118484897
CeLAND: search for a 4th light neutrino state with a 3 PBq 144Ce-144Pr electron antineutrino generator in KamLAND
Author(s): Gando, A; Gando, Y; Hayashida, S; Ikeda, H; Inoue, K; Ishidoshiro, K; Ishikawa, H; Koga, M; Matsuda, R; Matsuda, S; Mitsui, T; Motoki, D; Nakamura, K; Oki, Y; Otani, M; Shimizu, I; Shirai, J; Suekane, F; Suzuki, A; Takemoto, Y; Tamae, K; Ueshima, K; Watanabe, H; Xu, BD; Yamada, S; Yamauchi, Y; Yoshida, H; Cribier, M; Durero, M; Fischer, V; Gaffiot, J; Jonqueres, N; Kouchner, A; Lasserre, T; Leterme, D; Letourneau, A; Lhuillier, D; Mention, G; Rampal, G; Scola, L; Veyssiere, C; Vivier, M; Yala, P; Berger, BE; Kozlov, A; Banks, T; Dwyer, D; Fujikawa, BK; Han, K; Kolomensky, YG; Mei, Y; O'Donnell, T; Decowski, P; Markoff, DM; Yoshida, S; Kornoukhov, VN; Gelis, TVM; Tikhomirov, GV; Learned, JG; Maricic, J; Matsuno, S; Milincic, R; Karwowski, HJ; Efremenko, Y; Detwiler, A; Enomoto, S | Abstract: The reactor neutrino and gallium anomalies can be tested with a 3-4 PBq (75-100 kCi scale) 144Ce-144Pr antineutrino beta-source deployed at the center or next to a large low-background liquid scintillator detector. The antineutrino generator will be produced by the Russian reprocessing plant PA Mayak as early as 2014, transported to Japan, and deployed in the Kamioka Liquid Scintillator Anti-Neutrino Detector (KamLAND) as early as 2015. KamLAND's 13 m diameter target volume provides a suitable environment to measure the energy and position dependence of the detected neutrino flux. A characteristic oscillation pattern would be visible for a baseline of about 10 m or less, providing a very clean signal of neutrino disappearance into a yet-unknown, sterile neutrino state. This will provide a comprehensive test of the electron dissaperance neutrino anomalies and could lead to the discovery of a 4th neutrino state for Delta_m^2 g 0.1 eV^2 and sin^2(2theta) g 0.05.
1645909
Partial radiogenic heat model for Earth revealed by geoneutrino measurements
The Earth has cooled since its formation, yet the decay of radiogenic isotopes, and in particular uranium, thorium and 
potassium, in the planet’s interior provides a continuing heat source. The current total heat flux from the Earth to space is 44:2±1.0 TW, but the relative contributions from residual primordial heat and radiogenic decay remain uncertain. However, radiogenic decay can be estimated from the flux of geoneutrinos, electrically neutral particles that are emitted during radioactive decay and can pass through the Earth virtually unaffected. Here we combine precise measurements of the geoneutrino flux from the Kamioka Liquid-Scintillator Antineutrino Detector, Japan, with existing measurements from the Borexino detector, Italy.We find that decay of uranium-238 and thorium-232 together contribute 20.0^(+8.8)_(-8.6)TW to Earth’s heat 
flux. The neutrinos emitted from the decay of potassium-40 are below the limits of detection in our experiments, but are known to contribute 4TW. Taken together, our observations indicate that heat from radioactive decay contributes about half of Earth’s total heat flux. We therefore conclude that Earth’s primordial heat supply has not yet been exhausted.
41701681
Measurement of the 8B solar neutrino flux with the KamLAND liquid scintillator detector
We report a measurement of the neutrino-electron elastic scattering rate from ^8B solar neutrinos based on a 123 kton-day exposure of KamLAND. The background-subtracted electron recoil rate, above a 5.5-MeV analysis threshold is 1.49 ± 0.14(stat) ± 0.17(syst) events per kton-day. Interpreted as due to a pure electron flavor flux with a ^8B neutrino spectrum, this corresponds to a spectrum integrated flux of 2.77 ± 0.26(stat) ± 0.32(syst) ×10^6 cm^(−2_s^(−1). The analysis threshold is driven by ^(208)Tl present in the liquid scintillator, and the main source of systematic uncertainty is due to background from cosmogenic ^(11)Be. The measured rate is consistent with existing measurements and with standard solar model predictions which include matter-enhanced neutrino oscillation.
55546545
Validation of techniques to mitigate copper surface contamination in CUORE
In this article we describe the background challenges for the CUORE experiment posed by surface contamination of inert detector materials such as copper, and present three techniques explored to mitigate these backgrounds. Using data from a dedicated test apparatus constructed to validate and compare these techniques we demonstrate that copper surface contamination levels better than 10(-7)- 10(-8) Bq/cm(2) are achieved for U-238 and Th-232. If these levels are reproduced in the final CUORE apparatus the projected 90% C.L. upper limit on the number of background counts in the region of interest is 0.02-0.03 counts/keV/kg/y depending on the adopted mitigation technique. (C) 2013 Elsevier B.V. All rights reserved.
118695560
First results from the MuLan and MuCap experiments
MuLan and MuCap are ongoing experiments at the Paul Scherrer Institut, Switzerland, that use the muon lifetime to determine fundamental weak interaction parameters. The goal of MuLan is a 1 ppm measurement of the positive muon lifetime τμ+ to determine the Fermi constant GF to 0.5 ppm. The goal of MuCap is to make a 1% determination of the rate ΛS of the process of nuclear muon capture by the proton, μp→nν, by measuring the μ− disappearance rate in hydrogen gas to 10 ppm and subtracting the world average for the μ+ decay rate. A 1% determination of the capture rate ΛS is of interest because it would enable a 7% determination of gP, the induced pseudoscalar coupling of the nucleon. In 2007, both experiments published first results based upon data collected by each in 2004. MuLan reported an 11 ppm μ+ lifetime measurement, τμ+ = 2.197 013(24) μs, resulting in a new, 9.6 ppm world average, τμ+ = 2.197 019(21) μs, which determines the Fermi constant, GF = 1.166 371(6)×10−5 GeV−2, to 5 ppm. MuCap reported a 3%...
55856903
Sensitivity of CUORE to Neutrinoless Double-Beta Decay
Sensitivity of CUORE to Neutrinoless Double-Beta Decay b c,:L d e f F . Alessandria , E . A n d r e o t t i ' , R. A r d i t o , C. Arnaboldi , F . T. Avignone IIP , M . B a l a t a , I. Bandac , T. I. Banks ' ' , G . B a r f , J . Beeman , F . Bellini ' , A . Bersani , M . Biassoni ' , T. Bloxham , C. Brofferio ' , A . Bryant , C. B u c c i , X . Z. C a i , L . C a n o n i c a , S. C a p e l l i , L . Carbone , L . Cardani ' , M . Carrettoni , N . Casali ' , N . Chott , M . Clemenza ' , C. Cosmelli ' , O. Cremonesi , R. J . Creswick , I. Dafinei , A . Dally , A . De B i a s i , M . R Decowski ' ' , M . M . Deninno , A . de Waard , S. D i D o m i z i o ' , L . Ejzak '*, R. Faccini ' , D. Q. Fang , H . A . Farach , E . Ferri '°, F . Ferroni , E . F i o r i n i , L . F o g g e t t a ' ° , M . A . Franceschi*, S. J . Freedman G . Frossati , B . K . Fujikawa , A . Giachero , L . Gironi '°, A . Giuliani , P. G o r l a , C. G o t t i , E . Guardincerri , T. D . Gutierrez , E . E . H a l l e r ' , K . Han , K . M . Heeger , H . Z. Huang*', K . Ichimura , R. KadeP, K . K a z k a z , G . KeppeT, L . Kogler ' , Y u . G . Kolomensky ' , S. K r a f t ' , D . Lenz , Y . L . L i , X . L i # , E . Longo ' , Y . G . M a . C. M a i a n o ' , G . M a i e r , M . M a i n o ' , C. Mancini ' , C. Martinez , M . M a r t i n e z , R. H . M a r u y a m a , N . Moggi , S. Morganti , T. Napolitano*, S. Newman ' , S. N i s i , C. N o n e s ' ' , E . B . N o r m a n ' , A . N u c c i o t t i ' , F . O r i o , D. O r l a n d i , J . L . Ouellet ' , M . Pallavicini ' , V . Palmieri , L . Pattavina , M . P a v a n ' , M . P e d r e t t i , G . Pessina , S. P i r r o , E . P r e v i t a l i , V . Rampazzo , F . R i m o n d i J , C. Rosenfeld , C. Rusconi , C. S a l v i o n i , S. Sangiorgio '*, D . Schaeffer ' , N . D . Scielzo , M . S i s t i ' , A . R. S m i t h , F . Stivanello , L . Taffarello , G . Terenziani , W . D . T i a n , C. Tornei , S. Trentalange*', G . V e n t u r a ' , M . Vignati ' , B . S. W a n g ' , H . W . W a n g , C. A . Whitten J r . - \ T. Wise . A . Woodcraft , N . X u , L . Z a n o t t i ' , C. Zarra , B . X . Zhu*', S. Zucchelli J k e j w k x c c e , c b e c ab ah c (CUORE e a a c a c j e c c m aa c b,c aa,q af e a c q a a f ae a8 c ad, aa aa c e c n v e f p d e,c b c e e e c f c e s e e,c c f p,n f v ad Collaboration) a INFN - Sezione di Milano, Milano 1-20133 - Italy di Fisica e Matematica, Universita dell'Insubria, Como 1-22100 - Italy INFN - Sezione di Milano Bicocca, Milano 1-20126 - Italy Dipartimento di Ingegneria Strutturale, Politecnico di Milano, Milano 1-20133 - Italy Dipartimento di Fisica, Universita di Milano-Bicocca, Milano 1-20126 - Italy fDepartment of Physics and Astronomy, University of South Carolina, Columbia, SC 29208 - USA INFN - Laboratori Nazionali del Gran Sasso, Assergi (L'Aquila) 1-67010 - Italy Department of Physics, University of California, Berkeley, CA 94720 - USA 'Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94-720 - USA UN FN - Sezione di Bologna, Bologna 1-40127 - Italy Materials Science Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720 - USA 'Dipartimento di Fisica, Sapienza Universita di Roma, Roma 1-00185 - Italy INFN - Sezione di Roma, Roma 1-00185 - Italy INFN - Sezione di Genova, Genova 1-16146 - Italy Shanghai Institute of Applied Physics (Chinese Academy of Sciences), Shanghai 201800 - China Dipartimento di Fisica, Universita di Genova, Genova I-I6I46 - Italy Department of Physics, University of Wisconsin, Madison, WI 53706 - USA INFN - Laboratori Nazionali di Legnaro, Legnaro (Padova) 1-35020 - Italy Kamerlingh Onnes Laboratorium, Leiden University, Leiden, RA 2300 - The Netherlands INFN - Laboratori Nazionali di Frascati, Frascati (Roma) 1-00044 - Italy Centre de Spectrometrie Nucleaire et de Spectrometrie de Masse, 914-05 Orsay Campus - France b Dipartimento C d g h k M p q r f INFN - Sezione di Roma Tor Vergata, Roma 1-00133 - Italy ' 'Physics Department, California Polytechnic State University, San Luis Obispo, CA 934-07 - USA ^Department of Materials Science and Engineering, University of California, Berkeley, CA 94-720 - USA Department of Physics and Astronoma, University of California, Los Angeles, CA 90095 - USA Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94-720 - USA Lawrence Livermore National Laboratory, Livermore, CA 94-550 - USA Laboratorio de Fisica Nuclear y Astroparticulas, Universidad de Zaragoza, Zaragoza 50009 - Spain Department of Nuclear Engineering, University of California, Berkeley, CA 94-720 - USA Dipartimento di Fisica, Universita di Bologna, Bologna 1-4-0127 - Italy EH&S Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94-720 - USA flNFN - Sezione di Padova, Padova 1-35131 - Italy Dipartimento di Fisica, Universita di Firenze, Firenze 1-50125 - Italy INFN - Sezione di Firenze, Firenze 1-50125 - Italy SUPA, Institute for Astronoma, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ - UK v aa ab ac ad ae a ag ah al * C o r r e s p o n d i n g author Email addresses: e j z a k 8 w i s c . e d u ( L . E j z a k ) , s a n g i o r g i o l 8 1 1 n l . g o v (S. Sangiorgio) Presently at: Joint Research Center, Institute for Reference M a t e r i a l s and Measurements, 2440 Geel - B e l g i u m P r e s e n t l y at: Nikhef, 1098 X G A m s t e r d a m - T h e Netherlands P r e s e n t l y at: L o s A l a m o s N a t i o n a l L a b o r a t o r y , L o s A l a m o s , N M 87545 - U S A P r e s e n t l y at: C E A / Saclay, 91191 G i f - s u r - Y v e t t e - France Deceased Preprint submitted to Astroparticle Physics December
117855940
The Top $10^{500}$ Reasons Not to Believe in the Landscape
The String Landscape is a fantasy. We actually have a plausible landscape of minimally supersymmetric $AdS_4$ solutions of supergravity modified by an exponential superpotential. None of these solutions is accessible to world sheet perturbation theory. If they exist as models of quantum gravity, they are defined by conformal field theories, and each is an independent quantum system, which makes no transitions to any of the others. This landscape has nothing to do with CDL tunneling or eternal inflation. 
A proper understanding of CDL transitions in QFT on a fixed background dS space, shows that the EI picture of this system is not justified within the approximation of low energy effective field theory. The cutoff independent physics, defined by the Euclidean functional integral over the 4-sphere admits only a finite number of instantons. Plausible extensions of these ideas to a quantum theory of gravity obeying the holographic principle explain all of the actual facts about CDL transitions in dS space, and lead to a picture radically different from eternal inflation. 
Theories of Eternal Inflation (EI) have to rely too heavily on the anthropic principle to be consistent with experiment. Given the vast array of effective low energy field theories that could be produced by the conventional picture of the string landscape one is forced to conclude that the most numerous anthropically allowed theories will disagree with experiment violently.
124138605
String theory, holography and Quantum Gravity
14085873
Microscopic quantum mechanics of the p={rho} universe
We present a complete quantum mechanical description of a flat Friedmann-Robertson-Walker universe with equation of state p={rho}. We find a detailed correspondence with our heuristic picture of such a universe as a dense black hole fluid. Features of the geometry are derived from purely quantum input.
118356346
HOLOGRAPHIC SPACE–TIME AND ITS PHENOMENOLOGICAL IMPLICATIONS
I briefly review the theory of holographic space–time and its relation to the cosmological constant problem, and the breaking of supersymmetry (SUSY). When combined with some simple phenomenological requirements, these ideas lead to a fairly unique model for Tera-scale physics, which implies direct gauge mediation of SUSY breaking and a model for dark matter as a hidden sector baryon, with nonzero magnetic dipole moment.
119301083
Dirac Gluinos in the Pyramid Scheme
I point out several terms in the low energy effective Lagrangian of the Pyramid Scheme, which were missed in a previous analysis of the phenomenological consequences of the model. They lead to a Dirac contribution to the gluino mass, much larger than the one loop Majorana mass. The gluino can thus be much heavier than in previous estimates, without introducing corresponding large loop corrections to squark masses. As pointed out by a number of authors, this ameliorates the tension between the predictions of the model, and LHC data. I also point out that the model has corrections to the Higgs potential, both at the tree and loop levels, which may ameliorate fine tuning.