nove solar fin

Information about nove solar fin

Published on October 17, 2007

Author: Jancis

Source: authorstream.com

Content

Neutrino Oscillation in Venice :  Neutrino Oscillation in Venice The Solar neutrino Experiment with the ICARUS T600 detector @ Gran Sasso Lab The ICARUS Collaboration:  The ICARUS Collaboration INFN-Laboratori Nazionali del GranSasso, Italy Inst. of Exp. Physics, Warsaw University, Warsaw-Poland Inst. for Particle Physics, ETH, Zurich-Switzerland Dip.to di Fisica e INFN, Padova-Italy Dip.to di Fisica e INFN, Milano-Italy Dip.to di Fisica e INFN, Pavia-Italy Dip.to di Fisica e INFN, L’Aquila-Italy CERN, Geneva-Switzerland Dip.to Ing.Nucleare, Univ. di Milano, Milano-Italy IHEP-Academia Sinica, Beijing-China Dep.t of Physics, UCLA, LosAngeles-California, USA H.Niewodniczanski Inst. of Nucl. Phys., Krakow-Poland Inst. of Physics, Wroclaw Univ.,Wroclaw-Poland Inst. of Physics, Silesia Univ.,Katowice-Poland A. Soltan Inst. Of Nucl. Studies, Warsaw-Poland Fac. of Phys. And Nucl. Tech., Krakow-Poland ICFG-CNR and Dip.to di Fisica, Torino-Italy INFN-Laboratori Nazionali di Frascati, Roma-Italy Inst. of Physics, Jagellonian Univ., Krakow-Poland INFN-Pisa, Italy Slide3:  The ICARUS Technology (available for solar n exp.) ICARUS T600: status of the detector 1997- 2000: Realization completed (Pavia-INFN Exp. Hall) April-Aug. 2001: Full Test in experimental conditions (Pavia) 2001-2002: Transportation to LNGS (Underground Site) re-mounting and start physics run The solar neutrino experiment: Signal and Background event Rate Evaluation Signal: Based on BP98 Solar n Flux Bckgd: based on neutron flux direct measurement performed by ICARUS Collaboration at LNGS (Hall C) Signal to Background Discrimination: from full MC simulation Sensitivity to Oscillations: for different exposure time and active/sterile scenarios OUTLINE: Slide4:  wire pitch d d Drifting Ionizing Track e- Electric Field time Screen Grid Induction Plane Collection Plane Charge Induction wire Signal (schematic) Waveform T0 Tpeak Light Tdrift PMT Signal PMT UV Light ICARUS Event Stopping m and decay (3t prototype) Amplifier in LAr E1 E2 E3 Slide5:  Detector during construction LAr Cryostat (half-module) 20 m 4 m 4 m View of the inner detector Run @ Pv: full test in final experimental configuration (May-Aug) :  Run @ Pv: full test in final experimental configuration (May-Aug) Collection of large statistics of cosmic ray data with various trigger configurations: from long m tracks (up to 18 m length) to high multiplicity m bundles, to large el.m. and hadronic showers Slide7:  El.m. shower Full 2D View from the Collection Wire Plane 2 4 6 18 12 Wire coord. (m) 2 Drift coord. (m) Zoom details 1 1 3 2 2 3 m stop and decay in e Detail of a long (14 m) m track with d-ray spots El.m. shower T600 test @ Pv: Run 201 - Evt 12 Slide8:  Full 2D View from the Collection Wire Plane 2 4 12 6 18 2 Wire coord. (m) Drift Coord. (m) Zoom View Zoom View 3.1 m 0.9 m A spectacular event showing a dense Air Shower formed by hundreds of parallel tracks (muons and pions) and low energy g’s converting into electrons. Also visible in the zoom views a hadr. shower, an el.m. shower and a highly collimated muon bundle. el.m. shower had. shower m bundle T600 test @ Pv: Run 308 - Evt 4 (July 2nd, 2001) Slide9:  2 6 4 18 12 2 Wire coord. (m) Drift Coord. (m) Full 2D view from the Collection Wire Plane Zoom View 3.9 m 1.3 m Run 308 - Evt. 007 Large el.m. shower Slide10:  Sensitive to 8B component of the Solar n Spectrum n Elastic Scattering on Atomic Electrons: nx + e --> nx + e Two reactions can be exploited for Solar model independent studies GT: Gamow-Teller F : Fermi One primary e-track (above threshold) + M secondary e-tracks from Compton conversion of K* de-excitation gamma’s One isolated e-track (above threshold) with high angular correlation to the Sun direction Slide11:  EVENT Rates Inputs: BP98 n Flux (8B) Ar nuclear shell model calculation and measures on mirror nucleus n meas. @ LNGS g meas. @LNGS Tthr(e) = 5 MeV (limited by background) (Relatively) High Statistics available and reduced background, depending on the actual energy threshold: Slide12:  Real Event recorded with 50lt ICARUS Prototype 5.6 MeV e-Track End-point (Gamma source) Slide13:  a) Absorption event in two 2D views. (GEANT Montecarlo) b) Same event after digitization and hit finding algorithm. The gray scale of each pixel is proportional to the deposited charge. The resolution in the horizontal axis (drift direction) is 0.4 mm, and in the vertical axis is 3 mm (wire pitch). The projected track length is about 3 cm. The main electron energy is 7 MeV. The associated Compton energy is 2 MeV and the associated multiplicity is M=3. Assumed threshold for single Compton electron 150 keV The off-line selection between elastic and absorption events is based on the energy of the main electron (primary track) and on the total associated energy and multiplicity of secondary tracks (Compton) Slide14:  ... an other Montecarlo event (Gamow-Teller reaction) E primary electron track = 6700 keV Associated Compton energy= 2140 KeV Multiplicity of secondary tracks= 3 Compton activity limited to volume of about 50 cm radius around the primary vertex Slide15:  1 m 0.5 m e-like track ~6.5 MeV End-point 2 e-like spots from Compton conversion T600 test @ Pv: Run 785 - Evt 4 (July 22nd, 2001) 2 4 6 12 18 Drift Coord. (m) Zoom view ~800KeV ~800KeV Cosmic ray event containing a “Solar neutrino”-like signature “inverse b reaction” type with: Wire Coord. (m) Slide16:  Signal (ES, F and GT reactions) detection efficiency Background rejection power Sample contamination Full MC simulation for determination of: ES Channel 453 Background 14 F+GT Contamination 11 F+GT Channel 1616 Background 55 ES Contamination 17 Slide17:  Physics outcomes Cross-check the present solar neutrinos phenomenology with a real-time high resolution technique Direct test of the oscillations hypothesis for a good fraction of the allowed regions by means of the elastic to absorption channels ratio Discriminate active from sterile neutrino oscillations Precision test of the MSW mechanism by observation of spectral distortions (with Absorption events). Slide18:  active neutrino Active neutrino allowed regions Iso-R Curves Shaded regions: Allowed solutions from Present Solar n Exp.s (Homestake, Gallex, Sage and SuperK) [90% and 95% CL] ICARUS Sensitivity: Slide19:  Conclusions The ICARUS Technology is now fully operational at experimental scale (T600 detector is presently taking data in a surface test). After many years of technological development, it may start acting as a new, high resolution, real-time “player” in the Solar-n “game” (after installation in the GranSasso underground site). Two solar-n reactions in LAr are available, well separated in signature and available at rather large statistics for SSM model independent study. Possibility of enlarging the LAr mass at GS are under evaluation to find more about solar neutrino physics with Icarus: N.I.M. A455 (2000), 376. to find more about ICARUS: www.aquila.infn.it/icarus

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