LNGS Prima misura on line di neutrini solari a bassa energia (sub-MeV) - Borexino Prime misure su un fascio di neutrini long baseline (  appearence) -

Presentazione sul tema: "LNGS Prima misura on line di neutrini solari a bassa energia (sub-MeV) - Borexino Prime misure su un fascio di neutrini long baseline (  appearence) -"— Transcript della presentazione:

1 LNGS Prima misura on line di neutrini solari a bassa energia (sub-MeV) - Borexino Prime misure su un fascio di neutrini long baseline (  appearence) - Opera Monitor continuo di collassi gravitazionali - LVD Leader in LAr detectors for particle and astroparticle physics - Icarus Eccellenza a livello internazionale: Materia oscura - Dama/Libra, Cresst, Warp, Xenon Natura del neutrino - Cuore, Gerda Astrofisica nucleare - Luna

2 CONCLUSIONI I Laboratori del Gran Sasso costituiscono una grande risorsa per l’INFN. Stanno entrando in una seconda fase della loro vita, particolarmente ricca di attività con grande potenzialità di scoperta. I prossimi mesi saranno cruciali per il completamento dei lavori di messa in sicurezza e di up grade degli impianti che renderanno possibile realizzare questo ambizioso programma scientifico. Le risorse finanziarie e umane vanno adeguate alla nuova fase. Regole nuove per le Collaborazioni. La realizzazione di una nuova infrastruttura sotterranea, poco profonda, per un grande rivelatore ad Argon liquido che consenta nuovi studi sul decadimento del protone, sui neutrini astrofisici e su un futuro fascio artificiale è considerata di grande interesse dalla comunità. Il Gran Sasso può giocare un ruolo decisivo.

3 Occupancy Borexino OPERA HALL C HALL B HALL A LVD CRESST CUORE CUORICINO LUNA2 D AMA/LIBRA GENIUS-TF MI R&D XENON ICARUS GERDA WARP VIP LOW ACTIVITY LAB LISA BAM - OPERA WARP 2.3l

4 CNGS beam optimized for appearance 732 Km Given the distance:  flux optimized for the maximal number of  charged current interactions 17 GeV ( e + e )/  0.87%  /  2.1%  prompt negligible

5 The CNGS beam is operating smoothly with very good quality The tracking detectors of OPERA are taking data with practically no dead time More than 300 beam correlated events have been registered with a clean time distribution The recorded events show the expected tracking performances Correlation between tracks measured in the tracking detectors and emulsions installed in the target have been observed (work in progress) OPERA is now preparing the next step:  observing neutrino interactions in the Emulsion Cloud Chamber bricks Next step : end of october run !!! August run conclusions

6 Brick mass production Ad oggi sono stati prodotti 108 mattoni (tutti rispondenti alle specifiche) di cui: 70 anche nastrati con Alluminio 35 completi e forniti al BMS per prove di manipolazione automatica sul rivelatore in sala C Le 5 stazioni di impilaggio pressa sono in fase di messa a punto sullo sfogliamento piombo, fase resa piu’ complessa dall’elevato livello di auto-incollaggio delle lastrine di piombo Il 28 settembre arriva una nuova consegna di piombo con le modifiche richieste alla linea automatica di lavaggio e asciugatura. Se non si riscontrano problemi di sfogliamento si intende iniziare la produzione di massa dei mattoni dalla settimana prossima raggiungendo gradualmente la velocita’ nominale

7 Inclusive deep inelastic neutrino spectrum from CNGS as a function of the energy Neutrino electron events due to the intrinsic e contamination are shown as a function of the energy. They are very small (<0.5 %) below 30 GeV and rise at high energies. Systematic error is small (<5%).

8 Sensitivity region, in terms of Standard Deviations , for 6000 raw CNGS neutrino events. T600 at the CNGS offers an unique possibility of searching for sterile neutrinos, largely complementary and comparable to the Fermilab programme.

9 How many  are necessary  The branching ratio for  => e  is 16%; hence we expect 13.4 electron deep inelastic events, in addition to the ≈ 14 intrinsic beam associated e with energy <20 GeV. This is already per-se a significant effect, namely with 27.4 electron events observed vs. 14 ± 3.7 expected (3.6 s.d.). Events are absolutely clean and they are characterised by a momentum unbalance because of neutrino emission and a relatively low electron momentum. Selection criteria suggest a sufficiently clean separation from intrinsic beam associated e with kinematic cuts and an efficiency of 50%. Therefore one should expect about 7 ± 2.6  => e  events, some of which, hopefully, gold plated. This should be sufficient for a proof of existence, the actual value of  m 2 being already measured elsewhere in Soudan and S-K. At the effective neutrino energy of 20 GeV and  m 2 = 2.5E-3 eV 2, the expected  =>  is 1.4%. Therefore for 6000 CNGS events in the T600 we expect 84 raw  events.

10 Both cryostats @ final position:January 2007 Top cold shielding installed:February 15 th 2007 Cryogenic roof pass-through in place: Top insulation assembled on site: 15th March 2007 end March 2007 Installation of the rack supports: Instrumentation cryo-plant: April 2007 June 2007 Readout electronics in place & cabling:Start April 2007 N 2 and Ar circuits assembly: April/July 2007 Summarising ICARUS Bottom & lateral insulation @ LNGS: September 2006 … then :

11 Then… the start up.  Filling with the cryogenic liquids. “Power on”  Cooling down.  Cleaning cryostats.

12 Stato di Borexino durante il CNGS run di Agosto Riempimento della sfera iniziato il 1° August 2006 55 t di acqua  Durante il run contenuti nella sfera circa 55 t di acqua  Altezza dell’acqua rispetto al fondo della sfera circa 1.8 m  Superficie attiva ~ 10.5 m 2 Beam direction

13 WARP 140-kg Detector Passive neutron and gamma shield Active Veto 100 liters Chamber The WARP 140-kg detector to be installed and commissioned at LNGS- 140 kg active target, will possibly allow to reach into 10 -45 cm 2 covers most critical part of SUSY parameter space Complete neutron shield! 4π active neutron veto (9 tons Liquid Argon, 300 PMTs) 3D Event localization and definition of fiducial volume for surface background rejection Detector designed for positive confirmation of a possible WIMP discoveryActive control on nuclide-recoil background, owing to unique feature (LAr active veto) Cryostat designed to allocate a possible 1400 kg detector

14 140 kgs Detector: Schedule

15 10-15 cm thick Cu shield HP LAr in 4.2 m diameter SS cryostat HP water in 10 m diameter SS vessel Neutron moderator Cherenkov medium for µ veto GERDA Naked crystals in ultra-pure liquid proposed by G. Heusser, Ann. Rev. NPS 45 (1995) 54

16 Pulse Shape Analysis to select SSE  Claim: 4.2  signal Expected @ Q   2039.006±0.05 keV T 1/2 = 1.2 10 25 yr (± .69-4.18 yr) M ee ≈ 440 meV (100-900) KK Matr. El. M ee ≈700 meV Rodin et al. Matr. El. H.V. Klapdor-Kleingrothaus, et al. [ Phys.Lett. B586:(2004)198] MT = 10.9 kg (86% 76 Ge) x 13 yr Exposure (analysis): 50.57 kg y b = 0.11 yDRU before PSA Resolution on 8 years  = 3.27 keV 214 Bi 

17 GERDA Goals & Sensitivity

18 Mosè Mariotti, Assergi 26/09/2006 The second telescope Structure finished in December 2005 (in schedule) Structure finished in December 2005 (in schedule) Drive motors on Drive motors on Camera: ongoing production Camera: ongoing production Mirrors: 1/3 funded, now in production Mirrors: 1/3 funded, now in production Electronics: sampling & readout prototype ready, production pending Electronics: sampling & readout prototype ready, production pending Trigger: production pending Trigger: production pending Second telescope is important to overtake HESS’ sensitivity with lower energy threshold Second telescope is important to overtake HESS’ sensitivity with lower energy threshold HESS has just finished the foundations of its 5 th telescope, the “big one”, which should lower the threshold below MAGIC HESS has just finished the foundations of its 5 th telescope, the “big one”, which should lower the threshold below MAGIC Presently, thanks to our lower threshold, we have canceled the gap with HESS, but we risk to be again rushing to get them… Presently, thanks to our lower threshold, we have canceled the gap with HESS, but we risk to be again rushing to get them…

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20 CU integration completed at INFN-Pisa may 19 2006 The GLAST-LAT Calibration Unit tower 3 tower 2 tower 1 bay 0 CAL 101 CAL 119 CAL 109 TKR 8 TKR 16 2.5 towers, >1/8 of the LAT 110k Si strip 288 CsI logs + 5 ACD tiles on ISC

21 First results by IGEC2 6 month of data of AURIGA-EXPLORER-NAUTILUS May 20 - Nov 15, 2005 IGEC2 was the only gw observatory in operation search for transient gw signals to identify single candidates with high confidence : triple coincidences false alarm rate of 1 per century wider target signals than IGEC1 no candidates found

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23 AURIGA at design sensitivity (T=4.5K) Theoretical prediction by three-modes numerical model (spurious modes not included!). Most parameters of the model directly measured “in situ” or in separated bench tests (Transducer Test Facility). Mechanical Q set to: Q bar =4  10 6 Q tr =1.5  10 6 all noise sources scale with T (one-sided spectra) (FWHM) bandwidth enlarged:  26 Hz (1st run  1 Hz) T eff =300  K or 7800  at T=4.5K (1st run T eff >1mk at T=0.2K)