An accurate evaluation of electron (anti-)neutrino scattering on nucleons

Ricciardi, Giulia; Vignaroli, Natascia; Vissani, Francesco

doi:10.1007/jhep08(2022)212

Cited by 21 publications

(9 citation statements)

References 50 publications

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“…The order of the IBD cross section is 10 −41 cm 2 for the typical SN neutrino energies. SKSNSim includes the calculation by Vogel & Beacom (1999), Strumia & Vissani (2003;default in SKSNSim), and Ricciardi et al (2022). Users can switch between these calculations.…”

Section: ¯¯( )mentioning

confidence: 99%

Supernova Burst and Diffuse Supernova Neutrino Background Simulator for Water Cherenkov Detectors

Nakanishi,

Izumiyama,

Harada

et al. 2024

ApJ

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If a Galactic core-collapse supernova explosion occurs in the future, it will be critical to rapidly alert the community to the direction of the supernova by utilizing neutrino signals in order to enable the initiation of follow-up optical observations. In addition, there is anticipation that observation of the diffuse supernova neutrino background will yield discoveries in the near future, given that experimental upper limits are approaching theoretical predictions. We have developed a new supernova event simulator for water Cherenkov neutrino detectors, such as the highly sensitive Super-Kamiokande. This simulator calculates the neutrino interaction in water for two simulation purposes, individual core-collapse supernova bursts and diffuse supernova neutrino background. Based on this simulator, we can evaluate the precision in determining the location of supernovae and estimate the expected number of events related to the diffuse supernova neutrino background in Super-Kamiokande. In this paper, we describe the basic structure of the simulator and its demonstration.

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Section: ¯¯( )mentioning

confidence: 99%

Supernova Burst and Diffuse Supernova Neutrino Background Simulator for Water Cherenkov Detectors

Nakanishi,

Izumiyama,

Harada

et al. 2024

ApJ

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“…In the low energy range, the main interactions in Super-K are: Since the dominant reaction (about 90% of all events) of supernova neutrinos with water is IBD, we considered only the events produced by IBD in this work. In this work, we have considered the Super-K detection efficiency derived from Equation (4.4) of Ricciardi et al (2022; considering a threshold of 5 MeV). We show this efficiency as a function of energy in Figure 1.…”

Section: Super-kamiokandementioning

confidence: 99%

“…In this paper, rather than numerically simulate the explosion of a supernova, they propose a parameterized expression for the electron antineutrino flux expected at Earth, based on SN 1987A data. By following the methodology described in Section 2 of Vissani (2015) while considering the updated IBD cross section included in Ricciardi et al (2022), we assumed L 10 53 e = n and D = 6.4 Mpc and calculated the expected IBD positron spectrum in Super-K derived from antielectron neutrinos produced by SN 2023ixf. Then, by varying the distance of the supernova and integrating the spectrum in the range [5, 100] MeV, the number of expected events as a function of distance for Super-K has been evaluated.…”

Section: Super-kamiokandementioning

confidence: 99%

Low- and High-energy Neutrinos from SN 2023ixf in M101

Guetta,

Langella,

Gagliardini

et al. 2023

ApJL

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Supernova (SN) 2023ixf in M101 is the closest SN explosion observed in the last decade. Therefore, it is a suitable test bed to study the role of jets in powering the SN ejecta. With this aim, we explored the idea that high-energy neutrinos could be produced during the interaction between the jets and the intense radiation field produced in the SN explosion and eventually be observed by the IceCube neutrino telescope. The lack of detection of such neutrinos has significantly constrained both the fraction of stellar collapses that produce jets and/or the theoretical models for neutrino production. Finally, we investigated the possibility of detecting low-energy neutrinos from SN 2023ixf with the Super- and Hyper-Kamiokande experiments, obtaining, in both cases, subthreshold estimates.

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“…For simplicity and without losing accuracy, we employ the Huber-Mueller flux model here. The total cross-section of the IBD reaction σ tot (E ν ) can be precisely calculated [63][64][65]. The term "⊗G(E e + , σ d )" represents the Gaussian smearing processes to take into account the energy resolution of detector d with resolution σ d .…”

Section: Jhep03(2023)072mentioning

confidence: 99%

Towards a sub-percent precision measurement of sin2 θ13 with reactor antineutrinos

Zhang

Cao

2023

J. High Energ. Phys.

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Measuring the neutrino mixing parameter sin2θ13 to the sub-percent precision level could be necessary in the next ten years for the precision unitary test of the PMNS matrix. In this work, we discuss the possibility of such a measurement with reactor antineutrinos. We find that a single liquid scintillator detector on a reasonable scale could achieve the goal. We propose to install a detector of ∼ 10% energy resolution at about 2.0 km from the reactors with a JUNO-like overburden. The integrated luminosity requirement is about 150 kton · GW · year, corresponding to 4 years’ operation of a 4 kton detector near a reactor complex of 9.2 GW thermal power like Taishan reactor. Unlike the previous θ13 experiments with identical near and far detectors, which can suppress the systematics especially the rate uncertainty by the near-far relative measurement and the optimal baseline is at the first oscillation maximum of about 1.8 km, a single-detector measurement prefers to offset the baseline from the oscillation maximum. At low statistics ≲ 10 kton · GW · year, the rate uncertainty dominates the systematics, and the optimal baseline is about 1.3 km. At higher statistics, the spectral shape uncertainty becomes dominant, and the optimal baseline shifts to about 2.0 km. The optimal baseline keeps being ∼ 2.0 km for an integrated luminosity up to 106 kton · GW · year. Impacts of other factors on the precision sin2θ13 measurement are also discussed. We have assumed that the TAO experiment will improve our understanding of the spectral shape uncertainty, which gives the highest precision measurement of reactor antineutrino spectrum for neutrino energy in the range of 3–6 MeV. We find that the optimal baseline is ∼ 2.9 km with a flat input spectral shape uncertainty provided by the future summation or conversion methods’ prediction. The shape uncertainty would be the bottleneck of the sin2θ13 precision measurement. The sin2θ13 precision is not sensitive to the detector energy resolution and the precision of other oscillation parameters.

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An accurate evaluation of electron (anti-)neutrino scattering on nucleons

Cited by 21 publications

References 50 publications

Supernova Burst and Diffuse Supernova Neutrino Background Simulator for Water Cherenkov Detectors

Supernova Burst and Diffuse Supernova Neutrino Background Simulator for Water Cherenkov Detectors

Low- and High-energy Neutrinos from SN 2023ixf in M101

Towards a sub-percent precision measurement of sin2 θ13 with reactor antineutrinos

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