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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