the advanced scintillator compton telescope (ascot
TRANSCRIPT
Future Gamma-Ray Observatories - GSFC - March 24, 2016
The Advanced Scintillator Compton Telescope (ASCOT) Balloon Project
P. F. Bloser, M. L. McConnell, J. M. Ryan J. S. Legere, C. M. Bancroft, T. Sharma, A. Wright, T. Gorte
Space Science CenterUniversity of New Hampshire
Philosophy
• The ASCOT project is motivated by the theory that the most cost-effective, low-risk way to implement an advanced, general-purpose Compton telescope is to build directly on the experience of COMPTEL
• A advanced, scintillator-based Compton telescope would use modern detector materials to improve efficiency, energy resolution, and time-of-flight (ToF) resolution for background rejection
• It would also use advanced light readout devices, such as silicon photomultipliers (SiPMs), to reduce passive mass, volume, and power
Future Gamma-Ray Observatories - GSFC - March 24, 2016
COMPTEL Background
Future Gamma-Ray Observatories - GSFC - March 24, 2016
B
CGRO Platform
COMPTEL EGRET/OSSE
B
DC
AA
C
Kappadath, S. C., 1998, Ph.D. Thesis, University of New Hampshire
B A
C D
C near D1
“Good” ToF Window
ToF was critical to COMPTEL’s sensitivity:
COMPTEL suffered intense background from particle interactions:
Improved ToF resolution will greatly reduce background in straightforward
manner
NaI D2
Organic Liquid D1
Balloon Flight DemonstrationsUNH has conducted two successful balloon flight tests of available technology that would enable an advanced scintillator Compton telescope:
– The FAst Compton TELescope (FACTEL) experiment (September 2011): new scintillators (collaboration with LANL)
– The Solar Compton Telescope (SolCompT) experiment (August 2014): SiPM readouts
Future Gamma-Ray Observatories - GSFC - March 24, 2016
FACTEL Experiment• Compton telescope consisting of three 1-inch liquid organic D1
scintillators and three 1-inch LaBr3 D2 scintillators, all read out by fast PMTs
• D1-D2 separation of ~30 cm• D1 surrounded by plastic ACS• Pressure vessel, PC-104 flight computer
Future Gamma-Ray Observatories - GSFC - March 24, 2016
Liquid LaBr3 PMT
FACTEL Flight Results (2011)
Future Gamma-Ray Observatories - GSFC - March 24, 2016
• ToF spectrum fully described by two Gaussians
• “Down” and “Up” gammas cleanly separated
• FWHM ~ 1.2 ns
• Downward moving gamma spectrum agrees with Geant4 simulations
Julien, M., et al., 2012 IEEE NSS Conference Record, 1893
The Silicon Photomultiplier (SiPM)• Scintillator detectors limited by size, mass, and power of readout• A SiPM (aka SSPM, MPPC) is a summed array of tiny (~50 µm)
silicon APDs reverse-biased slightly above breakdown voltage in limited Geiger mode; recovers in 10s of ns
• SiPMs are compact, light, robust, low power, LV (30 - 70 V), and have gain (105 - 106), timing (~1 ns rise time), and effective quantum efficiency (20% - 30%) equivalent to PMTs
• Replacing PMTs with SiPMs in a Compton telescope would eliminate passive material, reduce mass, and allow closer packing
Future Gamma-Ray Observatories - GSFC - March 24, 2016 (Stapels et al. 2005)
Future Gamma-Ray Observatories - GSFC - March 24, 2016
SolCompT Experiment• 2-element Compton telescope: D1 is 1-inch
stilbene, D2 is 26 mm × 26 mm × 26 mm LaBr3
• Both read out using 2 × 2 array of Hamamatsu S11828-3344 MPPCs with transformer FEE for low input impedance
• Payload used hardware (pressure vessel, heaters, readout electronics, and PC-104 computer) flown in 2011 as part of the FACTEL payload
• Tagged 60Co source (~240 nCi) to monitor gain and energy resolution
D1
D2
15 cm
Frame
SolCompT Flight Results (2014)Although only had 3.75 hours at float, tagged events 60Co show good ToF and energy spectra:
Future Gamma-Ray Observatories - GSFC - March 24, 2016
-4 -2 0 2 4ToF (ns)
0
20
40
60
80
100
120
Cou
nts
0 500 1000 1500 2000Energy (keV)
0
2
4
6
8
10
Cou
nts
FWHM ~ 760 ps
-4 -2 0 2 4ToF (ns)
0
20
40
60
Cou
nts
Untagged events harder to interpret due to small spacing and surrounding material –but still see up vs. down on top of broad continuum:
Bloser, P. F., et al., 2016, NIM-A, 812, 92
The ASCOT Balloon Project• We are conducting a program to fly a larger scintillator-based
Compton telescope with SiPM readouts on a balloon and observe the Crab in a 1-day flight
• D1 will be p-terphenyl organic scintillator; D2 will be CeBr3 (due to difficulties with Saint-Gobain, also lower internal background)
• Will use the SensL MicroFC-60035-SMT 6 mm × 6 mm SiPM –has “fast” output, good for ToF
Future Gamma-Ray Observatories - GSFC - March 24, 2016
1.8 m
CSBF Rotator
Elevation Drive
Batteries
Power Relay Board
Mini-SIP
GPS Antenna
1.4 m
ASCOT Balloon Instrument• Instrument concept: basic “module” with 8 × 8 scintillator array
optically coupled to a 8 × 8 SiPM array• Each scintillator 15 × 15 × 25 mm3
• Each scintillator read out by 2 × 2 SiPM array (same as lab tests)• Detector layers each 2 × 2 array of modules• Two D1 layers, one D2 layer (cost)• Estimate ~4σ Crab detection
Future Gamma-Ray Observatories - GSFC - March 24, 2016
Cover
Scintillator
SiPM (2x2)SiPM Array Board
15 cm
VETO Panel
D1 Layers
(p-terphenyl)
15 cm
D2 Layer
(CeBr3)
FRP Frame
Instrument
Electronics
Flight
Computer
35 cm
ASCOT D1: P-terphenyl• 142 p-terphenyl crystals have been delivered • Show good uniformity, light output• Will be assembled into 8 × 8 array with Delrin housing
Future Gamma-Ray Observatories - GSFC - March 24, 2016
0 200 400 600 800 1000 1200Energy (keV)
0
500
1000
1500
Cou
nts
DataSimulation
0 1000 2000 3000 4000Pulse Height
1100
1200
1300
1400
1500
1600
PSD
252Cf
Neutrons
Gammas
Test data with test SiPM array
Project SMART Balloon Flight• A prototype D1 detector was flown as a weather balloon payload
by high school students participating in UNH’s Project SMART• Reached altitude of ~31 km, counting rate shows expected
behavior (Pfotzer Maximum)• “Poor man’s thermal/vac test”
Future Gamma-Ray Observatories - GSFC - March 24, 2016
0 5.0×103 1.0×104 1.5×104 2.0×104 2.5×104 3.0×104
Altitude (m)
0
5
10
15
20
Scin
tilla
tor R
ate
(cts
s-1)
ASCOT D2: CeBr3 Array• 8 × 8 vacuum-rated array made by Scionix• Initial testing shows slightly reduced energy resolution
compared to 13 × 13 × 13 mm3 LaBr3 crystal• Due to light loss via entrance window (i.e., cross talk):
Future Gamma-Ray Observatories - GSFC - March 24, 2016
0 500 1000 1500 2000 2500Energy (keV)
0
5
10
15
20
25
Ener
gy R
esol
utio
n (%
FWH
M)
CeBr3LaBr3
0 200 400 600 800Energy (keV)
0
50
100
150
Cou
nts/
keV
∆E/E = 6.2% @ 662 keV
Time of Flight
• Measured ToF resolution between one p-terphenyl and one CeBr3 pixel using custom CFD/TAC board
• We see very little PH-dependent walk in timing• For coincident 60Co events with large PH, get:
Future Gamma-Ray Observatories - GSFC - March 24, 2016
527 ± 34 ps (FWHM)
ASCOT Instrument• Mechanical design is underway• Electronics design as well• SiPMs will be mounted on 8-pixel “strip” boards,
plugged into motherboard
Future Gamma-Ray Observatories - GSFC - March 24, 2016
Initial Simulations• Preliminary simulations done with MGGPOD indicate
~4σ Crab detection• Have begun using MEGAlib for more detailed work
Future Gamma-Ray Observatories - GSFC - March 24, 2016
1 10Energy (MeV)
1.4
1.6
1.8
2.0
2.2
2.4
2.6
2.8
Effe
ctive
Are
a (c
m2 )
5
6
7
8
9
10
ARM
(deg
FW
HM)
Effective Area
Angular Resolution
ASCOT Balloon Response
1Energy (MeV)
1
10
100
1000
Cou
nts
MeV
-1
Simulation of Potential Explorer Mission
• Explorer-sized instrument concept: 7 × 7 array of modules forms a “layer”
• Three D1 layers and three D2 layers, 50 cm separation
• Assume FRP frame (as in FACTEL), plastic ACS
• Estimate 120 × 120 × 100 cm3 instrument, ~1000 kg payload
• Simulate response and background with MGGPOD – assume radiation inputs from Advanced Compton Telescope Concept Study for 5º inclination, 550 km LEO
• Use measured detector response
Future Gamma-Ray Observatories - GSFC - March 24, 2016
MGGPOD Payload Model
Hmm – why not on sides??
Simulated Compton Telescope Performance
Simulations indicate that an Explorer-sized Compton telescope using this technology would greatly improve on the performance of COMPTEL:
Future Gamma-Ray Observatories - GSFC - March 24, 2016
1 10Energy (MeV)
0
10
20
30
40
50
60
70
Effe
ctive
Are
a (c
m2 )
COMPTEL 0o
ASCOT 0o
ASCOT 30o
ASCOT 60o
1 10Energy (MeV)
10-6
10-5
10-4
10-3
phot
ons
cm-2 s
-1 M
eV-1
COMPTELASCOT
Cyg X-1 Hard State
Cyg X-1 Soft State
3m Sensitivity4 x 105 s
1Energy (MeV)
10-6
10-5
10-4
10-3
10-2
10-1
phot
ons
cm-2 s
-1 M
eV-1
3m Sensitivity
Tobs
= 106 sT
obs = 107 s
Much greater effective area than COMPTEL, especially below 1 MeV
~8 times better on-axis continuum sensitivity around 1 MeV for 2-week observation (compare to COMPTEL Cyg X-1 spectrum)
Instrument could study MeV spectra of multiple Galactic black holes (spectra from OSSE)