119028956
No Firewalls in Holographic Space-Time or Matrix Theory
We use the formalisms of Holographic Space-time (HST) and Matrix Theory[11] to investigate the claim of [1] that old black holes contain a firewall, i.e. an in-falling detector encounters highly excited states at a time much shorter than the light crossing time of the Schwarzschild radius. In both formalisms there is no dramatic change in particle physics inside the horizon until a time of order the Schwarzschild radius. The Matrix Theory formalism has been shown to give rise to an S-matrix, which coincides with effective supergravity for an infinite number of low energy amplitudes. We conclude that the firewall results from an inappropriate use of quantum effective field theory to describe fine details of localized events near a black hole horizon. In both HST and Matrix Theory, the real quantum gravity Hilbert space in a localized region contains many low energy degrees of freedom that are not captured in QU(antum) E(ffective) F(ield) T(heory) and omits many of the high energy DOF in QUEFT.
125302371
Cosmological SUSY Breaking and the Pyramid Scheme
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.
124138605
String theory, holography and Quantum Gravity
119283684
Holographic Space-time and Newton's Law
We derive Newton's Law from the formalism of Holographic Space-Time (HST). More precisely, we show that for a large class of Hamiltonians of the type proposed previously for the HST description of a geodesic in Minkowski space, the eikonal for scattering of two massless particles at large impact parameter scales as expected with the impact parameter and the energies of the particles in the center of mass (CM) frame. We also discuss the criteria for black hole production in this collision, and find an estimate, purely within the HST framework, for the impact parameter at which it sets in, which coincides with the estimate based on general relativity.
116990186
Essay: Supersymmetry, the Cosmological Constant, and a Theory of Quantum Gravity in Our Universe
There are many theories of quantum gravity, depending on asymptotic boundary conditions, and the amount of supersymmetry. The cosmological constant is one of the fundamental parameters that characterizes different theories. If it is positive, supersymmetry must be broken. A heuristic calculation shows that a cosmological constant of the observed size predicts superpartners in the TeV range. This mechanism for SUSY breaking also puts important constraints on low energy particle physics models.
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.
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.
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
73646575
Initial performance of the CUORE-0 experiment
CUORE-0 is a cryogenic detector that uses an array of tellurium dioxide bolometers to search for neutrinoless double-beta decay of $$\mathrm {^{130}Te}$$130Te. We present the first data analysis with $$7.1 \,\mathrm {kg\cdot y}$$7.1kg·y of total $$\mathrm {TeO_2}$$TeO2 exposure focusing on background measurements and energy resolution. The background rates in the neutrinoless double-beta decay region of interest (2.47 to $$2.57 \,\mathrm {MeV}$$2.57MeV) and in the $$\alpha $$α background-dominated region (2.70 to $$3.90\,\mathrm {MeV}$$3.90MeV) have been measured to be $${0.071\pm 0.011}$$0.071±0.011 and $${0.019\pm 0.002}\,\mathrm {counts/(keV\cdot kg\cdot y)}$$0.019±0.002counts/(keV·kg·y), respectively. The latter result represents a factor of 6 improvement from a predecessor experiment, Cuoricino. The results verify our understanding of the background sources in CUORE-0, which is the basis of extrapolations to the full CUORE detector. The obtained energy resolution (full width at half maximum) in the region of interest is $$5.7\,\mathrm {keV}$$5.7keV. Based on the measured background rate and energy resolution in the region of interest, CUORE-0 half-life sensitivity is expected to surpass the observed lower bound of Cuoricino with one year of live time.
54913753
Searching for Neutrinoless Double-Beta Decay of130Te with CUORE
Neutrinoless double-beta (0) decay is a hypothesized lepton-number-violating process that offers the only known means of asserting the possible Majorana nature of neutrino mass. The Cryogenic Underground Observatory for Rare Events (CUORE) is an upcoming experiment designed to search for 0 decay of 130Te using an array of 988 TeO2 crystal bolometers operated at 10 mK. The detector will contain 206 kg of 130Te and have an average energy resolution of 5 keV; the projected 0 decay half-life sensitivity after five years of livetime is 1.6 × 1026 y at 1 (9.5 × 1025 y at the 90% confidence level), which corresponds to an upper limit on the effective Majorana mass in the range 40–100 meV (50–130 meV). In this paper, we review the experimental techniques used in CUORE as well as its current status and anticipated physics reach.