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Status Report of the Borexino Experiment

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Experimental neutrino physics: natural beams, reactors and LBL Barbara Caccianiga-INFN Milano EPS- Conference on High Energy Physics 2015 22-29 July 2015 Vienna Neutrino Physics: the puzzle-making 2 Neutrino Physics: the puzzle-making Dm2 n2 12 2 Dm 13 3 Neutrino Physics: the puzzle-making q ~9o o 13 o ne q23~45 q12~33 n1 The Pontecorvo-Maki-Nakagawa-Sakata (PMNS) Matrix i n e 1 0 0 Dc13m2 0 s13e c12 s12 0 n1 n 12 n 0 c s 8x100 -5eV21 0 sn2 c 0 n 23 23 12 12 2 i n 0 s23 c23 s13e 0 c13 0 0 1 n 3 Dm2 13 n n 3x10-3eV2 3 44 Experimental neutrino physics: the puzzle making To complete the neutrino puzzle • Perform appearance and/or disappearance experiments using different neutrino sources and baselines; E n L n source n DETECTOR • Characteristic E/L sets the reach of the experiment in term of Dm2; • The possibility of probing different E/L within the same experiment allows to see the oscillatory pattern of appearance or disappearance thus enhancing sensitivity; 5 Experimental neutrino physics: the puzzle making To complete the neutrino puzzle • Perform appearance and/or disappearance experiments using different neutrino sources and baselines; E n L n source n DETECTOR Oscillations in vacuum (2 flavours) 2 Δmxy L P(ν ν )~sin 2 2θ sin 2 2 x y xy • Depends on E, L, Dm , q 4E 6 Experimental neutrino physics: the puzzle making To complete the neutrino puzzle • Perform appearance and/or disappearance experiments using different neutrino sources and baselines; E n L n source n DETECTOR Oscillations in matter (2 flavours) • Resonant effects for neutrinos 2 crossing matter; 2 M 2 (Δmxy )M L 2 P(νx νy )~sin 2θxy sin • Depends on E, L, Dm (also on 4E its sign!), q and r; 7 Experimental neutrino physics: the puzzle making To complete the neutrino puzzle • Perform appearance and/or disappearance experiments using different neutrino sources and baselines; E n L n source n DETECTOR Oscillations in matter (3 flavours) 2 • Depends on E, L, Dm ij, qi, CP.,.. 8 Experimental neutrino physics: the puzzle making To complete the neutrino puzzle • Perform appearance and/or disappearance experiments using different neutrino sources and baselines; E n L n source n DETECTOR NEUTRINO SOURCES - Natural sources (solar, atmosferic neutrinos) - Reactor neutrinos - Accelerator neutrinos (Long Baseline) 9 Experimental Neutrino Physics: the puzzle-making The Pontecorvo-Maki-Nakagawa-Sakata (PMNS) Matrix cij cosqij sij sinqij i n e 1 0 0 c13 0 s13e c12 s12 0 n1 n 0 c23 s23 0 1 0 s12 c12 0 n 2 atmosferic n SBL reactor n solar n accelerator in LBL reactor n n 0accelerator s23 n c23 s13e 0 c13 0 0 1 n 3 NEUTRINO SOURCES - Natural sources (solar, atmosferic neutrinos) - Reactor neutrinos - Accelerator neutrinos (Long Baseline) 10 Natural beams • Solar neutrinos • Atmosferic neutrinos 11 Natural beams Solar neutrinos E~ 1 MeV L~ 1011 m The Sun is powered by nuclear reactions which produce neutrinos pp CYCLE: ~99% of the sun energy CNO CYCLE: <1% of the sun energy Natural beams Solar neutrinos E~ 1 MeV L~ 1011 m E/L ~ 10-11 eV2 N.B.: resonance due to matter effects for E>1 MeV 2 ne disappearance: sensitive to (Dm )12+ q12 i n e 1 0 0 c13 0 s13e c12 s12 0 n1 n 0 c s 0 1 0 s c 0 n 23 23 12 12 2 i n• L is set0 by Nature,s23 c cannot23 be schanged;13e 0 c13 0 0 1 n 3 • Investigating different solar neutrino from different reactions it is possible to probe P(ne ne) as a function of E; Natural beams Solar neutrinos • I recall that the Solar Neutrino Problem was the first hint towards nu oscillations • Huge detectors based on hundreds/thousands of tons of detecting material Homestake Borexino Superkamiokande Gallex/SAGE SNO Natural beams Solar neutrinos Cerenkov Clorine Scintillator Gallium 15 Natural• Barbara beams Caccianiga -INFN Milano 50th Rencontres de Moriond- La Thuile, March 14th 21st 2015 Borexino: Nature 512, 383-386 (2014) observation of pp neutrinos (6.6 0.7)1010 cm-2s1 measured 10 -2 1 pp (5.98 0.04)10 cm s expected (high - Z) (6.03 0.04)1010 cm-2s1 expected (low - Z) Luminosity in neutrinos consistent with luminosity in photons Natural beams Solar neutrinos+KamLAND KamLAND+SOLAR 2 arXiV: 1409.4515 combined results on (Dm )12+ q12 Results from solar and KamLAND Survival probability P(ne ne) 2 0.18 5 2 Dm12 7.530.18 10 eV 2.3% precision 2 0.029 tan q12 0.4360.025 6.6% precision Oscillations Oscillations in vacuum in matter Natural beams Solar neutrinos+KamLAND What Next? Small tension (~2s ) in Dm2 between solar and KamLAND data Gonzales-Garcia,Maltoni,Schwetz . arXiV: 1409.5439 Tension comes from 1) no up-turn seen in the 8B spectrum so far; 2) indication for a non vanishing D/N asymmetry in SK; Non-standard interactions and super-light sterile neutrino? arXiV:1101.3875, arXiV:1307.3092, arXiV:1012.5627 Study transition region between vacuum and matter oscillation regime Natural beams Atmosferic neutrinos E~ 1 GeV L~ 104-107 m Secondary products of cosmic rays in the atmosphere ne, anti- ne, n, anti- n; BASELINE L ENERGY selecting q is equivalent to select L Natural beams Atmosferic neutrinos E~ 1 GeV L~ 104-107 m E/L ~ 10-3 eV2 n , anti- n disappearance 2 sensitive to (Dm )23+ q23 ne , anti- ne appearance First evidence of oscillations in this sector! Y. Fukudae (Super-Kamiokande Collaboration) et al. (1998). "Evidence for Oscillation of Atmospheric Neutrinos". Physical Review Letters 81 (8): 1562–1567. Natural beams Atmosferic neutrinos and neutrino mass hierarchy • Matter effects introduce a dependence on the sign of Dm2 and on the sign of A, where for n and anti- n respectively (Dm2 )m L PM (ν ν ) PM (ν ν ) sin 2θ sin 2 2θmsin 2 13 e μ μ e 23 13 4E sin22θ sin22θm 13 13 2 2 2G N E sin22q cos2q F e • resonance occurs when 13 13 Δm2 13 2 2 Dm13 cos(2q13 ) 2 2GF Ne E 2 2G N E (Dm2 )m Δm2 sin22q cos2q F e 13 13 13 13 Δm2 13 • This condition is met when E~30 GeV/r [g cm-3] for 1 GeV<E<20 GeV Natural beams Atmosferic neutrinos and neutrino mass hierarchy P(n n ) • Map upward n flux in bins Normal Hierarchy Inverted Hierarchy of (E,cosq); • cosq= -1 L~12000 Km; Letter of Intent PINGU- arXiV:1401.2046 Natural beams Atmosferic neutrinos and neutrino mass hierarchy P(anti-n anti-n ) Inverted Hierarchy Normal Hierarchy Note that: P(n n ) in NH P(n n )in IH • If it is not possible to distinguish between n and anti-n the effect of hierarchy washes out; • Fortunately s (n ) s (n ) and (n ) (n ) possible to see a few % effect due to hierarchy Letter of Intent PINGU- arXiV:1401.2046 Natural beams Atmosferic neutrinos and neutrino mass hierarchy • In the framework of IceCube and Km3NET; • Instrument ~ Mtons of ice (PINGU) or sea-water (ORCA) • Fine granularity to have low threshold; PINGU ORCA ..or alternatively use a magnetized 50 kton detector which is capable of distinguishing neutrinos from anti-neutrinos (INO project).. Natural beams Reactor neutrinos 25 Reactors Reactor neutrinos Reactor neutrinos: anti- ne mainly coming from the beta-decay of the fission products of 235U, 238U, 239Pu and 241Pu; E~ 5 MeV Detecting reaction: 3- 5 inverse beta decay L~ 10 10 m • CRITICAL: Systematics associated to the reactor n spectrum (depending on the fuel composition) Near and far detector; Reactors Reactor neutrinos antine disappearance Dm2 L Dm2 L Dm2 L 2 2 2 13 2 2 23 4 2 2 12 P(n e n e ) 1 sin 2q13 cos 2q12 sin sin 2q12 sin cos q13 sin 2q12 sin 4E 4E 4E Daya Bay ~60 km ~180 km JUNO KamLAND L ~ 180 Km 2 sensitive to (Dm )12+ q12 (solar term) Reactors Reactor neutrinos antine disappearance Dm2 L Dm2 L Dm2 L 2 2 2 13 2 2 23 4 2 2 12 P(n e n e ) 1 sin 2q13 cos 2q12 sin sin 2q12 sin cos q13 sin 2q12 sin 4E 4E 4E Daya Bay 2 2 2 Dmee L ~60 km sin 2q sin ~180 km 13 4E JUNO KamLAND L ~ 1.5 Km 2 sensitive to (Dm )13+ q13 Reactors Reactor neutrinos: Double-Chooz, RENO and Daya-Bay Double Chooz: • so far results only with the far detector • near detector takes data since dec 2014 (first results with both detectors by end of 2015) Daya-Bay: deeper, higher nuclear plant power, more far/near detectors, more favourable baseline; Reactors Reactor neutrinos: results on q13 RESULTS FROM DAYA-BAY (Moriond 2015) • Best precision on q13 measurement (~6%) 2 0.005 sin 213 0.0840.005 2 0.10 3 2 Δmee 2.440.11 10 eV χ 2/NDF 134.7/146 Reactors Reactor neutrinos antine disappearance Dm2 L Dm2 L Dm2 L 2 2 2 13 2 2 23 4 2 2 12 P(n e n e ) 1 sin 2q13 cos 2q12 sin sin 2q12 sin cos q13 sin 2q12 sin 4E 4E 4E Daya Bay ~60 km JUNO ~180 km KamLAND L ~ 60 Km sensitive to mass hierarchy Reactors Reactor neutrinos: the JUNO proposal antine disappearance Dm2 L Dm2 L Dm2 L 2 2 2 13 2 2 23 4 2 2 12 P(n e n e ) 1 sin 2q13 cos 2q12 sin sin 2q12 sin cos q13 sin 2q12 sin 4E 4E 4E Daya Bay ~60 km JUNO ~180 km Exploit interference in KamLAND n oscillations between atmospheric and solar term; • It is feasible because q13 is relatively large! • Unlike accelerator or atmosferic experiments this technique doesn’t depend on CP and q23 ; Reactors Reactor neutrinos: the JUNO proposal antine disappearance Dm2 L Dm2 L Dm2 L 2 2 2 13 2 2 23 4 2 2 12 P(n e n e ) 1 sin 2q13 cos 2q12 sin sin 2q12 sin cos q13 sin 2q12 sin 4E 4E 4E Exploit interference in n oscillations between atmospheric and solar term; Requires exceptional energy resolution Reactors Reactor neutrinos: the JUNO proposal Precision < 1% ! Civil construction: 2015-2017; Detector Installation:2016-2019; Filling and
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  • Icecube and Km3net: Lessons and Relations

    Icecube and Km3net: Lessons and Relations

    Elsevier Science 1 Journal logo IceCube and KM3NeT: Lessons and Relations Christian Spiering DESY, Platanenallee 6, Zeuthen, 15738 Germany Elsevier use only: Received date here; revised date here; accepted date here Abstract This talk presents conclusions for KM3NeT which may be drawn from latest IceCube results and from optimization studies of the IceCube configuration. It discusses possible coordinated efforts between IceCube and KM3NeT (or, for the time being, IceCube and ANTARES). Finally, it lists ideas for formal relations between neutrino telescopes on the cubic kilometer scale. © 2001 Elsevier Science. All rights reserved Keywords: Neutrino Telescopes 1. Introduction The IceCube neutrino telescope at the South Pole Assuming one detector on the Southern is approaching its completion and meanwhile has hemisphere (IceCube) and one or more detectors at provided first results from data taken with initial the Northern hemisphere (by now ANTARES [10] configurations [1]. KM3NeT will act as IceCube’s and NT200 [11], in the future KM3NeT [12] and counterpart on the Northern hemisphere, with a GVD [13]), various possibilities for coordinated sensitivity “substantially exceeding that of all physics programs and analyses open up. They are existing neutrino telescopes including IceCube” [2]. discussed in sections 3 and 4. KM3NeT is just finishing its design phase [3], but Finally, section 5 lists formal and procedural has not yet converged to a final configuration. The possibilities of cooperation between KM3NeT and cited sensitivity requirement results not only from IceCube. gamma ray observations and their phenomenological interpretation (see e.g. [4-9]), but also from early IceCube data. The first section of this paper is 2.