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Search Results: 1 - 10 of 117844 matches for " T. Lachenmaier "
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Implications of the SNO and the Homestake Results for the BOREXINO Experiment
S. M. Bilenky,T. Lachenmaier,W. Potzel,F. von Feilitzsch
Physics , 2001,
Abstract: Using the recent result of the SNO solar neutrino experiment, we have demonstrated in a model independent way that the contribution of Be-7 and other medium energy neutrinos to the event rate of the Homestake experiment is 4 sigma smaller than the BP2000 SSM prediction. We have considered the implications of this result for the future BOREXINO experiment.
Monte Carlo aided design of the inner muon veto detectors for the Double Chooz experiment
D. Dietrich,D. Greiner,J. Jochum,T. Lachenmaier,L. F. F. Stokes,M. R?hling
Physics , 2012, DOI: 10.1088/1748-0221/7/08/P08012
Abstract: The Double Chooz neutrino experiment aims to measure the last unknown neutrino mixing angle theta_13 using two identical detectors positioned at sites both near and far from the reactor cores of the Chooz nuclear power plant. To suppress correlated background induced by cosmic muons in the detectors, they are protected by veto detector systems. One of these systems is the inner muon veto. It is an active liquid scintillator based detector and instrumented with encapsulated photomultiplier tubes. In this paper we describe the Monte Carlo aided design process of the inner muon veto, that resulted in a detector configuration with 78 PMTs yielding an efficiency of 99.978 +- 0.004% for rejecting muon events and an efficiency of >98.98% for rejecting correlated events induced by muons. A veto detector of this design is currently used at the far detector site and will be built and incorporated as the muon identification system at the near site of the Double Chooz experiment.
Study on Neutron-induced Background in the CRESST Experiment
H. Wulandari,F. von Feilitzsch,M. Huber,Th. Jagemann,J. Jochum,T. Lachenmaier,J. -C. Lanfranchi,W. Potzel,W. Rau,M. Stark,S. Waller
Physics , 2003,
Abstract: CRESST II is an experiment for direct WIMP search, using cryogenic detectors. The ratio of the two signals (temperature rise and scintillation light) measured for each interaction is an excellent parameter for discrimination of radioactive background. The main remaining background is the neutron flux present at the experimental site, since neutrons produce the same signals as WIMPs do. Based on Monte Carlo simulations the present work shows how neutrons from different origins affect CRESST and which measures have to be taken into account to reach the goal sensitivity.
Low-Temperature Light Detectors: Neganov-Luke Amplification and Calibration
C. Isaila,C. Ciemniak,F. v. Feilitzsch,A. Gütlein,J. Kemmer,T. Lachenmaier,J. -C. Lanfranchi,S. Pfister,W. Potzel,S. Roth,M. v. Sivers,R. Strauss,W. Westphal,F. Wiest
Physics , 2011, DOI: 10.1016/j.physletb.2012.08.003
Abstract: The simultaneous measurement of phonons and scintillation light induced by incident particles in a scintillating crystal such as CaWO4 is a powerful technique for the active rejection of background induced by gamma's and beta's and even neutrons in direct Dark Matter searches. However, less than ~1% of the energy deposited in a CaWO4 crystal is detected as light. Thus, very sensitive light detectors are needed for an efficient event-by-event background discrimination. Due to the Neganov-Luke effect, the threshold of low-temperature light detectors based on semiconducting substrates can be improved significantly by drifting the photon-induced electron-hole pairs in an applied electric field. We present measurements with low-temperature light detectors based on this amplification mechanism. The Neganov-Luke effect makes it possible to improve the signal-to-noise ratio of our light detectors by a factor of ~9 corresponding to an energy threshold of ~21 eV. We also describe a method for an absolute energy calibration using a light-emitting diode.
Solar and Atmospheric Neutrinos: Limitations for Direct Dark Matter Searches
A. Gütlein,W. Potzel,C. Ciemniak,F. von Feilitzsch,N. Haag,M. Hofmann,C. Isaila,T. Lachenmaier,J. -C. Lanfranchi,L. Oberauer,S. Pfister,S. Roth,M. von Sivers,R. Strau?,A. Z?ller
Physics , 2010,
Abstract: In experiments for direct dark matter searches, neutrinos coherently scattering off nuclei can produce similar events as Weakly Interacting Massive Particles (WIMPs). To reach sensitivities better than about 10^-10 pb for the elastic WIMP nucleon spin-independent cross section in the zero-background limit, energy thresholds for nuclear recoils should be >2.05 keV for CaWO_4, >4.91 keV for Ge, >2.89 keV for Xe, >8.62 keV for Ar and >15.93 keV for Ne as target material. Atmospheric neutrinos limit the achievable sensitivity for the background-free direct dark matter search to >10^-12 pb.
GNO Solar Neutrino Observations: Results for GNOI
GNO Collaboration,M. Altmann,M. Balata,P. Belli,E. Bellotti,R. Bernabei,E. Burkert,C. Cattadori,G. Cerichelli,M. Chiarini,M. Cribier,S. d'Angelo,G. Del Re,K. H. Ebert,F. v. Feilitzsch,N. Ferrari,W. Hampel,J. Handt,E. Henrich,G. Heusser,J. Kiko,T. Kirsten,T. Lachenmaier,J. Lanfranchi,M. Laubenstein,D. Motta,W. Rau,H. Richter,S. Waenninger,M. Wojcik,L. Zanotti
Physics , 2000, DOI: 10.1016/S0370-2693(00)00915-1
Abstract: We report the first GNO solar neutrino results for the measuring period GNOI, solar exposure time May 20, 1998 till January 12, 2000. In the present analysis, counting results for solar runs SR1 - SR19 were used till April 4, 2000. With counting completed for all but the last 3 runs (SR17 - SR19), the GNO I result is [65.8 +10.2 -9.6 (stat.) +3.4 -3.6 (syst.)]SNU (1sigma) or [65.8 + 10.7 -10.2 (incl. syst.)]SNU (1sigma) with errors combined. This may be compared to the result for Gallex(I-IV), which is [77.5 +7.6 -7.8 (incl. syst.)] SNU (1sigma). A combined result from both GNOI and Gallex(I-IV) together is [74.1 + 6.7 -6.8 (incl. syst.)] SNU (1sigma).
Letter of Intent for Double-CHOOZ: a Search for the Mixing Angle Theta13
F. Ardellier,I. Barabanov,J. C. Barriere,M. Bauer,L. Bezrukov,C. Buck,C. Cattadori,B. Courty,M. Cribier,F. Dalnoki-Veress,N. Danilov,H. de Kerret,A. Di Vacri,A. Etenko,M. Fallot,Ch. Grieb,M. Goeger,A. Guertin,T. Kirchner,Y. S. Krylov,D. Kryn,C. Hagner,W. Hampel,F. X. Hartmann,P. Huber,J. Jochum,T. Lachenmaier,Th. Lasserre,Ch. Lendvai,M. Lindner,F. Marie,J. Martino,G. Mention,A. Milsztajn,J. P. Meyer,D. Motta,L. Oberauer,M. Obolensky,L. Pandola,W. Potzel,S. Schoenert,U. Schwan,T. Schwetz,S. Scholl,L. Scola,M. Skorokhvatov,S. Sukhotin,A. Letourneau,D. Vignaud,F. von Feilitzsch,W. Winter,E. Yanovich
Physics , 2004,
Abstract: Tremendous progress has been achieved in neutrino oscillation physics during the last few years. However, the smallness of the $\t13$ neutrino mixing angle still remains enigmatic. The current best constraint comes from the CHOOZ reactor neutrino experiment $\s2t13 < 0.2$ (at 90% C.L., for $\adm2=2.0 10^{-3} \text{eV}^2$). We propose a new experiment on the same site, Double-CHOOZ, to explore the range of $\s2t13$ from 0.2 to 0.03, within three years of data taking. The improvement of the CHOOZ result requires an increase in the statistics, a reduction of the systematic error below one percent, and a careful control of the cosmic ray induced background. Therefore, Double-CHOOZ will use two identical detectors, one at $\sim$150 m and another at 1.05 km distance from the nuclear cores. The plan is to start data taking with two detectors in 2008, and to reach a sensitivity of 0.05 in 2009, and 0.03 in 2011.
Complete results for five years of GNO solar neutrino observations
GNO COLLABORATION,M. Altmann,M. Balata,P. Belli,E. Bellotti,R. Bernabei,E. Burkert,C. Cattadori,R. Cerulli,M. Chiarini,M. Cribier,S. d'Angelo,G. Del Re,K. H. Ebert,F. v. Feilitzsch,N. Ferrari,W. Hampel,F. X. Hartmann,E. Henrich,G. Heusser,F. Kaether,J. Kiko,T. Kirsten,T. Lachenmaier,J. Lanfranchi,M. Laubenstein,K. Luetzenkirchen,K. Mayer,P. Moegel,D. Motta,S. Nisi,J. Oehm,L. Pandola,F. Petricca,W. Potzel,H. Richter,S. Schoenert,M. Wallenius,M. Wojcik,L. Zanotti
Statistics , 2005, DOI: 10.1016/j.physletb.2005.04.068
Abstract: We report the complete GNO solar neutrino results for the measuring periods GNO III, GNO II, and GNO I. The result for GNO III (last 15 solar runs) is [54.3 + 9.9 - 9.3 (stat.)+- 2.3 (syst.)] SNU (1 sigma) or [54.3 + 10.2 - 9.6 (incl. syst.)] SNU (1 sigma) with errors combined. The GNO experiment is now terminated after altogether 58 solar exposure runs that were performed between May 20, 1998 and April 9, 2003. The combined result for GNO (I+II+III) is [62.9 + 5.5 - 5.3 (stat.) +- 2.5 (syst.)] SNU (1 sigma) or [62.9 + 6.0 - 5.9] SNU (1 sigma) with errors combined in quadrature. Overall, gallium based solar observations at LNGS (first in GALLEX, later in GNO) lasted from May 14, 1991 through April 9, 2003. The joint result from 123 runs in GNO and GALLEX is [69.3 +- 5.5 (incl. syst.)] SNU (1 sigma). The distribution of the individual run results is consistent with the hypothesis of a neutrino flux that is constant in time. Implications from the data in particle- and astrophysics are reiterated.
Large underground, liquid based detectors for astro-particle physics in Europe: scientific case and prospects
Autiero, D.;Aysto, J.;Badertscher, A.;Bezrukov, L.;Bouchez, J.;Bueno, A.;Busto, J.;Campagne, J. -E.;Cavata, Ch.;Chaussard, L.;de Bellefon, A.;Declais, Y.;Dumarchez, J.;Ebert, J.;Enqvist, T.;Ereditato, A.;von Feilitzsch, F.;Perez, P. Fileviez;Goger-Neff, M.;Gninenko, S.;Gruber, W.;Hagner, C.;Hess, M.;Hochmuth, K. A.;Kisiel, J.;Knecht, L.;Kreslo, I.;Kudryavtsev, V. A.;Kuusiniemi, P.;Lachenmaier, T.;Laffranchi, M.;Lefievre, B.;Lightfoot, P. K.;Lindner, M.;Maalampi, J.;Maltoni, M.;Marchionni, A.;Undagoitia, T. Marrodan;Marteau, J.;Meregaglia, A.;Messina, M.;Mezzetto, M.;Mirizzi, A.;Mosca, L.;Moser, U.;Muller, A.;Natterer, G.;Oberauer, L.;Otiougova, P.;Patzak, T.;Peltoniemi, J.;Potzel, W.;Pistillo, C .;Raffelt, G. G.;Rondio, E.;Roos, M.;Rossi, B.;Rubbia, A.;Savvinov, N.;Schwetz, T.;Sobczyk, J.;Spooner, N. J. C.;Stefan, D.;Tonazzo, A.;Trzaska, W.;Ulbricht, J.;Volpe, C.;Winter, J.;Wurm, M.;Zalewska, A.;Zimmermann, R.
High Energy Physics - Phenomenology , 2007, DOI: 10.1088/1475-7516/2007/11/011
Abstract: This document reports on a series of experimental and theoretical studies conducted to assess the astro-particle physics potential of three future large-scale particle detectors proposed in Europe as next generation underground observatories. The proposed apparatus employ three different and, to some extent, complementary detection techniques: GLACIER (liquid Argon TPC), LENA (liquid scintillator) and MEMPHYS (\WC), based on the use of large mass of liquids as active detection media. The results of these studies are presented along with a critical discussion of the performance attainable by the three proposed approaches coupled to existing or planned underground laboratories, in relation to open and outstanding physics issues such as the search for matter instability, the detection of astrophysical- and geo-neutrinos and to the possible use of these detectors in future high-intensity neutrino beams.
The Physics Potential of the LENA Detector
Michael Wurm,Franz von Feilitzsch,Marianne Goeger-Neff,Tobias Lachenmaier,Timo Lewke,Quirin Meindl,Randolph Moellenberg,Lothar Oberauer,Juha Peltoniemi,Walter Potzel,Marc Tippmann,Juergen Winter
Physics , 2010,
Abstract: The large-volume liquid-scintillator detector LENA (Low Energy Neutrino Astronomy) has been proposed as a next-generation experiment for low-energy neutrinos. High-precision spectroscopy of solar, Supernova and geo-neutrinos provides a new access to the otherwise unobservable interiors of Earth, Sun and heavy stars. Due to the potent background discrimination, the detection of the Diffuse Supernova Neutrino Background is expected for the first time in LENA. The sensitivity of the proton lifetime for the decay into Kaon and antineutrino will be increased by an order of magnitude over existing experimental limits. Recent studies indicate that liquid-scintillator detectors are capable to reconstruct neutrino events even at GeV energies, providing the opportunity to use LENA as far detector in a long-baseline neutrino beam experiment.
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