Diffuse supernova neutrinos at underground laboratories

Lunardini, Cecilia

doi:10.1016/j.astropartphys.2016.02.005

Cited by 96 publications

(106 citation statements)

References 178 publications

(432 reference statements)

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“…This conclusion applies to the invisible process, and to any kind of neutrino decay, because it is independent of the neutrino decay products [56]. Likewise, lifetimes up to a similar level would be tested if the diffuse neutrino flux emitted by all past supernovae is measured in the near future [57][58][59].…”

Section: Conclusion and Final Remarksmentioning

confidence: 99%

Constraining the invisible neutrino decay with KM3NeT-ORCA

et al. 2019

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Several theories of particle physics beyond the Standard Model consider that neutrinos can decay. In this work we assume that the standard mechanism of neutrino oscillations is altered by the decay of the heaviest neutrino mass state into a sterile neutrino and, depending on the model, a scalar or a Majoron. We study the sensitivity of the forthcoming KM3NeT-ORCA experiment to this scenario and find that it could improve the current bounds coming from oscillation experiments, where three-neutrino oscillations have been considered, by roughly two orders of magnitude. We also study how the presence of this neutrino decay can affect the determination of the atmospheric oscillation parameters sin 2 θ 23 and ∆m 2 31 , as well as the sensitivity to the neutrino mass ordering.the CP phase δ. These parameters have been measured in solar, reactor, atmospheric and long-baseline accelerator neutrino oscillation experiments. The level of precision reached by current experiments is such that, from the global picture [1-5], neutrino oscillation physics is entering the precision era. However, there are still some unknowns to be established: 1. The true ordering of neutrino masses: we still do not know if the order of the neutrino mass spectrum is normal (NO), where m 3 is the heaviest mass state, or inverted (IO), where m 2 is the heaviest one. Recent oscillation results show a preference for NO [1, 2], although the real neutrino mass ordering is not fully determined yet [6]. 2. The octant of the atmospheric angle: the measured value of sin 2 θ 23 is close to maximal (0.5), but it can be either smaller (lower octant) or larger (upper octant). 3. The exact value of the CP phase δ: values of δ ≈ 0.5π are now highly disfavored, but still a large part of the parameter space remains allowed. At 2σ confidence level, CP might be maximally violated, but also conserved. 4. The absolute scale of neutrino masses: so far there are only upper bounds on it, coming from beta decay experiments and cosmological measurements [7]. 5. The nature of neutrinos: are they Dirac or Majorana particles? In the latter case, there are two extra CP phases to be determined, which are only accessible through neutrinoless double beta decay experiments (see e.g. [8]).The last two points can not be determined by neutrino oscillation experiments, since flavor oscillations are insensitive to the absolute neutrino masses and to the Majorana CP phases. Conversely, the three first issues are expected to be solved by the future long-baseline experiment DUNE, which will measure very well the mass ordering [9] as well as the value of the CPviolating phase and the octant of the atmospheric mixing angle [10] within the standard three-neutrino picture. The determination of the mass ordering of neutrinos is also one of the main physics goals of the future atmospheric experiment ORCA (Oscillation Research with Cosmics in the Abyss) [11], that will provide precise measurements of the atmospheric parameters too. ORCA will be basically an updated version of the ANTARES neutrino...

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Section: Conclusion and Final Remarksmentioning

confidence: 99%

Constraining the invisible neutrino decay with KM3NeT-ORCA

et al. 2019

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“…Barker et al [20] focused on only high-A isotopes (near argon) and Gehman et al [21] considered only isotopes produced by high-energy neutrons. More recently, Franco et al [22] produced a thorough study of spallation backgrounds for low-energy (≤ 1.3 MeV) solar neutrinos, but did not provide the details needed for the higher energies (5)(6)(7)(8)(9)(10)(11)(12)(13)(14)(15)(16)(17)(18)(19)(20) MeV) of DUNE.…”

Section: Introductionmentioning

confidence: 99%

Developing the MeV potential of DUNE: Detailed considerations of muon-induced spallation and other backgrounds

Zhu

Beacom

2019

Phys. Rev. C

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The Deep Underground Neutrino Experiment (DUNE) could be revolutionary for MeV neutrino astrophysics, because of its huge detector volume, unique event reconstruction capabilities, and excellent sensitivity to the νe flavor. However, its backgrounds are not yet known. A major background is expected due to muon spallation of argon, which produces unstable isotopes that later beta decay. We present the first comprehensive study of MeV spallation backgrounds in argon, detailing isotope production mechanisms and decay properties, analyzing beta energy and time distributions, and proposing experimental cuts. We show that above a nominal detection threshold of 5-MeV electron energy, the most important backgrounds are -surprisingly -due to low-A isotopes, such as Li, Be, and B, even though high-A isotopes near argon are abundantly produced. We show that spallation backgrounds can be powerfully rejected by simple cuts, with clear paths for improvements. We compare these background rates to rates of possible MeV astrophysical neutrino signals in DUNE, including solar neutrinos (detailed in a companion paper [Capozzi et al. arXiv:1808.08232 [hepph]]), supernova burst neutrinos, and the diffuse supernova neutrino background. Further, to aid trigger strategies, in the Appendixes we quantify the rates of single and multiple MeV events due to spallation, radiogenic neutron capture, and other backgrounds, including through pileup. Our overall conclusion is that DUNE has high potential for MeV neutrino astrophysics, but reaching this potential requires new experimental initiatives.

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“…On average a SN explodes every second in the Universe and we could detect the cumulative neutrino flux, the DSNB [3,7,8]. The DSNB should be clearly detectable in the region around 20-30 MeV, where it is expected to be above the reactor and atmospheric backgrounds.…”

Section: Diffuse Supernova Neutrino Backgroundmentioning

confidence: 99%

“…The DSNB will allow us to learn about the stellar population, other than provide with an independent test of the SN rate [3,7,8]. In what follows, we will outline some of the open issues in SN and neutrino astrophysics, as well as future directions.…”

Section: Introductionmentioning

confidence: 99%

Supernova Neutrinos: New Challenges and Future Directions

Tamborra¹

2017

J. Phys.: Conf. Ser.

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Abstract. Neutrinos are key particles in core-collapse supernovae. Traveling unimpeded through the stellar core, neutrinos can be direct probes of the still uncertain and fascinating supernova mechanism. Intriguing recent developments on the role of neutrinos during the stellar collapse are reviewed, as well as our current understanding of the flavor conversions in the stellar envelope. The detection perspectives of the next burst will be also outlined.

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Diffuse supernova neutrinos at underground laboratories

Cited by 96 publications

References 178 publications

Constraining the invisible neutrino decay with KM3NeT-ORCA

Constraining the invisible neutrino decay with KM3NeT-ORCA

Developing the MeV potential of DUNE: Detailed considerations of muon-induced spallation and other backgrounds

Supernova Neutrinos: New Challenges and Future Directions

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