Neutrino Oscillation in Venice The Solar neutrino Experiment

Neutrino Oscillation in Venice The Solar neutrino Experiment with the ICARUS T 600 detector @ Gran Sasso Lab July 24 th, 2001 NO-VE Workshop 1

The ICARUS Collaboration ( ( ( ( ( July 24 th, 2001 INFN-Laboratori Nazionali del Gran. Sasso, 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, Los. Angeles-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 NO-VE Workshop 2

OUTLINE: • The ICARUS Technology (available for solar n exp. ) • ICARUS T 600: 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 BP 98 Solar n Flux • Bckgd: based on neutron flux direct measurement performed by ICARUS Collaboration at LNGS (Hall C) • Signal to Background Discrimination: • Sensitivity to Oscillations: July 24 th, 2001 from full MC simulation for different exposure time and active/sterile scenarios NO-VE Workshop 3

Electric Field Ionizing Track PMT ICARUS Event UV Light Drifting ein LAr E 1 Stopping m and decay (3 t prototype) Screen Grid d E 3 Induction Plane Amplifier July 24 th, 2001 Collection NO-VE Workshop Plane Charge d E 2 T 0 Light wire pitch Induction wire Signal (schematic) Waveform Tdrift Tpeak PMT Signal time 4

LAr Cryostat (half-module) View of the inner detector 4 m 4 m 20 m Detector during construction July 24 th, 2001 NO-VE Workshop 5

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 July 24 th, 2001 NO-VE Workshop 6

2 Full 2 D View from the Collection Wire Plane Drift coord. (m) 1 3 2 2 4 Zoom details 6 Wire coord. (m) 12 18 T 600 test @ Pv: Run 201 - Evt 12 1 El. m. shower 2 m stop and decay in e Detail of a long (14 m) m track with d-ray spots 3 July 24 th, 2001 El. m. shower. NO-VE Workshop 7

Full 2 D View from the Collection Wire Plane 2 Drift Coord. (m) 4 2 6 Wire coord. (m) 12 18 Zoom View 3. 1 m Zoom View m bundle had. shower el. m. shower July 24 th, 2001 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. NO-VE Workshop T 600 test @ Pv: Run 308 - Evt 4 (July 2 nd, 2001) 8

Full 2 D view from the Collection Wire Plane 2 Drift Coord. (m) 2 4 6 Wire coord. (m) 12 18 Zoom View 3. 9 m 1. 3 m Run 308 - Evt. 007 Large el. m. shower July 24 th, 2001 NO-VE Workshop 9

GT: Gamow-Teller F : Fermi • Sensitive to 8 B component of the Solar n Spectrum • Two reactions can be exploited for Solar model independent studies n Elastic Scattering on Atomic Electrons: nx + e --> nx + e 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

(Relatively) High Statistics available and reduced background, depending on the actual energy threshold: Tthr(e) = 5 Me. V (limited by background) EVENT Rates Inputs: • BP 98 n Flux (8 B) • Ar nuclear shell model calculation and measures on mirror nucleus • n meas. @ LNGS • g meas. @LNGS July 24 th, 2001 NO-VE Workshop 11

Real Event recorded with 50 lt ICARUS Prototype 5. 6 Me. V e-Track (Gamma source) End-point July 24 th, 2001 NO-VE Workshop 12

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) a) Absorption event in two 2 D 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 Me. V. • The associated Compton energy is 2 Me. V and the associated multiplicity is M=3. Assumed threshold for single Compton electron 150 ke. V July 24 th, 2001 NO-VE Workshop 13

. . . an other Montecarlo event (Gamow-Teller reaction) E primary electron track = 6700 ke. V Associated Compton energy= 2140 Ke. V Multiplicity of secondary tracks= 3 Compton activity limited to volume of about 50 cm radius around the primary vertex July 24 th, 2001 NO-VE Workshop 14

Drift Coord. (m) 2 4 6 12 Zoom view • e-like track ~6. 5 Me. V End-point 0. 5 m • 2 e-like spots from Compton conversion ~800 Ke. V 1 m ~800 Ke. V T 600 test @ Pv: Run 785 - Evt 4 (July 22 nd, 2001) 18

Full MC simulation for determination of: • Signal (ES, F and GT reactions) detection efficiency • Background rejection power • Sample contamination ES Channel 453 Background 14 F+GT Contamination 11 F+GT Channel Background ES Contamination July 24 th, 2001 1616 55 17 NO-VE Workshop 16

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). July 24 th, 2001 NO-VE Workshop 17

ICARUS Sensitivity: Iso-R Curves Active neutrino allowed regions Shaded regions: Allowed solutions from Present Solar n Exp. s (Homestake, Gallex, Sage and Super. K) [90% and 95% CL] July 24 th, 2001 NO-VE Workshop active neutrino 18

Conclusions • The ICARUS Technology is now fully operational at experimental scale (T 600 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 Gran. Sasso 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. A 455 (2000), 376. * to find more about ICARUS: www. aquila. infn. it/icarus July 24 th, 2001 NO-VE Workshop 19