCMs then send their data via high-speed switches to a computer farm where the full events are built and, if satisfying trigger criteria, sent to permanent storage [4]. The NOvA power distribution system supplies power to four different electronic components used in the readout: 3.5 V to the front-end boards, 425 V to the avalanche photo-diodes, 24 V to the thermoelectric coolers, and 24 V to the data concentrator modules.…”

Section: Introductionmentioning

confidence: 99%

The NOvA power distribution system

Dukes

Ehrlich

Goadhouse

et al. 2018

Nuclear Instruments and Methods in Physics Research Section A:

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We describe the power distribution systems and grounding schemes built for the near and far detectors of the NOvA long-baseline neutrino experiment. They are used to power the avalanche photodiodes and their thermoelectric coolers, the front-end boards that read out, digitize and time stamp the signals from the avalanche photodiodes, and the data concentrator modules used to receive and format the data from the front-end boards before sending them to a farm of computers used to build the events. The system powers 344,064 readout channels in the far detector and 20,192 channels in the near detector.

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“…These remaining cosmics can be identified as entering events and discarded, while neutrino interactions start well inside the detector volume, for an additional reduction in cosmic background of 10 7 (10 8 for ν e candidates), for a total reduction of > 10 12 . For non-beam physics, a trigger farm examines the data in real time to save interesting data [8]. For example, a burst of neutrinos from a core-collapse supernova in our galaxy would create an increased rate of 10 MeV positrons via inverse beta decay, if we can trigger on this signature [9].…”

Section: Pos(icrc2017)1023mentioning

confidence: 99%