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P.G. PelferUniversity of Florence and INFN, Firenze, Italy
F. DubeckyInstitute of Electrical Engineering, Slovak Academy of Sciences
Bratislava, Slovakia
A.OwensESA/ESTEC
Noordwijk,Netherland
P.G. PelferUniversity of Florence and INFN, Firenze, Italy
F. DubeckyInstitute of Electrical Engineering, Slovak Academy of Sciences
Bratislava, Slovakia
A.OwensESA/ESTEC
Noordwijk,Netherland
Solar Neutrino Spectrometer with InP Detectors
Solar Neutrino Spectrometer with InP Detectors
P.G.Pelfer SIENA2002
P.G.Pelfer , SIENA2002
Why InP Solar Neutrino Experiment ?Why InP Solar Neutrino Experiment ?
Semi Insulting InP Material
base material for:
Hard X-Ray Detectors
Fast Electronics and Optoelectronics
InP Spectrometer,
the Smallest, Real Time, Lower Energy
pp Solar Neutrino Spectrometer
The Solar Neutrino Spectrometer from/for R&D on InP X-Ray Detectors ?
Requirements for Hard X-Ray Detectors of the New GenerationRequirements for Hard X-Ray
Detectors of the New Generation
• Room temperature (RT) operation• Portability• Fast reaction rate• Universal detection ability• Good detection parameters: CCE, FWHM, DE• Radiation hardness• Well established material technology • Well established device technology (10 m)• FE Electronics and Optoelectronics
integration on the Detector
• LOW COST
RT OPERATION: EG > 1.2 eV POLARISATION EFFECT: EG < 2.5 eV HIGH ENERGY RESOLUTION: EG small HIGH STOPPING POWER: Z > 30 HIGH CARRIER MOBILITY: > 2000 cm2/Vs
CANDIDATES
CdTe, HgI2, GaAs, InP
P.G.Pelfer , SIENA2002
P.G.Pelfer SIENA2002
• BASIC KNOWLEDGE
• Solar Neutrino Physics• X-ray astronomy
• X-ray physics
• MEDICINE• Digital X-ray radiology (stomatology, mammography, ...)
• Positron emission tomography• Dosimetry
• NONDESTRUCTIVE ON-LINE PROCESS CONTROL• Material defectoscopy
• MONITORING• Environmental control
• Radioactive waste management• Metrology (testing of radioactive sources, spectrometry...)
• NATIONAL SECURITY• Contraband inspections: cargo control
• Detection of drugs and plastic explosives • Cultural heritage study
DETECTOR APPLICATIONSDETECTOR APPLICATIONS
P.G.Pelfer SIENA2002
SemiInsulating InP Wafer6” 6” diameter, diameter, 1 mm1 mm thick
Pad Detectors
Basic Component ofNeutrino Spectrometer
Present InP Material and Detector TechnologyPresent InP Material and Detector Technology
Neutrino from the SunNeutrino from the Sun
ChlorineHomestakee + 37Cl 37Ar + e-
GalliumSAGE, Gallex, GNOe + 71Ga 71Ge + e-
WaterKamioka, SuperKx + e- x + e- (ES)
D2OSNOx + e- x + e- (ES)e + d p + p + e- (CC)x + d n + p + e- (NC)
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
Requirements for Indium Solar Neutrino SpectrometerRequirements for Indium Solar Neutrino Spectrometer
1. Indium incorporated into the detector
2. Energy resolution ∆E/E of the order of 25% at 600 keV. Important for spectrometry as well as background reduction.
3. Time resolution of the order of 100 ns for ~ 100 keV radiations.
4. Position resolution ∆V/V 10-7 at a reasonable cost. Very important for background reduction
5. Good energy resolution for low energy radiations ( ~ 50 keV )
6. Made with materials of high radiactive purity
497.33 keV
E e(E - 118 keV ) + 115 Sn*
Delay = 4.76 sec
115Sn* 115Sn + e-(88 112 keV)/1 (115.6 keV) + 2(497.33 keV)
1/2= 4.76 sec
-
e
115In (95.7%)
1/2=6x1014 y
115Sn
612.81 keV9/2+
7/2+
1/2+
3/2+1
2
0
Neutrino Detection by In TargetNeutrino Detection by In Target
P.G.Pelfer , SIENA2002
P.G.Pelfer SIMC XIIJuly 2002, Smolenice Castle
The Neutrino TagThe Neutrino Tag
a - e delay = 10 sec ( e/1 + 2 ) coincidence
b - ( e/1 + 2 ) in prompt coincidence ( gate 100 ns )
c - ( e + e ) in spatial coincidence in a microcell ( few mm3 )
d - 1 contained in a “ 1 cm3 cell “ surrounding primary microcell
e - 2 shower trigger in at least two “ 1 cm3 cell “
f - 2 contained in a macrocell ( more than 27 “ 1 cm3 cell “ ) surrounding primary microcell
g - E( e/1 ) = 50-200 keV
h - E( 2 ) = 450-750 keV
i- E(1 + 2 ) = 500-750 keV
P.G.Pelfer , SIENA2002
" prompt event “ in a “1 cm3 cell”
“ delayed event “ in a 27 cm3 macrocell
12
3 4 5
6
789
12
3 4 5
6
789
e
1
2
10 s
time
Solar Neutrino Eventin InP Detector
Solar Neutrino Eventin InP Detector
Calorimeter Module
1 cm3 cell
106 InP “1 cm3 cell”
1 neutrino event once a day for 1011 background events
100 mm 200 mm
Spectrometer Module
Spectrometer Building Block
Pad Detectors
V microcell 1 mm3
N microcell /cm3 1000
FULL NEUTRINO SPECTROMETERFULL NEUTRINO SPECTROMETER
Nmodules 125
P.G.Pelfer , SIENA2002
pp
Be(384)
spectrum of In (*10 )115 -11
Be (862)
pep (1442)
d
*
[S
NU
per
20
keV
]
E [keV]e
Expected Electron Energy Spectrumfrom In Solar Neutrino Experiment
Expected Electron Energy Spectrumfrom In Solar Neutrino Experiment
P.G.Pelfer , SIENA2002
SI InP Material and Detector TechnologySI InP Material and Detector Technology
P.G.Pelfer , SIENA2002
Original BUFFERS realised using ion implantation in backside (PATENTED)
Symmetrical circular contact configuration, 2mm , using both-sided photolithography
Final metallisation: TiPtAu on top and AuGeNi on backside
Surface passivation by Silicon Nitride
Producer:
JAPAN ENERGY Co., Japan
Growth Technique:
LECHigh-Temperature Wafer Annealing
Resistivity (300 K): 4.9x107 cm
Hall Mobility (300K): 4410 cm2/Vs
Fe Content: 2x1015 cm-3
Orientation: <100>
Final Wafer Thickness: ~ 200 m
InP Detector Test SetupInP Detector Test Setup
3.142 mm2 x 200 m
P.G.Pelfer , SIENA2002
E=2.4 keV at 5.9 keV : 8.5 keV at 59.54 keV
P.G.Pelfer , SIENA2002
Energy Resolution vs Shaping Time andSpectral Response in InP Laboratory Measurements
Energy Resolution vs Shaping Time andSpectral Response in InP Laboratory Measurements
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a
EaeEFE
Linearity and Resolution vs X Ray Energyin InP Laboratory Measurements
Linearity and Resolution vs X Ray Energyin InP Laboratory Measurements
P.G.Pelfer , SIENA2002
Synchrotron Radiation MeasurementsSynchrotron Radiation Measurements
Beamline set-up
XY stage
detectorslits
Beam pipe
To mono/focusing optics
Beam profile ~20 20 m2, E/E > 104
Optical bench
HASYLAB X-1, BESSY-II WLS beamlines. Energy range 10 keV to 100 keV
P.G.Pelfer , SIENA2002
Pulse Height Spectra in InP HASYLAB MeasurementsPulse Height Spectra in InP HASYLAB Measurements
P.G.Pelfer , SIENA2002
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EaeEFE
InP Derectors Linearity and Energy Resolution in the Measurements at HASYLAB
InP Derectors Linearity and Energy Resolution in the Measurements at HASYLAB
P.G.Pelfer , SIENA2002
InP Spatial DistributionsInP Spatial Distributions
Count rate
Peak centroid
Resolvingpower
contact
bond wire
The detectors spatial response measured at HASYLAB using a 50 50 m2, 15 keV X-ray
beam.
P.G.Pelfer , SIENA2002
InP Detector BESSY-II Measurements: Detection Efficiency vs Energy and Thickness
InP Detector BESSY-II Measurements: Detection Efficiency vs Energy and Thickness
Depletion depth derived from C/V measurements = 170 mEfficiency measured relative to a calibrated Ge(HP) detectorFitted depth from efficiency measurements = (191 40) m
))(exp(1))(exp()(1
dEtEE InPii
n
d= Aor/C
WLS beamline
P.G.Pelfer , SIENA2002
InP Spectra Laboratory Cryogenic Measurements InP Spectra Laboratory Cryogenic Measurements
T=-60oC T=-170oC
E=2.4 keV at 5.9 keV : 8.5 keV at 59.54 keV E=0.9 keV at 5.9 keV : 2.5 keV at 59.54 keV
ST=10sST=2s
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
Present Radiation Detectors based on Bulk SI InP Fe doped have very good Detection Parameters
for the X ray Detection
from HASYLAB SR FaciltyFWHM from 2.5 KeV at 5.9 KeV to 5.5 KeV at 100 KeV
DE 10% at 100 KeV for 200 m thick Detector
dueto Better Material from Japan Energyand to Improved Interface Technology
Some Problems for Detector Polarisation
Detectors performance good for Solar Neutrino Spectrometer
Optimisation is our next research goal
Summary and DiscussionSummary and Discussion
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
InP and In-Liquid Scintillator
pp Solar Neutrino Detector
InP DETECTROR In-Liquid Scintillator DETECTOR
Radiation Damage Studies by 10 MeV Proton Beam Radiation Damage Studies by 10 MeV Proton Beam
Tests carried out at the accelerator facility of the Department of Chemistry, University of Helsinki, The incident beam energy was 10 MeV. Irradiations were carried out at room temperature and unbiased.
Bottom line: Si energy resolution degraded by a factor of 6 for a proton fluence of 8 x 1010 protons cm-2 (=60 krad), whereas InP degraded by only 20% for fluence of 1.6 x 1011 protons cm-2 (however the initial resolution was much worse).
Detectors tested [email protected] Area thickness [email protected] Area thickness
Si 245 eV 0.9 mm2, 500m CdZnTe 450 eV 3.1 mm2, 2500m GaAs 470 eV 0.9 mm2, 40m HgI2 600 eV 7.0 mm2, 500m InP 2.5 keV 3.1 mm2, 180m TlBr 900 eV 3.1 mm2, 800m
P.G.Pelfer , SIENA2002
Radiation Damage Studies. Energy Resolution vs Proton Fluence Radiation Damage Studies. Energy Resolution vs Proton Fluence
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
ACKNOWLEDGEMENTSACKNOWLEDGEMENTS
Authors are grateful to:
Slovak Academy of Sciences
Slovak Grant Agency and
Slovak Ministry of Economy,
European Spatial Agency,
Istituto Nazionale di Fisica Nucleare,
University of Florence
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
Good energy resolution in the interval
50÷150 keV
Large detector volume or thickness (mm)
High ratio between peak to valleyNo high applied bias voltage
Low dark currentShort charge collection time
High fabrication yield ofgood quality detectors
Radiation Hardness
Stability of detector in environmental conditions and ageing
Relevant requirements depend from specific detector applications
Detector RequirementsDetector Requirements Materials RequirementsMaterials Requirements
Bulk Material
1- , ee, hh :high mobility, long carrier lifetime and high product mobiliiy lifetime
2-material homogeneity in term of purity, stoichiometry, absence of structural defects.
Highly uniform material critical for fabrication of thick X-Rays detectors.
3-high resistivity generally required (107 cm) , high breakdown voltage, low dark
current
Epitaxial Materials not examined
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
Pad and Double Side Strip Detector ArrayPad and Double Side Strip Detector Array
PAMELA EMCal Si Microstrips Layers
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
NeutronSpectrography
NeutronSpectrography
•Possible room temperature operation
•High stopping power
•Electron mobilities 3 times that of Si
•Possible neutrino detection medium
•Epitaxial and bulk growth available
•Standard semiconductor processing
Indium phosphide X-ray detectors
Beam pipe
To mono/focusing optics
Optical bench
Beamline set-up
slits
Beam profile ~20 20 m2, E/E > 104
Synchrotron radiation measurementsHASYLAB X-1 and BESSY-II WLS beamlines. Energy range 10 keV to 100 keV
detector
XY stage
Radiation damage studies: experimental
Tests carried out at the accelerator facility of the Department of Chemistry, University of Helsinki using an IBA Cyclone 10/5, proton cyclotron, The incident beam energy was 10 MeV. Irradiations were carried out at room temperature and unbiased. Devices were tested using 55Fe, 109Cd and 241Am radioactive sources, with initial and final characterizations at HASYLAB
Bottom line: Si energy resolution degraded by a factor of 6 for a proton fluence of 8 x 1010 protons cm-2 (=60 krad), whereas InP degraded by only 20% for fluence of 1.6 x 1011 protons cm-2 (120 krads Si equivalent), however the initial resolution was much worse.
Detectors tested [email protected] Area thickness [email protected] Area thickness
Si 245 eV 0.9 mm2, 500m CdZnTe 450 eV 3.1 mm2, 2500m GaAs 470 eV 0.9 mm2, 40m HgI2 600 eV 7.0 mm2, 500m InP 2.5 keV 3.1 mm2, 180m TlBr 900 eV 3.1 mm2, 800m
Science Payloads and Advanced Concepts
Radiation damage studies: dose history
Science Payloads and Advanced Concepts
P.G.Pelfer , SIENA2002
Linear ScannerLinear Scanner
X Rays
Linear array of 32 InP pixels
Linear array of 32 InP pixel and FE electronics cooled with a Peltier cooler
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
Termonuclear Neutrino Sources from the SunTermonuclear Neutrino Sources from the Sun
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
P.G.Pelfer SIMC XIIJuly 2002, Smolenice Castle
Detector PrototypeDetector Prototype
Unitarz Cell
Basic Arraz Lazer
Prototype Technology
6“ Wafer VGF Technology (U.Sahr, Erlangen)
PADS / STRIPS
1 cm thick / << 1 cm thick
ELECTRONICS: problem only for a number of the channels
P.G.Pelfer , SIENA2002
PAMELA Electromagnetic CalorimeterPAMELA Electromagnetic Calorimeter
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
Figura del wafer 6 inches con il pattern
Dei pixel
Tecnologia 6inch
Semiisolante Fe doped
P.G.Pelfer , SIENA2002
SMALLEST; REAL TIME,
LOWER ENERGY pp SOLAR NEUTRINO
DETECTOR
Module dimension
Module number ( 1 neutrino per day )
Easy shielding from environmental radiation
Many possible topological configuration
Challenging readout solutions
10 “ WAFERS InP ?
P.G.Pelfer , SIENA2002
MODULO ELEMENTAREUNITARIO
PER IL RIVELATORE DI InP
P.G.Pelfer , SIENA2002
MODULO ELEMENTAREUNITARIO
PER IL RIVELATORE DI InP
- Large Groups from many different Countries High Concentration of the needed Expertise
High Experiment Budget ( >100 Meuro, cost of a standard SN exp.)
Interest of the Companies for the Experiment itself No limited time for developing and testing Devices and
Detectors.
P.G.Pelfer , SIENA2002
Calorimeter Module
1 cm3 cell
106 InP “1 cm3 cell”
1 neutrino event once a day for 1011 background events
Solar Neutrino EventSolar Neutrino Event
Solar Neutrino DetectorSolar Neutrino Detector
P.G.Pelfer , SIENA2002
1 macrocell = 27 “1 cm3 cell”
Nmodules 125
•Possible room temperature operation
•High stopping power
•Electron mobilities 3 times that of Si
•Possible neutrino detection medium
•Epitaxial and bulk growth available
•Standard semiconductor processing
Indium Phosphide X-ray DetectorsIndium Phosphide X-ray Detectors
P.G.Pelfer SIENA2002
InP detector construction
3.142 mm2 x 180m thick Fe doped device
Science Payloads and Advanced Concepts
EBIC technique - SI InP: Carrier extraction??EBIC technique - SI InP: Carrier extraction??
Bias voltage: 0, - 60 V, + 60 V
SI InP:
MASPECP+ electrode
JEImplanted bufferEXTRACTION??
Energy Resolution vs Shaping Time andSpectral Response in InP Laboratory Measurements
Energy Resolution vs Shaping Time andSpectral Response in InP Laboratory Measurements
E=2.4 keV at 5.9 keV : 8.5 keV at 59.54 keV
P.G.Pelfer , SIENA2002
P.G.Pelfer , SIENA2002
2
12355.2/355.2
a
EaeEFE
Linearity and Resolution vs X Ray Energyin InP Laboratory Measurements
Linearity and Resolution vs X Ray Energyin InP Laboratory Measurements
P.G.Pelfer , SIENA2002
Beam pipe
To mono/focusing optics
Optical bench
Beamline set-up
slits
Beam profile ~20 20 m2, E/E > 104
Synchrotron radiation measurementsHASYLAB X-1 and BESSY-II WLS beamlines. Energy range 10 keV to 100 keV
detector
XY stage
Energy Spectra in InP HASYLAB MeasurementsEnergy Spectra in InP HASYLAB Measurements
P.G.Pelfer , SIENA2002
InP Derectors Linearity and Energy Resolution in the Measurements at HASYLAB
InP Derectors Linearity and Energy Resolution in the Measurements at HASYLAB
2
12355.2/355.2
a
EaeEFE
P.G.Pelfer , SIENA2002
contact
Count rate
Peak centroid
Resolvingpower
bond wire
The detectors spatial response measured at HASYLAB using a 50 50 m2, 15 keV X-ray beam.
P.G.Pelfer , SIENA2002
Detection Efficiency vs X-Ray Energy and Detector ThicknessDetection Efficiency vs X-Ray Energy and Detector Thickness
InP new laboratory cryogenic measurements
T=-60oC T=-170oC
E=2.4 keV at 5.9 keV : 8.5 keV at 59.54 keV E=0.9 keV at 5.9 keV : 2.5 keV at 59.54 keV
ST=10sST=2s
Science Payloads and Advanced Concepts