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Summary of astroparticle physics at LNF

Summary of astroparticle physics at LNF. Astroparticle physics at INFN and LNF NAUTILUS/EXPLORER Update on OPERA/CNGS Physics in space: perspectives at LNF The PVLAS anomaly and its troubled fate Brief remainder of the other activities (NEMO, BENE, ICARUS) Conclusions. F. Terranova, LNF.

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Summary of astroparticle physics at LNF

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  1. Summary of astroparticle physics at LNF Astroparticle physics at INFN and LNF NAUTILUS/EXPLORER Update on OPERA/CNGS Physics in space: perspectives at LNF The PVLAS anomaly and its troubled fate Brief remainder of the other activities (NEMO, BENE, ICARUS) Conclusions F. Terranova, LNF

  2. Activities at INFN (table) and LNF (exp in shaded areas) 0-3 Full time equivalent physicists and engineers (FTE) 3-8 FTE >8 FTE

  3. } National trend (INFN) Local trend (LNF) 36 in 2008 28 in 2008 11 in 2008 6.4 in 2008

  4. Calibration signal ROG – Status of the detectors Since 2003 in continuous data taking with a sensitivity 8·10-22<Sh1/2<10-20 within 40 Hz bandwidth Analysis of the Explorer-Nautilus coincidences in the years 2001 and 2003 already published, in progress for 2004 NAUTILUS DUTY CYCLE ~95% (single antenna) 90% (coincident operation) EXPLORER

  5. Another excellent application of the BTF facility First results with Al5056 bar Superconducting state: provides an explanation of the CR effect observed by Nautilus Normal-SC transition: to be better understood Normal (non-SC) state Nb data in SC and normal states: Europhys. Lett., 76 (6), pp. 987–993 (2006)

  6. IGEC2 joint search for GW burst events: first results form May-December 2005 Phys.Rev.D76:102001,2007 NEW UPPER LIMIT ON THE BURST RATE IGEC 2006 data analysis in progress: • No detector 0.9 days • Single 19.9 days • Double 140.8 days • Triple249.4days 95% coverage IGEC2

  7. Resonant bar detectors • Very well know detectors: crewless operation and CR effects understood • Exclude the existence of nearby (~100 pc) GW bursters giving pulses with relatively high SNR and rate of the order of 1/y. • They will have a crucial survey role between Ott.2007 – and summer 2009, i.e. after VIRGO-vsr1 / LIGO-S5 and before VIRGO+ / eLIGO; • Correlated data taking with interferometers; HOWEVER: • Sensitivity significantly worse than present VIRGO and LIGO EXPLORER 05 07 1990 91 92 93 94 95 96 97 98 99 02 01 03 04 06 00 01 03 04 IGEC2 NAUTILUS Major upgrades 96 97 98 99 02 04 01 03 06 00 05 07

  8. Containers for the emulsion-lead bricks (« walls ») OPERA-LNF General support structure Scintillators Magnets Veto RPC Drift tubes Brick insertion machine Automatic scanning of nuclear emulsion LNF projects Projects with partecipation of LNF Brick production machine (“BAM”) Non-LNF projects

  9. The brick production saga and …its happy end  • The Brick Assembling Machine (“BAM”) was conceived to maximize the brick quality stability in a mass production mode. Goal was to produce 936 bricks/day. • BAM construction started in march 2005 in firm site (Pavia, Italy). Delivered in Gran Sasso in June 2006 with a few months of delay and without a complete commissioning in firm. • Startup of mass production was extremely troublesome due to the lack of optimization of the whole chain w.r.t. the actual lead-emulsion input materials (800 bricks produced in 3 weeks!!) • Major interventions up to March March: ~60 bricks/day April: ~200 bricks/day May: ~450 bricks/day July: ~590 bricks/day October: ~650-700 bricks/day October 31st, for 66973: 42% of OPERA Estimated end of production: June 2007 Many people at LNF contributed to the operation and complete re-optimization of the BAM:, G.Catitti (SSCR), A.Ceccarelli (SSCR), U.Denni (SEA), A.Franceschi (SSCR), C.Fusco (Div-Acc), N.Intaglietta (SSCR), T. Napolitano (SSCR), A.Tiburzi (SSCR), T.Tonto (EDP), M.Ventura (DR) and both LNF and INFN strongly supported this enterprise.

  10. The 2007 CNGS run • At current brick filling time of OPERA we would have expected between 150-200 events into the bricks depending on the CNGS max intensity and duty cycle. We got only 38 (exp for 0.824 1018 pot: 34.6) due to several problems at CNGS: • Repair of conductors [origin of the problem due to forces + brazing, seen also in K2K] • Problem at the ventilation (tried a temporary fix) • Early shutdown: The electronics controlling the cooling/ventilation system and temperature monitoring started going in a faulty status, this then became irrecoverable for some units and bringing to a complete loss of communication [location of PLC’s etc. is incompatible with local neutron fluence] Possible damage to materials without cooling. Ventilation operating in non standard mode and conflicting with the access procedures with a violation of INB rules Many concerns have been raised by OPERA and INFN to CERN DG since the problems indicate that a revision of the CNGS operation at high intensity is very urgent: restart CNGS “as a project” and not only as a SPS beamline; allocate appropriate manpower In spite of this, the location of the internal events has been a crucial step in the validation of the OPERA concept and it allowed to test the whole analysis chain: brick finding with real-time detector, brick extraction, development and scanning

  11. REAL TIME DETECTORS EMULSIONS CC NC

  12. PAMELA Launched in orbit on June 15, 2006, on board of the DK1 satellite by a Soyuz rocket from the Bajkonour launch site. Since July 11, 2006, Pamela is in continuous data taking mode Till the 30th of August PAMELA has collected data for about 29.3x106 seconds corresponding to about 340 days (~8100h) of continuous data taking (7x108 events) . Data analysis up to 30/4/07 • Activities at LNF: • Testbeams at CERN and GSI: high energy protons, electrons (>200 GeV) and nuclei • Data taking (Moscow) and analysis

  13. Preliminary !!! Transitory events: Moreton Wave, Dec 2006 Galactic H and He spectra

  14. LARES • A 1% test of Lense-Thirring using purely passive satellites tracked by Earth-based lasers • Extension of the technique used by Ciufolini et al. (*) to test at 10% level the effect using 11 y of data from LAGEOS 1&2 and the recent data of GRACE • A purely passive satellite: • Full tungsten-alloy body • Weight/Ø ~ 400 Kg / 386 mm (baseline option) • Aimed at minimizing non-gravit. perturb.  Surface/ Mass (M/S) of LARES ~ 2.8  (M/S) of LAGEOS • A dedicated space climate facility at LNF for thermal and optical calibration • Emissivity/reflectivity of reflectors (CCR) and tungsten alloy (W) • Tsurface of CCR and W-alloy • Thermal relaxation time of CCR (tCCR) and of W rings (tW-RING) • Far field diffraction patters (FFDP) of each CCR in air • FFDP of each CCR in varying space climatic conditions (*) I.Ciufolini and E.C.Pavlis, Nature 431, 2004

  15. Integrated LARES thermal and optical tests at SCF Rotation/tilt from top flange Spare window Solar Simulator LASER window 532 nm laser 2nd optical table; now operational IR camera window CCD

  16. ETRUSCO, space experiment on GNSS Space qualification of laser ranging to Global Navigation Satellite System (GALILEO, GPS-3) INSTITUTES INFN-LNF (PI) ITALIAN AIR FORCE (CO-PI) INTERNATIONAL LASER RANGING SERVICE ASI - CENTER FOR SPACE GEODESY @ MATERA UNIV. OF MARYLAND NASA-GSFC UNIV. OF BOLOGNA INDUSTRIAL PARTNERS KAYSER ITALIA G&A ENGINEERING EXPLORA

  17. NEMO-LNF BENE-INFN Absolute measurements of water trasparency (the NERONE facility) 2006: first results 2007: new measurements in the Km3 candidate site (blu and green light laser) NERONE2: long-term underground measurements (re-engineering of the project) At LNF mainly focused on high energy Beta Beams and emulsion detectors for the Neutrino Factories ICARUS and LAr/LXe R&D

  18. B = 0 B = 5.5 T PVLAS From 2000 evidence of birefringence and dicroism Phys.Rev.Lett.96:110406,2006 • Change in laser (100  800 mW) • Improved screening of cables • Screening of the connection circuit to mu-metal • Helmholtz coils along the mirrors • Initial polarization rotated by 54˚ • New compressor for He recuperation

  19. Conclusions Astroparticle physics at INFN is pursued both in large collaborations and in university-size experiments: a very healthy approach that has been attracting many people and ideas in the last decade. • LNF is giving major contributions to the search of GW with resonant bars and to the CNGS physics programme. • These activities are of medium and long range (2-5 years) • Activities related with astroparticle and fundamental physics in space are growing with time both at INFN and LNF • Rather broad range: • Neutrinos: OPERA, ICARUS, BENE • Astroparticle underwater: NEMO • Astroparticle in space (WIZARD/PAMELA) • Gravitational wave: NAUTILUS/EXPLORER • Fundamental physics in space (LARES) and in lab (PVLAS)

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