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The Kamioka Liquid Scintillator Antineutrino Detector (KamLAND) is an electron antineutrino detector at the Kamioka Observatory, an underground neutrino detection facility in Hida, Gifu, Japan. The device is situated in a drift mine shaft in the old KamiokaNDE cavity in the Japanese Alps. The site is surrounded by 53 Japanese commercial nuclear reactors. Nuclear reactors produce electron antineutrinos ( \( {\bar {\nu }}_{e} \) ) during the decay of radioactive fission products in the nuclear fuel. Like the intensity of light from a light bulb or a distant star, the isotropically-emitted \( {\bar {\nu }}_{e} \) flux decreases at 1/R2 per increasing distance R from the reactor. The device is sensitive up to an estimated 25% of antineutrinos from nuclear reactors that exceed the threshold energy of 1.8 megaelectronvolts (MeV) and thus produces a signal in the detector.

If neutrinos have mass, they may oscillate into flavors that an experiment may not detect, leading to a further dimming, or "disappearance," of the electron antineutrinos. KamLAND is located at an average flux-weighted distance of approximately 180 kilometers from the reactors, which makes it sensitive to the mixing of neutrinos associated with large mixing angle (LMA) solutions to the solar neutrino problem.

KamLAND Detector

The KamLAND detector's outer layer consists of an 18 meter-diameter stainless steel containment vessel with an inner lining of 1,879 photo-multiplier tubes (1325 17" and 554 20" PMTs).[2] Photocathode coverage is 34%. Its second, inner layer consists of a 13 m-diameter nylon balloon filled with a liquid scintillator composed of 1,000 metric tons of mineral oil, benzene, and fluorescent chemicals. Non-scintillating, highly purified oil provides buoyancy for the balloon and acts as a buffer to keep the balloon away from the photo-multiplier tubes; the oil also shields against external radiation. A 3.2 kiloton cylindrical water Cherenkov detector surrounds the containment vessel, acting as a muon veto counter and providing shielding from cosmic rays and radioactivity from the surrounding rock.

Electron antineutrinos (νe) are detected through the Inverse beta decay reaction \( {\bar {\nu }}_{e}+p\to e^{+}+n \) , which has a 1.8 MeV \( {\bar {\nu }}_{e} \) energy threshold. The prompt scintillation light from the positron ( \( {\displaystyle e^{+}} \) ) gives an estimate of the incident antineutrino energy, \( {\displaystyle E_{\nu }=E_{prompt}+<E_{n}>+0.9MeV}, \) where \( {\displaystyle E_{prompt}} \) is the prompt event energy including the positron kinetic energy and the \( {\displaystyle e^{+}e^{-}} \) annihilation energy. The quantity < \( E_{n} \) > is the average neutron recoil energy, which is only a few tens of kiloelectronvolts (keV). The neutron is captured on hydrogen approximately 200 microseconds (μs) later, emitting a characteristic 2.2 MeV
γ
ray. This delayed-coincidence signature is a very powerful tool for distinguishing antineutrinos from backgrounds produced by other particles.

To compensate for the loss in ν ¯ e {\displaystyle {\bar {\nu }}_{e}} {\bar {\nu }}_{e} flux due to the long baseline, KamLAND has a much larger detection volume compared to earlier devices. The KamLAND detector uses a 1,000-metric-ton detection mass, which is over twice the size of similar detectors, such as Borexino. However, the increased volume of the detector also demands more shielding from cosmic rays, requiring the detector be placed underground.

As part of the Kamland-Zen double beta decay search, a balloon of scintillator with 320 kg of dissolved xenon was suspended in the center of the detector in 2011.[3] A cleaner rebuilt balloon is planned with additional xenon. KamLAND-PICO is a planned project that will install the PICO-LON detector in KamLand to search for dark matter. PICO-LON is a radiopure NaI(Tl) crystal that observes inelastic WIMP-nucleus scattering.[4] Improvements to the detector are planned, adding light collecting mirrors and PMTs with higher quantum efficiency.
Results
Neutrino oscillation

KamLAND started to collect data on January 17, 2002. First results were reported using only 145 days of data.[5] Without neutrino oscillation, 86.8±5.6 events were expected, however, only 54 events were observed. KamLAND confirmed this result with a 515-day data sample,[6] 365.2 events were predicted in the absence of oscillation, and 258 events were observed. These results established antineutrino disappearance at high significance.

The KamLAND detector not only counts the antineutrino rate, but also measures their energy. The shape of this energy spectrum carries additional information that can be used to investigate neutrino oscillation hypotheses. Statistical analyses in 2005 show the spectrum distortion is inconsistent with the no-oscillation hypothesis and two alternative disappearance mechanisms, namely the neutrino decay and de-coherence models. It is consistent with 2-neutrino oscillation and a fit provides the values for the Δm2 and θ parameters. Since KamLAND measures \( \Delta {m^{2} \) most precisely and the solar experiments exceed KamLAND's ability to measure θ, the most precise oscillation parameters are obtained in combination with solar results. Such a combined fit gives \( {\displaystyle \Delta {m^{2}}=7.9_{-0.5}^{+0.6}\cdot 10^{-5}{\text{eV}}^{2}} \) and \( {\displaystyle \tan ^{2}\theta =0.40_{-0.07}^{+0.10}} \) , the best neutrino oscillation parameter determination to that date. Since then a 3 neutrino model has been used.

Precision combined measurements were reported in 2008[7] and 2011:[8]

\( {\displaystyle \Delta m_{21}^{2}=7.59\pm 0.21\cdot 10^{-5}\,{\text{eV}}^{2},\,\,\tan ^{2}\theta _{12}=0.47_{-0.05}^{+0.06}} \)

Geological antineutrinos (geoneutrinos)

KamLAND also published an investigation of geologically-produced antineutrinos (so-called geoneutrinos) in 2005. These neutrinos are produced in the decay of thorium and uranium in the Earth's crust and mantle.[9] A few geoneutrinos were detected and these limited data were used to limit the U/Th radiopower to under 60TW.

Combination results with Borexino were published in 2011,[10] measuring the U/Th heat flux.

New results in 2013, benefiting from the reduced backgrounds due to Japanese reactor shutdowns, were able to constrain U/Th radiogenic heat production to \( {\displaystyle 11.2_{-5.1}^{+7.9}} \) TW [11] using 116 \( {\bar {\nu }}_{e} \) events. This constrains composition models of the bulk silicate Earth and agrees with the reference Earth model.
KamLAND-Zen Double Beta Decay Search

KamLAND-Zen uses the detector to study beta decay of 136Xe from a balloon placed in the scintillator in summer 2011. Observations set a limit for neutrinoless double-beta decay half-life of 1.9×1025 yr.[12] A double beta decay lifetime was also measured: \( {\displaystyle 2.38\pm {0.02(\mathrm {stat} )}\pm {0.14(\mathrm {syst} )}*10^{21}} \) yr, consistent with other xenon studies.[3] KamLAND-Zen plans continued observations with more enriched Xe and improved detector components.

An improved search was published in August 2016, increasing the half-life limit to 1.07×1026 yr, with a neutrino mass bound of 61–165 meV.[13]

The first KamLAND-Zen apparatus, KamLAND-Zen 400, has as of 2018 completed two research programs, Phase I (2011 Oct. - 2012 Jun.) and Phase II (2013 Dec. - 2015 Oct.). The combined data of Phase I and II implied the lower bound \( {\displaystyle 1.07\times 10^{26}} \) years for the neutrinoless double beta decay half-life.

The second KamLAND-Zen experiment apparatus, KamLAND-Zen 800, with bigger balloon of about 750kg of Xenon was installed in the KamLAND detector 10 May 2018. The operation is expected to start winter 2018-2019 with 5 years of expected operation.[14]

The KamLAND-Zen collaboration is planning to construct another apparatus, KamLAND2-Zen in the long term.
References

Iwamoto, Toshiyuki (February 2003), Measurement of Reactor Anti-Neutrino Disappearance in KamLAND (PDF) (Ph.D. thesis), Tohoku University, archived from the original (PDF) on 2014-10-06
Suzuki, Atsuto; Collaboration, KamLand (2005-01-01). "Results from KamLAND Reactor Neutrino Detection". Physica Scripta. 2005 (T121): 33. Bibcode:2005PhST..121...33S. doi:10.1088/0031-8949/2005/T121/004. ISSN 1402-4896.
Gando, A.; et al. (KamLAND-Zen Collaboration) (19 April 2012). "Measurement of the double-β decay half-life of 136Xe with the KamLAND-Zen experiment". Physical Review C. 85 (4): 045504.arXiv:1201.4664. Bibcode:2012PhRvC..85d5504G. doi:10.1103/PhysRevC.85.045504.
Fushimi, K; et al. (2013). "PICO-LON Dark Matter Search". Journal of Physics: Conference Series. 469 (1): 012011. Bibcode:2013JPhCS.469a2011F. doi:10.1088/1742-6596/469/1/012011.
Eguchi, K.; et al. (KamLAND Collaboration) (2003). "First results from KamLAND: evidence for reactor antineutrino disappearance". Physical Review Letters. 90 (2): 021802–021807.arXiv:hep-ex/0212021. Bibcode:2003PhRvL..90b1802E. doi:10.1103/PhysRevLett.90.021802. PMID 12570536.
Araki, T.; et al. (KamLAND Collaboration) (2005). "Measurement of neutrino oscillation with KamLAND: evidence of spectral distortion". Physical Review Letters. 94 (8): 081801–081806.arXiv:hep-ex/0406035. Bibcode:2005PhRvL..94h1801A. doi:10.1103/PhysRevLett.94.081801. PMID 15783875.
Abe, S.; et al. (KamLAND Collaboration) (5 Jun 2008). "Precision Measurement of Neutrino Oscillation Parameters with KamLAND". Physical Review Letters. 100 (22): 221803.arXiv:0801.4589. Bibcode:2008PhRvL.100v1803A. doi:10.1103/PhysRevLett.100.221803. PMID 18643415.
Gando, A.; et al. (2011). "Constraints on θ13 from A Three-Flavor Oscillation Analysis of Reactor Antineutrinos at KamLAND". Physical Review D. 83 (5): 052002.arXiv:1009.4771. Bibcode:2011PhRvD..83e2002G. doi:10.1103/PhysRevD.83.052002.
Araki, T.; et al. (KamLAND Collaboration) (2005). "Experimental investigation of geologically produced antineutrinos with KamLAND". Nature. 436 (7050): 499–503. Bibcode:2005Natur.436..499A. doi:10.1038/nature03980. PMID 16049478.
Gando, A.; et al. (KamLAND Collaboration) (17 July 2011). "Partial radiogenic heat model for Earth revealed by geoneutrino measurements" (PDF). Nature Geoscience. 4 (9): 647–651. Bibcode:2011NatGe...4..647K. doi:10.1038/ngeo1205.
A. Gando et al. (KamLAND Collaboration) (2 August 2013). "Reactor on-off antineutrino measurement with KamLAND". Physical Review D. 88 (3): 033001.arXiv:1303.4667. Bibcode:2013PhRvD..88c3001G. doi:10.1103/PhysRevD.88.033001.
Gando, A.; et al. (KamLAND-Zen Collaboration) (7 February 2013). "Limit on Neutrinoless ββ Decay of 136Xe from the First Phase of KamLAND-Zen and Comparison with the Positive Claim in 76Ge". Physical Review Letters. 110 (6): 062502.arXiv:1211.3863. Bibcode:2013PhRvL.110f2502G. doi:10.1103/PhysRevLett.110.062502. PMID 23432237.
Gando, A.; et al. (KamLAND-Zen Collaboration) (16 August 2016). "Search for Majorana Neutrinos Near the Inverted Mass Hierarchy Region with KamLAND-Zen". Physical Review Letters. 117 (8): 082503.arXiv:1605.02889. Bibcode:2016PhRvL.117h2503G. doi:10.1103/PhysRevLett.117.082503. PMID 27588852.

http://www.ba.infn.it/~now/now2018/assets/yoshihitogandonow2018.pdf

Further reading

Abe, S; et al. (KamLAND Collaboration) (2008). "Precision Measurement of Neutrino Oscillation Parameters with KamLAND". Physical Review Letters. 100 (22): 221803.arXiv:0801.4589. Bibcode:2008PhRvL.100v1803A. doi:10.1103/PhysRevLett.100.221803. PMID 18643415.
Eguchi, K; et al. (KamLAND Collaboration) (2004). "High sensitivity search for
ν
e's from the sun and other sources at KamLAND". Physical Review Letters. 92 (7): 071301–071305.arXiv:hep-ex/0310047. Bibcode:2004PhRvL..92g1301E. doi:10.1103/PhysRevLett.92.071301. PMID 14995837.

External links

KamLAND official website
KamLAND at Lawrence Berkeley National Laboratory (Berkeley Lab)

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Breakthrough Prize laureates
Mathematics

Simon Donaldson, Maxim Kontsevich, Jacob Lurie, Terence Tao and Richard Taylor (2015) Ian Agol (2016) Jean Bourgain (2017) Christopher Hacon, James McKernan (2018) Vincent Lafforgue (2019) Alex Eskin (2020) Martin Hairer (2021)

Fundamental physics

Nima Arkani-Hamed, Alan Guth, Alexei Kitaev, Maxim Kontsevich, Andrei Linde, Juan Maldacena, Nathan Seiberg, Ashoke Sen, Edward Witten (2012) Special: Stephen Hawking, Peter Jenni, Fabiola Gianotti (ATLAS), Michel Della Negra, Tejinder Virdee, Guido Tonelli, Joseph Incandela (CMS) and Lyn Evans (LHC) (2013) Alexander Polyakov (2013) Michael Green and John Henry Schwarz (2014) Saul Perlmutter and members of the Supernova Cosmology Project; Brian Schmidt, Adam Riess and members of the High-Z Supernova Team (2015) Special: Ronald Drever, Kip Thorne, Rainer Weiss and contributors to LIGO project (2016) Yifang Wang, Kam-Biu Luk and the Daya Bay team, Atsuto Suzuki and the KamLAND team, Kōichirō Nishikawa and the K2K / T2K team, Arthur B. McDonald and the Sudbury Neutrino Observatory team, Takaaki Kajita and Yōichirō Suzuki and the Super-Kamiokande team (2016) Joseph Polchinski, Andrew Strominger, Cumrun Vafa (2017) Charles L. Bennett, Gary Hinshaw, Norman Jarosik, Lyman Page Jr., David Spergel (2018) Special: Jocelyn Bell Burnell (2018) Charles Kane and Eugene Mele (2019) Special: Sergio Ferrara, Daniel Z. Freedman, Peter van Nieuwenhuizen (2019) The Event Horizon Telescope Collaboration (2020) Eric Adelberger, Jens H. Gundlach and Blayne Heckel (2021) Special: Steven Weinberg (2021)

Life sciences

Cornelia Bargmann, David Botstein, Lewis C. Cantley, Hans Clevers, Titia de Lange, Napoleone Ferrara, Eric Lander, Charles Sawyers, Robert Weinberg, Shinya Yamanaka and Bert Vogelstein (2013) James P. Allison, Mahlon DeLong, Michael N. Hall, Robert S. Langer, Richard P. Lifton and Alexander Varshavsky (2014) Alim Louis Benabid, Charles David Allis, Victor Ambros, Gary Ruvkun, Jennifer Doudna and Emmanuelle Charpentier (2015) Edward Boyden, Karl Deisseroth, John Hardy, Helen Hobbs and Svante Pääbo (2016) Stephen J. Elledge, Harry F. Noller, Roeland Nusse, Yoshinori Ohsumi, Huda Zoghbi (2017) Joanne Chory, Peter Walter, Kazutoshi Mori, Kim Nasmyth, Don W. Cleveland (2018) C. Frank Bennett and Adrian R. Krainer, Angelika Amon, Xiaowei Zhuang, Zhijian Chen (2019) Jeffrey M. Friedman, Franz-Ulrich Hartl, Arthur L. Horwich, David Julius, Virginia Man-Yee Lee (2020) David Baker, Catherine Dulac, Dennis Lo, Richard J. Youle (2021)

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Neutrino detectors, experiments, and facilities
Discoveries

Cowan–Reines ( νe ) Lederman–Schwartz–Steinberger ( νμ) DONUT ( ντ) Neutrino oscillation SN 1987 neutrino burst

Operating
(divided by primary neutrino source)
Astronomical

ANITA ANTARES ASD BDUNT Borexino BUST HALO IceCube LVD NEVOD SAGE Super-Kamiokande SNEWS

Reactor

Daya Bay Double Chooz KamLAND RENO STEREO

Accelerator

ANNIE ICARUS (Fermilab) MicroBooNE MINERνA MiniBooNE NA61/SHINE NOνA NuMI T2K

0νββ

AMoRE COBRA CUORE EXO GERDA KamLAND-Zen MAJORANA NEXT PandaX SNO+ XMASS

Other

KATRIN WITCH

Construction

ARA ARIANNA Baikal-GVD BEST DUNE Hyper-Kamiokande JUNO KM3NeT SuperNEMO FASERν

Retired

AMANDA CDHS Chooz CNGS Cuoricino DONUT ERPM GALLEX Gargamelle GNO Heidelberg-Moscow Homestake ICARUS IGEX IMB K2K Kamiokande KARMEN KGF LSND MACRO MINOS MINOS+ NARC NEMO OPERA RICE SciBooNE SNO Soudan 2 Utah

Proposed

CUPID GRAND INO LAGUNA LEGEND LENA Neutrino Factory nEXO Nucifer SBND UNO JEM-EUSO WATCHMAN

Cancelled

DUMAND Project Long Baseline Neutrino Experiment NEMO Project NESTOR Project SOX BOREX

See also

BNO (Baksan or Baxan Neutrino Observatory) Kamioka Observatory LNGS SNOLAB List of neutrino experiments

Physics Encyclopedia

World

Index

Hellenica World - Scientific Library

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