KamLAND

(KAMioka Liquid scintillator Anti-Neutrino Detector)

Other Web pages: LBL, Hawaii, Stanford, Spires

Useful Links

References

Precision Measurement of Neutrino Oscillation Parameters with KamLAND

$\Delta m^{2}_{21} = 7.59^{+0.21}_{-0.21} \times 10^{-5} eV^{2} \tan^2 \vartheta_{12} = 0.47^{+0.06}_{-0.05}$

(30 January 2008)

Experimental investigation of geologically produced antineutrinos with KamLAND

(27 July 2005)

First Measurement of Total Radioactive Power of the Earth

Measurement of Neutrino Oscillation with KamLAND: Evidence of Spectral Distortion - v3

(1 November 2004)

258 observed $\bar\nu_e -> \bar\nu_e$ events

expected events without oscillations

expected background events

disappearance confirmed at 99.998% C.L.

energy spectrum shows distorsions with 99.6% C.L.

best-fit of KamLAND data: $\Delta{m}^2 = 7.9 {}^{+0.6}_{-0.5} \times 10^{-5} \mathrm{eV}^2$

best-fit of KamLAND + solar data: $\Delta{m}^2 = 7.9 {}^{+0.6}_{-0.5} \times 10^{-5} \mathrm{eV}^2$ , $\tan^2\theta = 0.40 {}^{+0.10}_{-0.07}$

Measurement of Neutrino Oscillation with KamLAND: Evidence of Spectral Distortion

(13 June 2004)

see also: G. Gratta, Results from the KamLAND experiment, Neutrino 2004

258 observed $\bar\nu_e -> \bar\nu_e$ events

expected events without oscillations

disappearance confirmed at 99.995% C.L.

energy spectrum shows distorsions with 99.9% C.L.

best-fit of KamLAND data: $\Delta{m}^2 = 8.3 \times 10^{-5} \mathrm{eV}^2$ , $\tan^2\theta = 0.41$

best-fit of KamLAND + solar data: $\Delta{m}^2 = 8.2 {}^{+0.6}_{-0.5} \times 10^{-5} \mathrm{eV}^2$ , $\tan^2\theta = 0.40 {}^{+0.09}_{-0.07}$

A High Sensitivity Search for $\bar{\nu}_{e}$ 's from the Sun and Other Sources at KamLAND - hep-ex/0310047

$\Phi_{\bar\nu_e}^{sun} < 3.7 \times 10^2 \text{cm}^{-2} s^{-1} (90% \text{C.L.})$

$P_{\nu_e -> \bar\nu_e}^{sun} < 2.8{\times}10^{-4}$ $\text{for}$ $8.3 MeV < E_{\bar{\nu}_e} < 14.8 MeV$

(24 October 2003)

KamLAND Nails Neutrino Oscillations

6 December 2002

$P_{\nu_e -> \nu_e} = 0.611 +- 0.085 +- 0.041$ Best Fit: $\Delta{m}^2 = 6.9 \times 10^{-5} \mathrm{eV}^2$ , $\sin^22\vartheta = 1.0$

First Results from KamLAND: Evidence for Reactor Anti-Neutrino Disappearance, hep-ex/0212021

Useful Links

Dissertations
Data release accompanying the 2nd KamLAND Reactor Result
Proposal for US Participation in KamLAND Proposal for US Participation in KamLAND

References

References are divided in

1 - PhD Theses
2 - Neutrino Oscillations
3 - Neutrino Oscillations - Slides
4 - Solar Neutrinos
5 - Geo-Neutrinos
6 - Neutrinoless Double Beta Decay
7 - Physics
8 - Neutrino Flux
9 - Detector
10 - Background
11 - Proposal
12 - Conference Proceedings

The references in each group are listed in approximate inverted chronological order.
Click on the reference label to search it in Spires.

1 - PhD Theses

[1-1]: Measurement of neutrino oscillation with KamLAND, Detwiler, Jason A., 2005. UMI-31-62394. http://kamland.stanford.edu/TalksAndPublications/DetwilerThesis.pdf.

2 - Neutrino Oscillations

[2-1]: Enhanced Constraints on $\theta_{13}$ from A Three-Flavor Oscillation Analysis of Reactor Antineutrinos at KamLAND, A. Gando et al. (The KamLAND), Phys. Rev. D83 (2011) 052002, arXiv:1009.4771.
[2-2]: Precision Measurement of Neutrino Oscillation Parameters with KamLAND, Abe, S. et al. (KamLAND), Phys. Rev. Lett. 100 (2008) 221803, arXiv:0801.4589.
From the abstract: Combining with solar neutrino data, we obtain $\Delta m^{2}_{21} = 7.59^{+0.21}_{-0.21} \times 10^{-5} eV^{2}$ and $\tan^2 \vartheta_{12} = 0.47^{+0.06}_{-0.05}$ .
From the article: The spectrum indicates almost two cycles of the periodic feature expected from neutrino oscillation.
[2-3]: Measurement of Neutrino Oscillation with KamLAND: Evidence of Spectral Distortion, T. Araki et al. (KamLAND), Phys. Rev. Lett. 94 (2005) 081801, arXiv:hep-ex/0406035.
From the article: See this summary.
[2-4]: First Results from KamLAND: Evidence for Reactor Anti-Neutrino Disappearance, K. Eguchi et al. (KamLAND), Phys. Rev. Lett. 90 (2003) 021802, arXiv:hep-ex/0212021.
From the abstract: In an exposure of 162 ton $\cdot$ yr (145.1 days) the ratio of the number of observed inverse $\beta$ -decay events to the expected number of events without disappearance is $0.611 +- 0.085 {\rm (stat)} +- 0.041 {\rm (syst)}$ for $\bar{\nu}_e$ energies 3.4 MeV. The deficit of events is inconsistent with the expected rate for standard $\bar{\nu}_e$ propagation at the 99.95% confidence level. In the context of two-flavor neutrino oscillations with CPT invariance, these results exclude all oscillation solutions but the "Large Mixing Angle" solution to the solar neutrino problem using reactor $\bar{\nu}_e$ sources.

3 - Neutrino Oscillations - Slides

[3-1]: KamLAND (Anti-Neutrino Status), I. Shimizu (KamLAND), 2007. TAUP 2007. http://www.awa.tohoku.ac.jp/taup2007/slides/workshop14/roomA/02-KamLAND-AntiNeutrino-Status-Shimizu.pdf.

4 - Solar Neutrinos

[4-1]: Measurement of the 8B Solar Neutrino Flux with KamLAND, S. Abe et al. (KamLAND), Phys. Rev. C84 (2011) 035804, arXiv:1106.0861.
[4-2]: A High Sensitivity Search for $\bar{\nu}_{e}$ 's from the Sun and Other Sources at KamLAND, K. Eguchi et al. (KamLAND), Phys. Rev. Lett. 92 (2004) 071301, arXiv:hep-ex/0310047.
From the abstract: Data corresponding to a KamLAND detector exposure of 0.28 kton-year has been used to search for $\bar{\nu}_e$ 's in the energy range $8.3 MeV < E_{\bar{\nu}_e} < 14.8 MeV$ . No candidates were found for an expected background of events. This result can be used to obtain a limit on $\bar{\nu}_{e}$ fluxes of any origin. Assuming that all $\bar{\nu}_e$ flux has its origin in the Sun and has the characteristic solar $\nu_e$ energy spectrum, we obtain an upper limit of $3.7 \times 10^2 \text{cm}^{-2} s^{-1}$ (90% C.L.) on the $\bar{\nu}_e$ flux. We interpret this limit, corresponding to $2.8{\times}10^{-4}$ of the Standard Solar Model $\nu_e$ flux, in the framework of spin-flavor precession and neutrino decay models.

5 - Geo-Neutrinos

[5-1]: Experimental investigation of geologically produced antineutrinos with KamLAND, T. Araki et al. (KamLAND), Nature 436 (2005) 499-503. http://www.nature.com/nature/journal/v436/n7050/abs/nature03980.html;jsessionid=2B54E1F6E002C96A8C0F0275FB860964.
From the abstract: Assuming a Th/U mass concentration ratio of 3.9, the 90 per cent confidence interval for the total number of geoneutrinos detected is 4.5 to 54.2. This result is consistent with the central value of 19 predicted by geophysical models.
From the article: ... a "rate only" analysis gives $25 {}^{+19}_{-18}$ geoneutrino candidates from the $^{238}U$ and $^{232}\text{Th}$ decay chains. Dividing by the detection efficiency, live-time, and number of target protons, the total geoneutrino detected rate obtained is $5.1 {}^{+3.9}_{-3.6} \times 10^{-31}$ $\bar\nu_e$ per target proton per year.
...
The 99% confidence upper limit obtained on the total detected $^{238}U$ and $^{232}\text{Th}$ geoneutrino rate is $1.45 \times 10^{-30}$ $\bar\nu_e$ per target proton per year, corresponding to a flux at KamLAND of $1.62 \times 10^7 cm^{-2} \text{s}^{-1}$ . On the basis of our reference model, this corresponds to an upper limit on the radiogenic power from $^{238}U$ and $^{232}\text{Th}$ decay of 60 TW.

6 - Neutrinoless Double Beta Decay

[6-1]: Measurement of the Double-Beta Decay Half-life of ^{136}Xe in KamLAND-Zen, (KamLAND-Zen), arXiv:1201.4664, 2012.

7 - Physics

[7-1]: A study of extraterrestrial antineutrino sources with the KamLAND detector, A. Gando et al. (KamLAND), arXiv:1105.3516, 2011.
[7-2]: Study of the Production of Radioactive Isotopes through Cosmic Muon Spallation in KamLAND, Abe, S. et al. (KamLAND), Phys. Rev. C81 (2010) 025807, arXiv:0907.0066.
[7-3]: Search for the Invisible Decay of Neutrons with KamLAND, KamLAND collaboration (KamLAND), Phys. Rev. Lett. 96 (2006) 101802, arXiv:hep-ex/0512059.

8 - Neutrino Flux

[8-1]: A simple model of reactor cores for reactor neutrino flux calculations for the KamLAND experiment, K. Nakajima et al., arXiv:physics/0607126, 2006.

9 - Detector

[9-1]: The KamLAND Full-Volume Calibration System, B.E. Berger et al. (KamLAND), JINST 4 (2009) P04017, arXiv:0903.0441.
[9-2]: A C-13(alpha,n)O-16 calibration source for KamLAND, David W. McKee, Jerome K. Busenitz, Igor Ostrovskiy, Nucl. Instrum. Meth. A587 (2008) 272-276, arXiv:0711.3624.
[9-3]: Online monitoring system and data management for KamLAND, M.Motoki, F.Suekane, K.Tada, Y.Tsuda, Nucl. Instrum. Meth. A534 (2004) 59, arXiv:hep-ex/0405074.

10 - Background

[10-1]: Muon Simulations for Super-Kamiokande, KamLAND and CHOOZ, Alfred Tang, Glenn Horton-Smith, Vitaly A. Kudryavtsev, Alessandra Tonazzo, Phys. Rev. D74 (2006) 053007, arXiv:hep-ph/0604078.

11 - Proposal

[11-1]: Proposal for US Participation in KamLAND, Busenitz, J. et al., 1999. http://kamland.lbl.gov/TalksPaper/Papers/KamLAND.US.Proposal.pdf.

12 - Conference Proceedings

[12-1]: Recent Results from KamLAND, Ichimura, Koichi, Collaboration, for the KamLAND (KamLAND), arXiv:0810.3448, 2008. ICHEP08.
[12-2]: High Sensitivity Anti-Neutrino Detection by KamLAND, S. Hatakeyama et al. (KamLAND), arXiv:hep-ex/0405001, 2004. Moriond EW04.
[12-3]: An Overview of the KamLAND 1-kiloton Liquid Scintillator, F. Suekane et al., arXiv:physics/0404071, 2004. "KEK-RCNP International School and Mini-Workshop for Scintillating Crystals and their Applications in Particle and Nuclear Physics". (Nov. 17-18, 2003, KEK, Japan).
[12-4]: KamLAND: updated results, Inoue, K., 2004. Neutrino Oscillation Workshop NOW 2004, September 11-17, 2004, Conca Specchiulla (Otranto, Italy). http://www.ba.infn.it/~now2004/talks/12_09_04/plen/KamLAND.pdf.
[12-5]: Results from the KamLAND experiment, G. Gratta (KamLAND), 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/monday/gratta.pdf.
Comment: See Measurement of Neutrino Oscillation with KamLAND: Evidence of Spectral Distortion.
[12-6]: Recent Results from KamLAND, J. Detwiler (KamLAND), eConf C0307282 (2003) TW04, arXiv:hep-ex/0311007. SLAC Summer Institute, July 2003.
[12-7]: KamLAND results, Inoue, K., arXiv:hep-ex/0307030, 2003. XXXVIII Rencontres de Moriond on Electroweak Interactions and Unified Theories Les Arcs, France, 15-22 March 2003.
[12-8]: First KamLAND Results, Kamyshkov, Y., 2003. IV INTERNATIONAL CONFERENCE on NON-ACCELERATOR NEW PHYSICS - NANP 2003 - Dubna, Russia, June 23-28, 2003. http://nanp.dubna.ru/talks/kamyshkov.pdf.
Comment: Slide n. 41 shows comparison of data (13 bins) with 2- $\nu$ oscillation, best fit $\chi^2 = 2.8$ , and with no oscillation - constant flux suppression, $\chi^2 = 5.3$ . (M.L.).
[12-9]: KamLAND Results, Inoue, K., 2003. The 4th Workshop on Neutrino Oscillations and their Origin (NOON2003), February 10-14, 2003, Ishikawa Kousei Nenkin Kaikan, Kanazawa, Japan. http://www-sk.icrr.u-tokyo.ac.jp/noon2003/transparencies/10/Inoue-KamLAND.pdf.
[12-10]: An update on progress at KamLAND, Dazeley, S. A. (KamLAND), arXiv:hep-ex/0205041, 2002.
[12-11]: First Results from KamLAND: Evidence for $\bar{\nu}_e$ disappearance, Gratta, G. (Kamland), 2002. SLAC Colloquium, December 2002. http://hep.stanford.edu/neutrino/KamLAND/TalksAndPublications/KamLAND_FirstResults_SLAC_Colloq.pdf.
[12-12]: KamLAND: Examination of the LMA solution with reactor neutrinos, Suzuki, A. (Kamland), 2002. XVI International Conference on Particles and Nuclei, Osaka, Japan, September 30 - October 4, 2002. http://www.rcnp.osaka-u.ac.jp/Divisions/np2/PaNic02/Suzuki.pdf.
[12-13]: Status of KAMLAND Project, Suekane, F. (Kamland), 2002. Conference on Physics beyond the Standard Model - BEYOND THE DESERT 02 - Oulu, Finland, 2-7 June 2002. http://cupp.oulu.fi/trans/Suekane.pdf.
[12-14]: Start of Kamland, Shirai, J. (Kamland), 2002. TXXth International Conference on Neutrino Physics and Astrophysics May 25 - 30, 2002, Munich, Germany. http://neutrino2002.ph.tum.de/pages/transparencies/suzuki.
[12-15]: The KamLAND detector and backgrounds for solar neutrino detection, Furuno, K., 2002. III^rd International Workshop on Low Energy Solar Neutrinos - LOW NU 2002, 22-24 May 2002, Heidelberg, Germany. http://www.mpi-hd.mpg.de/nubis/www_lownu2002/transparency/furuno_lownu_2002.pdf.
[12-16]: Commissioning the KamLAND experiment, Tolik, N., 2002. The April Meeting 2002 of the American Physical Society. http://www.awa.tohoku.ac.jp/KamLAND/APS_April2002.pdf.
[12-17]: Kamland, Ishihara, K., 2001. The Third International Workshop on Neutrino Factories based on Muon Storage Rings (NuFACT'01) May 24th - May 30th, 2001, Tsukuba, Japan. http://www-prism.kek.jp/nufact01/May26/WG1/26wg1_ishihara.pdf.
[12-18]: Kamland, Goldman, j., 2001. 3rd Workshop on Neutrino Oscillations and their Origin: NOON01. http://www-sk.icrr.u-tokyo.ac.jp/noon2001/transparency/dec05/goldman/goldman.pdf.
[12-19]: KamLAND: A reactor neutrino experiment testing the solar neutrino anomaly, Piepke, A. (KamLAND), Nucl. Phys. Proc. Suppl. 91 (2001) 99-104.
[12-20]: Neutrino physics with the KamLAND detector, De Braeckeleer, L. (KamLAND), Nucl. Phys. Proc. Suppl. 87 (2000) 312-314.
[12-21]: The present status of KamLAND, Suzuki, A. (KamLAND), Nucl. Phys. Proc. Suppl. 77 (1999) 171-176.
[12-22]: Physics opportunities with the KamLAND experiment, Wang, Yi Fang (KamLAND), 1998. Talk given at 29th International Conference on High-Energy Physics (ICHEP 98), Vancouver, Canada, 23-29 Jul 1998.
[12-23]: KamLAND experiment: Exploring low energy neutrino physics, Shirai, J., 1998.

Neutrino Unbound

We Can Put an End to Word Attachments

Authors:
Carlo Giunti / giunti@to.infn.it
Marco Laveder / marco.laveder@pd.infn.it

Last Update: Fri 10 Feb 2012, day 41 of the year 2012, 09:08:55 UTC