Kamioka Liquid Scintillator Antineutrino Detector

Short description: Neutrino oscillation experiment in Japan

Schematic of the KamLAND detector

[ ⚑ ]  36°25′21″N 137°18′55″E﻿ / ﻿36.4225°N 137.3153°E﻿ / 36.4225; 137.3153[1]: 105 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 (ν¯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 ν¯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.

## Contents

* 1 KamLAND Detector
* 2 Results
* 2.1 Neutrino oscillation
* 2.2 Geological antineutrinos (geoneutrinos)
* 2.3 KamLAND-Zen Double Beta Decay Search
* 3 References
* 4 Further reading
* 5 External links

## 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 (Template:Subatomic Particle) are detected through the Inverse beta decay reaction ν¯e+p->e++n, which has a 1.8 MeV ν¯e energy threshold. The prompt scintillation light from the positron (e+) gives an estimate of the incident antineutrino energy, Eν=Eprompt+<En>+0.9MeV, where Epromptis the prompt event energy including the positron kinetic energy and the e+e− annihilation energy. The quantity <En> 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 [[Physics:Gamma ray|Template:Subatomic Particle 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 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.[citation needed] It is consistent with 2-neutrino oscillation and a fit provides the values for the Δm2 and θ parameters. Since KamLAND measures Δm2 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 Δm2=7.9−0.5+0.6⋅10−5eV2 and tan2θ=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]

Δm212=7.59±0.21⋅10−5eV2,tan2θ12=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 11.2−5.1+7.9 TW [11] using 116 ν¯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: 2.38±0.02(stat)±0.14(syst)*1021 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, 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 1.07×1026 years for the neutrinoless double beta decay half-life. The KamLAND-Zen 400 operated from 2011 October to 2015 October and was then replaced by KamLAND-Zen 800.[14]

The second KamLAND-Zen experiment apparatus, KamLAND-Zen 800, with bigger balloon of about 750 kg of Xenon was installed in the KamLAND detector 10 May 2018. The operation was expected to start winter 2018-2019 with 5 years of expected operation.[15]

The KamLAND-Zen 800 experiment started data taking in January 2019 and first results were published in 2020.[16] In March 2022 the KamLAND-Zen Collaboration using the KamLAND-Zen 800 published results about neutrinoless double-beta decay in Xe-136 using data collected between February 5, 2019 and May 8, 2021. No neutrinoless double-beta decay was observed, and the established lower bound for half-life was T > 2.3×1026 yr corresponding to upper limits on the effective Majorana neutrino mass of 36 – 156 meV.[17]

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

## References

1. ↑ Iwamoto, Toshiyuki (February 2003), Measurement of Reactor Anti-Neutrino Disappearance in KamLAND, Tohoku University, http://kamland.lbl.gov/Dissertations/IwamotoToshiyuki-DoctorThesis.pdf
2. ↑ Suzuki, Atsuto; Collaboration, KamLand (2005-01-01). "Results from KamLAND Reactor Neutrino Detection" (in en). Physica Scripta 2005 (T121): 33. doi:10.1088/0031-8949/2005/T121/004. ISSN 1402-4896. Bibcode: 2005PhST..121...33S. http://stacks.iop.org/1402-4896/2005/i=T121/a=004.
3. ↑ 3.0 3.1 Gando, A. (19 April 2012). "Measurement of the double-β decay half-life of 136Xe with the KamLAND-Zen experiment". Physical Review C 85 (4): 045504. doi:10.1103/PhysRevC.85.045504. Bibcode: 2012PhRvC..85d5504G.
4. ↑ Fushimi, K (2013). "PICO-LON Dark Matter Search". Journal of Physics 469 (1): 012011. doi:10.1088/1742-6596/469/1/012011. Bibcode: 2013JPhCS.469a2011F.
5. ↑ Eguchi, K. (2003). "First results from KamLAND: evidence for reactor antineutrino disappearance". Physical Review Letters 90 (2): 021802–021807. doi:10.1103/PhysRevLett.90.021802. PMID 12570536. Bibcode: 2003PhRvL..90b1802E.
6. ↑ Araki, T. (2005). "Measurement of neutrino oscillation with KamLAND: evidence of spectral distortion". Physical Review Letters 94 (8): 081801–081806. doi:10.1103/PhysRevLett.94.081801. PMID 15783875. Bibcode: 2005PhRvL..94h1801A.
7. ↑ Abe, S. (5 Jun 2008). "Precision Measurement of Neutrino Oscillation Parameters with KamLAND". Physical Review Letters 100 (22): 221803. doi:10.1103/PhysRevLett.100.221803. PMID 18643415. Bibcode: 2008PhRvL.100v1803A.
8. ↑ Gando, A. (2011). "Constraints on θ13 from A Three-Flavor Oscillation Analysis of Reactor Antineutrinos at KamLAND". Physical Review D 83 (5): 052002. doi:10.1103/PhysRevD.83.052002. Bibcode: 2011PhRvD..83e2002G.
9. ↑ Araki, T. (2005). "Experimental investigation of geologically produced antineutrinos with KamLAND". Nature 436 (7050): 499–503. doi:10.1038/nature03980. PMID 16049478. Bibcode: 2005Natur.436..499A.
10. ↑ Gando, A. (17 July 2011). "Partial radiogenic heat model for Earth revealed by geoneutrino measurements". Nature Geoscience 4 (9): 647–651. doi:10.1038/ngeo1205. Bibcode: 2011NatGe...4..647K. https://authors.library.caltech.edu/25422/1/Gando2011p15815Nat_Geosci.pdf.
11. ↑ A. Gando et al. (KamLAND Collaboration) (2 August 2013). "Reactor on-off antineutrino measurement with KamLAND". Physical Review D 88 (3): 033001. doi:10.1103/PhysRevD.88.033001. Bibcode: 2013PhRvD..88c3001G.
12. ↑ Gando, A. (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. doi:10.1103/PhysRevLett.110.062502. PMID 23432237. Bibcode: 2013PhRvL.110f2502G.
13. ↑ Gando, A. (16 August 2016). "Search for Majorana Neutrinos Near the Inverted Mass Hierarchy Region with KamLAND-Zen". Physical Review Letters 117 (8): 082503. doi:10.1103/PhysRevLett.117.082503. PMID 27588852. Bibcode: 2016PhRvL.117h2503G.
14. ↑ Abe, S. et al. (2022). "A Search for Correlated Low-energy Electron Antineutrinos in KamLAND with Gamma-Ray Bursts". The Astrophysical Journal 927 (1): 69. doi:10.3847/1538-4357/ac4e7e. Bibcode: 2022ApJ...927...69A.
15. ↑ Yoshihito, Gando (14 September 2018). "Neutrinoless double beta decay search with KamLAND-Zen". https://web2.ba.infn.it/now/now2018/assets/yoshihitogandonow2018.pdf.
16. ↑ Gando, Yoshihito (2020). "First results of KamLAND-Zen 800". Journal of Physics: Conference Series 1468: 012142. doi:10.1088/1742-6596/1468/1/012142.
17. ↑ Collaboration, KamLAND-Zen (2023). "Search for the Majorana Nature of Neutrinos in the Inverted Mass Ordering Region with KamLAND-Zen". Physical Review Letters 130 (5): 051801. doi:10.1103/PhysRevLett.130.051801. PMID 36800472. Bibcode: 2023PhRvL.130e1801A.

## Further reading

* Abe, S (2008). "Precision Measurement of Neutrino Oscillation Parameters with KamLAND". Physical Review Letters 100 (22): 221803. doi:10.1103/PhysRevLett.100.221803. PMID 18643415. Bibcode: 2008PhRvL.100v1803A.
* Eguchi, K (2004). "High sensitivity search for νe's from the sun and other sources at KamLAND". Physical Review Letters 92 (7): 071301–071305. doi:10.1103/PhysRevLett.92.071301. PMID 14995837. Bibcode: 2004PhRvL..92g1301E.νe's+from+the+sun+and+other+sources+at+KamLAND&rft.jtitle=[[Physics:Physical+Review+Letters|Physical+Review+Letters]]&rft.aulast=Eguchi&rft.aufirst=K&rft.au=Eguchi, K&rft.date=2004&rft.volume=92&rft.issue=7&rft.pages=071301–071305&rft_id=info:doi/10.1103/PhysRevLett.92.071301&rft_id=info:pmid/14995837&rft_id=info:bibcode/2004PhRvL..92g1301E&rfr_id=info:sid/en.wikibooks.org:Astronomy:Kamioka_Liquid_Scintillator_Antineutrino_Detector">

## External links

* KamLAND official website
* KamLAND at Lawrence Berkeley National Laboratory (Berkeley Lab)
* KamLAND experiment record on INSPIRE-HEP

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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
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* BUST
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* NEVOD
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|

Reactor|

* Daya Bay
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Accelerator|

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0νββ|

* AMoRE
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Other|

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See also|

* BNO
* Kamioka Observatory
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* List of neutrino experiments

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