Present Status of LVD

Agafonova, N. Yu.; Ashikhmin, V. V.; Dadykin, V. L.; Dobrynina, E. A.; Enikeev, R. I.; Korchaguin, V. B.; Lyashko, I. A.; Malgin, A. S.; Ryasny, V. G.; Ryazhskaya, O. G.; Shakiryanova, I. R.; Talochkin, V. P.; Yakushev, V. F.

doi:10.1142/9789814663618_0020

Cited by 3 publications

(7 citation statements)

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“…At the present, low-energy neutrinos detectors on data-taking, viz. Super Kamiokande [16], LVD [18], Borexino [19] and KamLAND [20] provide all the information needed to perform this study and we report results for these detectors considering both the situation where the detector operates alone and the case in which multiple detectors operate as a network exploiting the advantages of a combined coincident search.…”

Section: Methodsmentioning

confidence: 99%

Pinpointing astrophysical bursts of low-energy neutrinos embedded into the noise

Casentini

Pagliaroli

Vigorito

et al. 2018

J. Cosmol. Astropart. Phys.

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We propose a novel method to increase the probability of identifying impulsive astrophysical bursts of low-energy neutrinos. The proposed approach exploits the temporal structure differences between astrophysical bursts and background fluctuations and it allows us to pinpoint weak signals otherwise unlikely to be detected. With respect to previous search strategies, this method strongly reduces the misidentification probability, e.g. for Super Kamiokande this reduction is a factor of ∼ 9 within a distance of D ∼ 200 kpc without decreasing the detection efficiency. In addition, we extend the proposed method to a network of different detectors and we show that the Kamland & LVD background reduction is improved by a factor ∼ 20 up to an horizon of D ∼ 75 kpc.

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Section: Methodsmentioning

confidence: 99%

Pinpointing astrophysical bursts of low-energy neutrinos embedded into the noise

Casentini

Pagliaroli

Vigorito

et al. 2018

J. Cosmol. Astropart. Phys.

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“…LVD is a 1000 t liquid scintillator instrument aimed at detecting neutrinos from core collapse supernovae [37]. Given its goal, one of its essential features is its modularity: it consists of an array of 840 scintillator counters, organised in sub-sectors that can take data independently one from another.…”

Section: The Muon Data Setmentioning

confidence: 99%

“…A detailed description of the instrument is given in [37]: we recall here the main characteristics related to the selection of muons in the scintillator detector 1 . Each 1.5 m 3 scintillator counter is viewed from the top by three photomultipliers (PMTs).…”

Section: The Muon Data Setmentioning

confidence: 99%

“…MeV, within 175 ns, in two or more counters (this time width is chosen to take into account for the jitter of the PMT's transit time). We apply to individual counters the same quality cuts that have been described in [37], based on checks of their counting rate and energy spectrum. The average rate of muons crossing LVD is monitored and it is 0.097 ± 0.010 s −1 , the mean per counter being f µ (c) ∼ 50 d −1 .…”

Section: The Muon Data Setmentioning

confidence: 99%

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Characterization of the varying flux of atmospheric muons measured with the Large Volume Detector for 24 years

Agafonova¹,

Aglietta²,

Antonioli³

et al. 2019

Phys. Rev. D

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The Large Volume Detector (LVD), hosted in the INFN Laboratori Nazionali del Gran Sasso, is triggered by atmospheric muons at a rate of ∼ 0.1 Hz. The data collected over almost a quarter of century are used to study the muon intensity underground. The 50-million muon series, the longest ever exploited by an underground instrument, allows for the accurate longterm monitoring of the muon intensity underground. This is relevant as a study of the background in the Gran Sasso Laboratory, which hosts a variety of long-duration, low-background detectors. We describe the procedure to select muon-like events as well as the method used to compute the exposure. We report the value of the average muon flux measured from 1994 to 2017: I 0 µ = 3.35 ± 0.0005 stat ± 0.03 sys · 10 −4 m −2 s −1 . We show that the intensity is modulated around this average value due to temperature variations in the stratosphere. We quantify such a correlation by using temperature data from the European Center for Medium-range Weather Forecasts:we find an effective temperature coefficient α T = 0.94 ± 0.01 stat ± 0.01 sys , in agreement with other measurements at the same depth. We scrutinise the spectral content of the time series of the muon intensity by means of the Lomb-Scargle analysis. This yields the evidence of a 1-year periodicity, as well as the indication of others, both shorter and longer, suggesting that the series is not a pure sinusoidal wave. Consequently, and for the first time, we characterise the observed modulation in terms of amplitude and position of maximum and minimum on a year-by-year basis.When high-energy cosmic rays enter the atmosphere, they produce a large number of secondary particles, in a series of successive interactions with atmospheric nuclei, called extensive air showers (EAS). EAS particles produced in the upper atmosphere propagate longitudinally through the atmosphere: at ground level, the most abundant among them are muons, which are produced in the decay of short-lived mesons, namely charged pions and kaons. Thanks to their small energy loss, small cross-section and long lifetime, higher energy (above ∼ 1 TeV) muons can penetrate deeply underground. Thus, large acceptance instruments located underground, originally designed for, e.g., neutrino or proton decay studies, all have excellent capabilities for the study of high energy atmospheric muons.The Large Volume Detector (LVD) [1], located in the INFN Laboratori Nazionali del Gran Sasso (LNGS) at a minimal depth of 3100 m w.e., is one of such detectors. Despite the large amount of overhead rock, LVD is triggered by atmospheric muons at a rate of ∼ 0.1 Hz.Underground muons are exploited for a variety of physics analyses, most notably for the measurement of the flux and the composition of Galactic cosmic rays (see e.g., [2] and [3]) as well as for the search for anisotropies (see [4], [5] and [6]). Also, the study of muons underground allows for the measurement of the high-energy part (above 1 TeV) of the sea-level muon energy spectrum through the depth-intens...

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“…Neutrino observatories often exploit nuclei to detect astrophysical neutrinos. Scintillator detectors such as JUNO [35] use carbon, water Cherenkov like Super-Kamiokande or the future Hyper-Kamiokande use oxygen, LVD has iron nuclei [37], DUNE is based on argon [50] and the HALO observatory uses lead [39]. The SNEWS network of observatories is ready to observe a future core-collapse supernova explosion [40].…”

Section: Observational Aspects and Nuclear Physicsmentioning

confidence: 99%

Neutrino astrophysics and its connections to nuclear physics

Volpe

2018

J. Phys.: Conf. Ser.

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We highlight recent developments in neutrino astrophysics. We discuss some of the connections with nuclear physics. Milestones in neutrino astrophysicsNeutrino astronomy started with the pioneering measurement of solar neutrinos by R. Davis' experiment in the sixties [1] and the observation of neutrinos from the supernova 1987A located in the Large Magellanic Cloud by Kamiokande II [2], by IMB [3] and Baksan [4]. Evidence of ultra-high energy neutrinos in the PeV energy range by the ICECUBE Collaboration has initiated high energy neutrino astronomy [5]. Moreover, the measurements of gravitational waves from binary black holes [6] and neutron star mergers [7] has opened the era of multi-messenger astronomy.Neutrinos are elementary massive particles with mixings. This is known since the discovery of vacuum oscillation by the Super-Kamiokande experiment [8], that had an impact in particle physics, astrophysics and cosmology. This phenomenon occurs because the mass or propagation basis and the flavor or interaction basis do not coincide. They are related by the Pontecorvo-Maki-Nakagawa-Sakata unitary matrix [9] which depends on three mixing angles, one Dirac and two Majorana phases, if there exists only three active neutrino flavors. If neutrinos are Dirac particles, the neutrino mass can be implemented by adding a right-handed singlet to the Glashow-Weinberg-Salam model. If neutrinos are Majorana particles, significant extensions to the standard model are necessary that produce total lepton number violation (see e.g. the book [10]).First identified by R. Davis' experiment, the solar neutrino deficit problem has been solved with the neutrino oscillation discovery [8], the SNO measurement of the total solar neutrino flux in agreement with expectations from the Standard Solar Model [11] and with the identification of the Large-Mixing-Angle (LMA) solution by KamLAND [12] (see e.g.[13] for a review). In particular, the production of solar neutrinos and their flavor conversion are well understood. Historically, the study of solar ν has played a major role in establishing how energy is produced in low mass main sequence stars, as our Sun, and in ascertaining neutrino flavor conversion. The precise measurement of neutrinos coming from the Sun's interior have confirmed that the protonproton (pp) reaction chain, that burns hydrogen to produce helium-4 nuclei, is responsible for 99% of energy production in the Sun [15]. The (hopefully) future measurement of neutrinos

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Present Status of LVD

Cited by 3 publications

References 0 publications

Pinpointing astrophysical bursts of low-energy neutrinos embedded into the noise

Pinpointing astrophysical bursts of low-energy neutrinos embedded into the noise

Characterization of the varying flux of atmospheric muons measured with the Large Volume Detector for 24 years

Neutrino astrophysics and its connections to nuclear physics

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