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52° International Winter Meeting on Nuclear Physics Status of art of FARCOS Project L. Acosta2,8, F. Amorini2, A. Anzalone2, L. Auditore4,5, G. Cardella1, E. De Filippo1, L. Francalanza2,3, R. Gianì2,3, G. Lanzalone2,7, I. Lombardo6, T. Minniti4,5, E. Morgana5, S. Norella5, A. Pagano1, E.V. Pagano2,3, M. Papa1, S. Pirrone1, G. Politi1,3, L. Quattrocchi4,5 ,F. Rizzo2,3, P. Russotto1, A. Trifirò4,5, M. Trimarchi4,5, G. Verde1 1. INFN Sezione di Catania 2. INFN LNS 3. Dipartimento di Fisica e Astronomia Università di Catania 4. INFN_Gruppo Collegato di Messina 5. Dipartimento di Fisica e Scienze della Terra Università Messina 6. INFN-Sezione di Napoli and Dipartimento di fisica Università di Napoli Federico II 7. Università Kore Enna 8. Departamento de Física Aplicada, Universidad de Huelva, Huelva, Spain OUTLINE FARCOS physics cases Simulation results Test on CsI(Tl) crystals Test on DSSSD strip detectors New front-end electronics planned Conclusions and perspectives 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration FARCOS PHYSYCS CASES (1) 1- Dynamics in heavy-ion collisions (low and intermediate energies, stable beams and RIB) -Femtoscopy: space time probes of light particle emitting source 2- Invariant mass spectroscopy (with stable and exotic fragmentation beams) -Multi-particle decay correlations -Cluster states (alpha-conjugate, boson condensates) G. Verde et al., PRC 65 (2002) 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration → p+ 7Be W.Tan, PRC 2004 8B FARCOS PHYSYCS CASES (2) p-p Correlation Efficiency curve Granularity=7° High resolution is necessary in order to reconstruct the exact shape of correlation function at low values of Qrel REQUIREMENTS High granularity High energy resolution High angular resolution 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration FARCOS (Fentomscopy ARray for Correlation and Spettroscopy) View of array DSSSD 300 µm (1°stage) Basic telescope DSSSD 1500 µm (2° stage) photodiodes 4 CsI(Tl) crystals (3rd stage) 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration Features planned for FARCOS array High energy and angular resolution (θ,φ) Wide dynamic range of identification -MeV to GeV Pulse-shape capabilities -Low identification thresholds Modularity Flexibility -Electronics integrated, reconfigurable -Copuling with 4π array, magnetic spectrometers, neutron detectors, etc.. Portability -Copuling with several facilities around the world 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration EFFFECTS OF ANGULAR RESOLUTION ON CORRELATION FUNCTIONS ONE TELESCOPE SIMULATION: 6Li->d+α d 6Li α NINE TELESCOPES IN 3x3 CONFIGURATION T=7MeV SOURCE β=0.3 (50 MeV) 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration EFFFECTS OF ANGULAR RESOLUTION ON CORRELATION FUNCTIONS Effects of geometrical setup Efficiency Relative energy reconstruction FWHM=18% FWHM=12% Δθ=1.4o d=72mm Both setup cover the same angular region The efficiency increases by a factor about 25 Δθ=0.5o d=250mm The resolution increases by a factor about 3 FWHM=6% FWHM=4% EFFICIENCY and RESOLUTION necessary to obtain a good reconstruction of correlation functions. 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM TEST ON DETECTORS DSSSD (Double- Sided Silicon Strip Detector) TEST Preamplifiers Experimental Setup “Mixed” α source 239Pu, 241Am,244Cm Mesytec MPR-32 NPA prototype Strip detector Vacuum chamber Low power consumption: <900 mW Energy resolution 1500μm (alpha source) ~0.5% for E=5.48 MeV peak 32 channels Hybrid charge preamplifiers in a volume of about 8cm x 10cm x 2cm Rise‐Time (pulser): 3-7 nsec for Cinput=0-100pF Available with several sensitivities (5, 10, 45, 100 mV/MeV…) 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration TEST ON DETECTORS Charge sharing phenomena FRONT Also 0.7% of total events … After calibration Resolution=45 KeV It is impossible to recover these events 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration … TEST ON DETECTORS LIGHT RESPONSE UNIFORMITY TESTS OF CsI(Tl) CRYSTALS SURFACE TEST WITH α SOURCE Experimental Setup α SOURCE 241A 5.48 MeV SCANNING SYSTEM VACUUM CHAMBER SBG055 SBG052 Sij Lij L L 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration … CARATTERIZZAZIONE DEI RIVELATORI … TEST ON DETECTORS LIGHT RESPONSE UNIFORMITY TESTS OF CsI(Tl) CRYSTALS DEPHT TEST: α+208Pb a E=62AMeV Sij Experimental setup All crystals show nonuniformity under 1% After correction Before correction First 4 prototype of FARCOS telescope Resolution=0.8% Resolution=0.5% CHIMERA chamber 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration Lij L L New front-end electronics planned for FARCOS array Hardware Architecture General Electronics for TPCs DETECTOR ARRAY PA Shaper SCA Pulser 132 channelS for each telescope µTCA Crate µTCA Backplane Multiplicities 1 Gb Ethernet per COBO µTCA Backplane Trigger / TS DAQ Network Switch DAQ Workstations 10 Gb Ethernet 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration …….. In progress First peak resolution:180 KeV 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration Performed simulations show that we expect good performances of apparatus and possibility to achieve, with suitable geometrical setup, resolutions and efficiency to have precise meaurements of correlation functions We will continue our study of light response at inner depth of crystals using higher energy beams We are moving towards ASIC electronics in order to control and process the signals produced by each channel of FARCOS telescope 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration Some of the experiments planned in 2014 @ LNS 31 January 2014, Bormio (Italy). L.Quattrocchi for EXOCHIM Collaboration EXOCHIM collaboration PARTICIPANTS L. Acosta1, T. Minniti2,3, L. Quattrocchi2,3 , G. Verde4, G. Cardella4, F. Amorini1, A. Anzalone1, L. Auditore2,3, E. De Filippo4, L. Francalanza1,5, E. Geraci4,5, C. Guazzoni7,8, E. La Guidara4,9, G. Lanzalone1,10, I. Lombardo1,5, C. Maiolino1, E.V. Pagano1,5, A. Pagano4, M. Papa4, S. Pirrone4, G. Politi4,5, F. Porto1,5, F. Rizzo1,5, P. Russotto1,5, A. Trifirò2,3, M. Trimarchi2,3, M. Vigilante13,14. INSTITUTIONS 1INFN-LNS; 2INFN- Gruppo Collegato di Messina; 3Dip. Fis. Univ. Messina; 4INFN- Sez. Catania; 5Dip. Fis. e Astr. Univ. Catania; 7INFN- Sez. Milano; 8Dip. Fis. Univ. Milano; 9CSFNSM, Catania; 10Univ. KORE, Enna, Italy; 11Univ. de Huelva, Spain;13INFN- Sez. Napoli; 14Dip. Fis. Univ. Napoli. THANK YOU FOR YOUR ATTENTION RESERVE 1 R(q) k Koonin-Pratt Equation Ycoin p1, p2 Yevt.mixing p1, p2 1 R q 1 dr S r K r , q Kernel function Source function Probability of emitting two particles with a relative distance r r 1 r 2 recorded at the time when the last particle is emitted K r , q q r Nuclear Coulomb 2 1 82 < Qrel < 86MeV/c 82 < Qrel < 86MeV/c