Modular Survey Spectrometer and Compton Imager - · PDF fileModular Survey Spectrometer and...
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Modular Survey Spectrometer and Compton Imager
Audrey MacLeodIonizing Radiation StandardsMeasurement Science and StandardsNational Research Council Canada
On behalf of the SCoTSS collaboration (Silicon photomultiplier-based Compton Telescope for Safety and Security) . NRC: P. Saull, A. MacLeod. NRCan: L. Sinclair, A. McCann, DRDC: P-L. Drouin, L. Erhardt, R. Ueno, D. Waller
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Outline
● Introduction– What is a Compton imager?
– Potential applications
● History of Compton imaging at the National Research Council Canada (NRC)
● Current project to commercialize a Compton imager + spectrometer
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Display location of radioactive sources (those that emit gamma rays) overlaid on a visual image of the surroundings.
Aid intelligence gathering prior to or following a radiological or nuclear incident.
What is a Compton imager?
Simulation
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April 5, 2016 Carleton Physics Seminar 4
Courtesy of L. Sinclair
Spectrometer large logs of scintillator NaI(Tl)
Co-60
Current state of surveying techniques in Canada: airborne and truck surveying with sensitive spectrometers
Current spectrum
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Why an imager?Source inside building radiating through door
Phase 1: truck-borne surveyidentifies highest intensity location along road x = x2 tree?
Phase 2: camera correctly locates source on line through doorx = x0 or x = x1 building
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shelf-shielding – directional
pin-hole camera imaging
punch-through mask
incomplete absorption(Compton scattering)coded aperture imaging
Azimuthal information only
A much better approach is to use Compton imaging
Competing imaging methods have major limitations
Methods Limitations
Mask
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reconstructed positionfrom five projected cones
Incoming gamma ray Compton scatters off an electron
Reconstruction of scattering angle from measured energies
Compton imaging relies on tracking the gamma ray as it scatters through your detector
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Comptel pioneered Compton imaging Flew on NASA’s Gamma-Ray Observatory
from 1991- 2000
Detected gamma-ray sources (0.75 - 30 MeV)
Al-26 emission at 1.8 MeV → indicates star formation.
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H3D : CZT semiconductor
HandheldsLow Sensitivity:
Volume ~ < 50 cm3
GeGi: segmented HPGe detector
Very High Sensitivity Ultra Large Volume
High Cost
SORDS
MISTI
High Sensitivity:Medium-Large Volume
Affordable
H3D : CZT semiconductor
- Portable: suitable for mounting on various platforms (truck, helicopter, etc).
-Operates in survey mode: high sensitivity: spectrometer + Compton imager
A gap exists in the market for a mid-sized imager/spectrometer
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Inorganic scintillator – good choice for large-volume + low cost + decent resolution
Co
st
Res
ol u
tio
n● Semiconductors (HPGe, CZT, …)
● Inorganic Scintillator (NaI, LaBr3,…)
● Organic Scintillator (PVT)
● Liquid Scintillator
Scintillators converts high energy radiation to visible light!
Detection Medium: Inorganic scintillator
https://Wiki.uio.no/mn/safe/nukwik/index.php
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Scintillator Light Readout: SiPMs
Close-up of 3x3 mm SiPM(array of APDs)
All APD outputs summed ~400 um
There are 76 384 of these APDs on this SPM Array
Silicon Photomuliplier (SiPMs or SPMs):Arrays of avalanche photodiodes (APDs) operating in Geiger mode
APD
Light-weight: Suitable choice for a portable device
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Two Compton imagers were developed (2008 – 2013)Project funded by CRTI (chemical, biological, radiological and nuclear, CBRN,
Research and Technology Initiative)
Pixel ImagerL. Sinclair (Natural Resources Canada)P. Saull (National Research Council Canada)
Bar ImagerD. HannaA. MacLeodP. Boyle(McGill)
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Two designs pursued
PMT PMT
SiPMSiPM
Bar design
Pixel design
(McGill)
(NRC/NRCan)
PMT: photomultiplier tube
SPM: silicon photomultiplier
Early tests showed pixel design would be more robust in the field.
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Pixel imager
Absorber: 10 x 10 array of NaI(Tl)/PMT
Scatter: Two 9x9 arrays of 1.35 cm3 CsI(Tl)/SiPM
Optical camera
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A typical event yields a single Compton cone
Scatter energy deposit
Absorber energy deposit
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Source Localization
Source
Minimization (real data) [ ~ 10 s ]
Back-projection (real data) [2 hrs – 0.6 mCi Cs-137 at 8 m]
1) Back-projection Image
Back-projecting Compton cones onto a plane and converting into angular units
2) Iterative χ2 Minimization
Find the vector v(θ,ϕ) that minimizes the angular distance to all the Compton cones (weighted by their uncertainties)
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Demonstration of imager
performance
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April 5, 2016 Carleton Physics Seminar 184 seconds of data taking
0.6 mCi Cs-137 at 10 m, 20o off axis(equivalent to background level in lab)
1-, 2-, and 3-sigma probability contours for source location
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April 5, 2016 Carleton Physics Seminar 19
60 seconds of data taking
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June 4th, 2015 CSS RN Science Day, NRC-MSS 20
Cs-137
It is a highly sensitive spectrometer.
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Alarms when a source is present
Courtesy of N. Stanley
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Imaging Multiple Isotopes
0.6 mCi Na-22, 0.6 mCi Cs-137 placed at 7m
Reconstructed in 30 s
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Spectral photo-querying
● Move cursor over room photo ● Plot energy of all Compton cones which have an angle of
closest approach to cursor direction to within ~ 3 degrees● Can improve signal-to-background
– Useful for detecting shielded sources (ie. shielded special nuclear material (SNM)).
– Example: 1 to 2 minutes with 0.6 mCi Cs-137 and Na-22 sources present at ~ 9 m
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Background example 1
Energy (MeV)
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Cs-137 (0.662 MeV)
Energy (MeV)
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Na-22(0.511 MeV,1.274 MeV)
Energy (MeV)
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All reconstructed to within 0.5 m in less than 2 minutes (0.6 mCi Cs-137 source)
Triangulation
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Project Overview● Deliverable (late-2017): commercial sensitive spectrometer suitable
for radiation surveying, with precision imaging capability
● Industry partner (RSI) has wealth of experience fielding rugged radiation detectors for use in the field
● Modular Design: imagers of different size and therefore price point
Example module Example 3x3 array
Build uparrays of various sizes
32 channels 288 channels
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Scatter pixelsScatter pixel:
- SiPM: 2 x 2 array of ArrayC-60035-4Ps - Scintillator: 1.35 cm3 CsI(Tl) crystal
6.5% FWHM at 662 keV
32 keV X-rays
Typical performance: - Energy Resolution ~ 6.5 % at 662 keV- Noise (energy-equivalent) ~ 1.6 keV
Sample trace
Scatter pixel
Custom SiPM array board
Low Noise → record lower energy deposits → image low energy sources
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Absorber crystal: - form a 2 x 2 array of ArrayC-60035-4Ps - mate to 2.8 cm3 CsI(Tl) crystal
Typical performance: - Energy Resolution ~ 6.5 % at 662 keV- Noise ~ 4.6 keV
Lot of sensors (Cancino)
Sipm Absorber pixel
Absorber pixels
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1° precision achieved in minutes
EGSnrc + GEANT4 Simulations: 1 mCi Cs-137 at 10 m
Smallest Module
SCAT ABS
1° precision achieved in secondsLarge imager: 3x3 array
SCAT ABS
The imager will be highly sensitive
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April 5, 2016 Carleton Physics Seminar 33
32-channel interim fieldable imager
Absorber: 4 x 4 array of 2.8 cm3 CsI(Tl)/SiPM Scatter: 4 x 6 array of 1.35 cm3 CsI(Tl)/SiPM
- Allows us to gain invaluable field experience for feedback into mission-ready imager design - Currently being assembled
RSI digitizer board
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Summary
● Compton imaging has a wide range of applications
● Project to commercialize a Compton imager for first responders is underway– A highly sensitive spectrometer with imaging
capabilities
– Portable: suitable for different surveying platforms (truck, helicopter etc.)
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Extra Slides
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A Cs-137 line source in the shape of a 'C'
Simulation: Extended source imaging
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Compton scattering is the dominant interaction process from several hundred keV – several MeV
Energy Regime of Interest
Germanium
Co-57 Co-60
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April 5, 2016 Carleton Physics Seminar 38
Self-shielding imagingUse shadow of scatter plane on absorber plane to localize point source
Simulate source and fieldable imager (4 x 4 arrays in scatter and absorber) with Geant4
Step 0.6 mCi Cs-137 at 10 m from detector every 2o from -10o to +10o
Will work best for low-energy sources
scatter
absorber
~ 1-degree angular resolution in 1 minute
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Visible:Mirrors/lenses
X ray:Glancing incidence mirrorsdiffraction
The electromagnetic spectrum
Gamma ray:Coded apertureCompton imagingPinhole