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Commissioning the KamLAND Experiment

Commissioning the KamLAND Experiment. Nikolai Tolich Stanford University. The KamLAND Collaboration. G.A.Horton-Smith, R.D.McKeown, J.Ritter, B.Tipton, P.Vogel California Institute of Technology C.E.Lane Drexel University Y-F.Wang IHEP, Beijing

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Commissioning the KamLAND Experiment

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  1. Commissioning the KamLAND Experiment Nikolai Tolich Stanford University

  2. The KamLAND Collaboration G.A.Horton-Smith, R.D.McKeown, J.Ritter, B.Tipton, P.Vogel California Institute of Technology C.E.Lane Drexel University Y-F.Wang IHEP, Beijing B.E.Berger, Y-D.Chan, D.A.Dwyer, S.J.Freedman, Y.Fu, B.K.Fujikawa, K.T.Lesko, K-B.Luk, H.Murayama, D.R.Nygren, C.E.Okada, A.W.Poon, H.M.Steiner, L.A.Winslow LBNL/UC Berkeley S.Dazeley, S.Hatakeyama, M.Murakami, R.C.Svoboda Louisiana State University J.Detwiler, G.Gratta, N.Tolich, Y.Uchida Stanford University K.Eguchi, S.Enomoto, K.Furuno, Y.Gando, J.Goldman, H.Hanada, H.Ikeda, K.Ikeda, K.Inoue, K.Ishihara, W.Ito, T.Iwamoto, T.Kawashima, H.Kinoshita, M.Koga, T.Maeda, T.Mitsui, M.Motoki, K.Nakajima, H.Ogawa, K.Oki, T.Sakabe, I.Shimizu, J.Shirai, F.Suekane, A.Suzuki, O.Tajima, K.Tamae, H.Watanabe Tohoku University L.DeBraeckeleer, C.Gould, H.Karwowski, D.Markoff, J.Messimore, K.Nakamura, R.Rohm, W.Tornow, A.Young TUNL J.Busenitz, Z.Djurcic, K.McKinny, D-M.Mei, A.Piepke, E.Yakushev University of Alabama P.Gorham, J.Learned, J.Maricic, S.Matsuno, S.Pakvasa University of Hawaii B.D.Dieterle University of New Mexico M.Batygov, W.Bugg, H.Cohn, Y.Efremenko, Y.Kamyshkov, Y.Nakamura University of Tennessee APS Meeting

  3. Solar LMA solution within reach • KamLAND (Kamioka Liquid-scintillator AntiNeutrino Detector) CHOOZ Palo Verde • Liquid-scintillator allows us to probe lower neutrino energies than water Cherenkov detectors KamLAND (expected) Solar LMA Solar SMA • KamLAND is studying the disappearance of electron anitneutrinos produced in nuclear reactors Solar LOW Mostly ruled out by recent SNO result • The reactor baseline is limited with 85.3% of the signal coming from reactors with a baseline of 140 km to 344 km Giving an expected Δm2 sensitivity of 710-6 eV2 Solar VAC APS Meeting

  4. The Detector 1km Overburden Electronics hut H2O Cerenkov veto counter 225 20” PMTs Ropes Steel sphere Balloon Buffer oil PMTs 1325 17” fast 554 20” large 34% coverage 1kton Liquid-scintillator Acrylic Sphere APS Meeting

  5. The Electronics PMTs DAQ Event Data Event Data Waveforms Run Conditions Run Conditions Event Data Run Conditions Trigger Command Trigger Command ESum NSum MACRO Electronics Trigger LBL Electronics APS Meeting

  6. The LBL Electronics • Waveforms for each PMT are recorded using Analogue Transient Waveform Digitizers (ATWDs) Allowing multi p.e. resolution • The ATWDs are self launching with a threshold ~1/3 p.e. • Each PMT is connected to 2 ATWDs Reducing deadtime • Each ATWD has 3 gains (20, 4, 0.5) Allowing a dynamic range of ~1mV to ~1V • There are 128 samples per waveform with a sample time of 1.5ns APS Meeting

  7. The Trigger • The trigger receives the number of PMTs above threshold on each FEE board every 25ns ~4 Gbytes/s • Based on the PMT hit pattern a capture command is sent to the LBL and MACRO electronics within 200 ns • Delayed trigger > ~0.5MeV less than 1ms after Prompt • Pre-scaled trigger > ~0.5MeV for 0.1ms every second • Prompt trigger > ~0.8MeV • Non physics triggers • Muon events all PMTs fire ~ ~ • Supernova “burst trigger” 48 events > 4MeV in 1s APS Meeting

  8. DAQ • KamLAND uses KINOKO for DAQ Outer Detector • KINOKO is a linux based DAQ system developed for KamLAND Inner Detector • Each VME crate is connected to a separate front end PC running a KINOKO process • The data from each front end PC is sent to a control PC Charge Time • The control PC is responsible for setting the run conditions, recording, and displaying the data APS Meeting

  9. Gain Calibration • Gain calibration has been done at 1p.e. level with peripheral LEDs • Very good quality single p.e. peak Charge • For gain calibration at higher p.e.’s we used a nitrogen laser • The laser intensity was controlled within 15% using different filters p.e.’s APS Meeting

  10. Timing Calibration Event Time All Tubes • Timing calibration was done using a dye laser =500nm Before Correction After Correction • The liquid scintillator is transparent at 500nm • This correction is waveform analysis dependent, we may be able to do better ns ns APS Meeting

  11. Energy Calibration 60Co 2.505 MeV + source • So far two sources have been placed in the detector, 60Co & 65Zn • The light yield is very high 241 p.e./MeV 65Zn 1.115 MeV  source NSum • Soon we will deploy a 137Cs 0.662 MeV  source and a AmBe 4.4 MeV neutron source NSum APS Meeting

  12. Energy Calibration 2 Neutrons following muons • Following muons we get neutron events, these allow us to calibrate the energy for neutrons • The energy of this peak is consistent with a 2.2 MeV n-capture Time since muon NSum • The capture time of 189±19s is consistent with the expected value of 180 s s APS Meeting

  13. Data is now coming in smoothly… stay tuned for results… APS Meeting

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