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James Webb Space Telescope :James Webb Space Telescope : Characterization of Flight Candidate Characterization of Flight Candidate
of Raytheon NIR InSb Arraysof Raytheon NIR InSb Arrays
5 Aug 2003
Craig McMurtry, William Forrest,
Andrew Moore, Judith Pipher
2
OverviewOverview
• Introduction
• Calibration of InSb SB-304 SCAs
• Dark current
• Noise
• QE
• Latent or Persistent Image Performance
• Operability
• Radiometric Stability
3
IntroductionIntroduction
• Raytheon Detectors Proposed for JWST NIRCam and NIRSpec
– InSb photo-diode detector technology• 0.5 – 5.3 m photo-response
– Based on SB-304 Read Out Integrated Circuit (ROIC) or multiplexer• 2048 x 2048 active pixels• 2 columns of 2048 reference pixels multiplexed to four outputs• Total readout format is 2056 x 2048
– University of Rochester provided detector array testing facilities for JWST level requirements
4
CalibrationCalibration
• Source Follower Gain– Gain through two SF FETs– SCA 006 SFGain=0.777– SCA 008 SFGain=0.785
• Capacitance– Noise2 vs Signal method– SCA 006
• 66 fF
• 3.22 e-/ADU
– SCA 008• 68 fF
• 3.32 e-/ADU
5
CalibrationCalibration
• Linearity– Plotted Signal Rate vs
Signal (C0/C)
– Small flux over long integration times
• Well Depth (Capacity)– @ 300 mV applied
detector bias– SCA 006 well depth =
1.4 x 105 e-– SCA 008 well depth =
1.3 x 105 e-– Larger well depths
possible with little or no increase in dark current
6
Dark Current Test MethodsDark Current Test Methods
• Dark dewars are difficult to make and keep dark
– Using an opaque mask placed in contact with InSb surface, UR dewar light leak < 0.006 e-/s
• 3 Methods of measurement– Usually yield same
values, although some discrepancies possible
• Dark Charge versus integration time
– With reference pixel correction, accurate for moderate dark currents
– Lengthy measurement
7
Dark Current Test MethodsDark Current Test Methods
• Noise2 versus integration time
– With reference pixel correction, accurate for small dark currents
– Also, lengthy measurement
8
Dark Current Test MethodsDark Current Test Methods
• SUTR Dark Charge vs. time
– With reference pixel correction, accurate for small dark currents
– Relatively short measurement (single 2200 sec integration)
– Addition of possible charge per read (e-/read) due to higher read rate
• Confuses measured dark current
• No detectable added noise from charge per read due to higher read rate!
9
Dark Current ResultsDark Current Results
• SCA 006
– Idark = 0.012 e-/s @ T=30.0K
– Idark = 0.024 e-/s @ T=32.3K
– Charge per read of 0.09 e-/read
• Again, no detectable noise due to this charge
– No measurable amp glow or digital circuit glow
10
Dark Current ResultsDark Current Results
• SCA 008
– Idark = 0.025 e-/s @ T=30.0K
– Charge per read of 0.07 e-/read
– No digital circuit glow
– Slight glow (0.05 e-/s including dark current) from output amplifier
• Covers small region (see operability section)
• Known multiplexer defects (shorts)
– Amp glow not seen on other multiplexers
11
System NoiseSystem Noise
• System Noise
– Shorting resistor placed between signal (video) and signal reference lines (analog ground)
– T=295K
– Connected and functioning detector in dewar to allow typical voltage/current paths which may cause cross talk (worst case)
12
Read NoiseRead Noise
• Read noise versus Fowler Sampling
– Measured at T=30.0K
– All integration times are 100 s
• SCA 006 read noise results
– Follows 1/sqrt(N) where N is the number of Fowler sample pairs
14
Noise Measurement MethodsNoise Measurement Methods
• Methods of measurement for total noise in 1000 seconds.
– Box average (often called “spatial” noise method) uses the {standard deviation of mean}/sqrt(2) of difference of two 1000 sec Fowler-8 images
– Full frame average (“spatial”) noise computed using difference of two 1000 sec Fowler-8 images, and plotting histogram of pixel values
• The width of the distribution corresponds to the average noise; mean is DC offset
• Gaussian fit reject Cosmic Ray• SCA 006 at right
15
Noise Measurement MethodsNoise Measurement Methods
• Methods of measurement (cont)
– Temporal noise measurement is computed by taking the standard deviation of the mean per pixel for a large number of 1000 sec Fowler-8 images (time series)
• Distribution is typically a Gaussian whose width depends on the number of images taken.
• Cosmic Ray hits removed from single images (4 clipping).
16
Total Noise ResultsTotal Noise Results
• Total Noise Requirement: < 9 e- in 1000 sec using Fowler-8 sampling
– SCA 006• 6.2 e- (Temporal method), 6.7 e- (Full frame spatial method) @ T=30.0K• 6.4 e- (Full frame spatial method) @ T = 32.3K• For 1000 sec Fowler-1, total noise is 12.0 e- (temporal method) @T=30.0K
– SCA 008• 7.9 e- (temporal method) @ T=30.0K
17
Quantum EfficiencyQuantum Efficiency
• Photon sources and calibration equipment– For > 3.0 m, photon source is room temperature black body surface
monitored with a calibrated temperature sensor• Subtract “extra signal” from image taken of liquid nitrogen cup
– For 1.0 m < < 3.0 m, photon source is NIST calibrated black body (Omega BB-4A, 100 – 1000 C, =0.99)
– For <1.0 m, photon source is stabilized visible light source feeding an integrating sphere with a NIST calibrated Si diode detector
– cos4 corrected• Responsive Quantum Efficiency
– RQE = signal/(expected #photons)• Signal is averaged signal measurement, corrected for non-linearity• Expected # photons from NIST calibrated detector or spectral black body
calculations
• Detective Quantum Efficiency– DQE = (Signal/Noise)2/(expected #photons)
• Noise obtained via standard deviation of difference of two measurements
18
Quantum Efficiency ResultsQuantum Efficiency Results
RQE;
DQE
0.65m
RQE;
DQE
0.70m
RQE;
DQE
1.25m
RQE;
DQE
1.65m
RQE;
DQE
2.19m
RQE;
DQE
3.81m
RQE;
DQE
4.67m
RQE;
DQE
4.89m
SCA 006
88%;
82%
105%;
95%
107%;
97%
96.2%;
96.7%
84.6%;
85.3%
97.1%;
98.5%
84.7%;
85.0%
80.1%;
-
SCA 008
- - 114%;
97.1%
- - - 86.8%;
-
-
DQE closely matches expected value from AR coating transmission as provided by Raytheon. From this, we infer that the optical fill factor is > 98%.
19
Latent Image ResultsLatent Image Results
Test #
SrceFlux(e-/s)
Source Exposure (s)
Source Fluence (e-)
Delay (s)*
Latent Integr’n Time (s)
Max. DesiredLatent Fluence (e-: %)
Meas’d (%)Latent Fluence SCA006 ; SCA008
1 300 100 30,000 30 100 9 ; 0.03 0.3 ; 0.12
2 300 100 30,000 1000 100 0.9 ; 0.003 0.017 ; ≤0.01
3 30 1000 30,000 30 1000 4.5 : 0.015 ;
4 300 500 150,000 30 100 90 ; 0.06 0.48 ; 0.22
5 300 500 150,000 1000 100 9 ; 0.006 0.03 ; ≤0.01
6 3 10,000 30,000 200 8000 Noise level
7 15 10,000 150,000 200 8000 Noise level
20
OperabilityOperability
• Operability is affected by two types of defects:
– Missing contact between InSb diode implant and multiplexer unit cell• First InSb bump-bonding to mux had moderate outages.• Significant strides made in very short time (see next slides).
– PEDs (Photo-emissive defects)• Defect centers that glow (both IR and visible photons).• Techniques in place which either eliminate or dramatically reduce glow
region such that ~20-40 pixel diameter region fail operability.• Future multiplexers will have additional circuitry to fully eliminate all
PEDs.• Foundry improvement to reduce/eliminate defects.
21
OperabilityOperability
• SCA 006
– Basic Fail = 13.5%
– Large fraction failing are unconnected pixels
23
Radiometric StabilityRadiometric Stability
• Method of measurement
– Using similar technique as RQE measurement at = 3.50 m, a room temperature black body source was the source of “stable” flux.
– A calibrated temperature sensor was used to monitor/calibrate variations in the temperature of the black body (radiation source).
– A series of integrations were then taken over a 9 hour period.
– Most of the errors or inaccuracies in this measurement are a result of source calibration error or instabilities in our system electronics and not due to the SCA itself.
• Result
– SCA 006 exhibited instabilities < 0.07% over 1000 s and < 0.19% over the total 32000 s.
– Further improvement by factor of 10 - 100 may be gained by using our NIST calibrated black body source.
24
MTF and Electrical Cross-TalkMTF and Electrical Cross-Talk
• MTF– Measured using knife
edge and circular apertures placed in contact with InSb surface
– Edge spread functions shown for two wavelengths
– Edge spread modeled by diffusion and rectangular pixel function which is the ratio of {pixel pitch/ distance between photon absorption and the depletion region}
25
MTF and Electrical Cross-TalkMTF and Electrical Cross-Talk
• MTF results (cont.)
– From the best fit model parameter, (frequency in cycles/thickness) can be determined, which in turn leads to MTF:
MTF = 0.64 (2 e –2)/(1 + e-4)
– If Nyquist frequency is taken as ½ , then MTF = 0.45• Similar measurement on SB-226 InSb SCA produced MTF=0.52
– If Nyquist frequency is taken as ¼ , as in Rauscher’s MTF document, then MTF = 0.58
• Exceeds (existing) requirement of 0.53 in JWST NASA 641 document
26
MTF and Electrical Cross-TalkMTF and Electrical Cross-Talk
• Cosmic ray hit pixel upsets used to quantify electrical cross-talk
– Histogram of 30K dark data difference showing peaks at 0.1% for next nearest neighbors and 0.5-1.2% for nearest neighbors
– Cross talk is < 2%
27
MTF and Electrical Cross-TalkMTF and Electrical Cross-Talk
• 4th pixel over electrical cross-talk
– 4 interleaved outputs = next pixel on same output is 4 pixels away
– Deterministic, can be removed or corrected in software
– Below is a table of pixel values in percentage of a single cosmic ray event; notice 4th pixel over is 2%
0 0.025 0.012 0.025 0.012 -0.025 0.037 -0.037 0.012 0.099
0 -0.025 0.074 0.546 0.099 0 0.037 -0.012 0.025 -0.062
0.012 -0.050 1.142 100 0.782 0.137 -0.248 2.062 -0.211 0.012
0.062 0.012 0.161 0.733 0.012 0.062 -0.074 0 -0.050 0
0.025 -0.062 -0.037 0.012 0.012 0 0.074 0.025 0.012 0.001
28
Additional TestsAdditional Tests
• NASA Ames conducted proton radiation testing at UC Davis
– Please see talk “Radiation environment performance of JWST prototype FPAs” 5167-25 on Wednesday
• STScI IDT Lab conducted independent tests on both InSb detector arrays from Raytheon and HgCdTe detector arrays from Rockwell Scientific.
– Please see talk “Independent testing of JWST detector prototypes” 5167-29 on Wednesday
29
Summary ofSummary ofSB-304 InSb SCA PerformanceSB-304 InSb SCA Performance
Parameter Requirement (Goal) SB-304-006 Result SB-304-008 Result
SCA Format 2048 x 2048 pixels 2048 x 2048 active + 2 reference columns
2048 x 2048 active + 2 reference columns
Fill Factor 95% (100%) 98% (100%) 98% (100%)
Bad Columns/Rows
<5 containing >1000 No Yes
Bad Pixel Clustering
< 20 cluster up to 20 pixels
No Yes
Pixel Operability >98% 86.5% basic,
82.1% meet N+QE
98.1% basic,
91.5% meet N+QE
Total Noise 1000 s 9 e- (2.5 e-) 6.2 e- 7.9 e-
Read Noise for single read
15 e- (7 e-) 12 e- (CDS) 14.5 e- (CDS)
Dark current < 0.01 e-/s 0.012 e-/s 0.025 e-/s
30
Summary ofSummary ofSB-304 InSb SCA PerformanceSB-304 InSb SCA Performance
Parameter Requirement (Goal) SB-304-006 Result SB-304-008 Result
DQE 70% 0.61.0 m
80% 1.05.0 m
(90%; 95%)
82% @ 0.65 m
97% @ J,H,L’’
-
97% @ J
Well Capacity > 6x104e- (2x105e-) 1.4 x 105e- 1.3 x 105e-
Electrical Cross-talk
<5% (<2%) <1.3% (nearest and next nearest pixel)
<1.3% (nearest and next nearest pixel)
Radiometric Stability
1% over 1000 s < 0.07% over 1000s < 0.07% over 1000s
Latent Image < 0.1% after 2nd read following >80% full well exposure
0.3%
(no amelioration)
0.12%
Frame Read Time 12 sec (<12 sec) < 11 sec < 11 sec
Pixel read rate 100KHz; 10 s/pix 100KHz; 10 s/pix 100KHz; 10 s/pix
Sub-array read 0.2 s for 1282 pixels <0.05 s for 1282 <0.05 s for 1282
31
ConclusionsConclusions
• Raytheon has produced a robust, mature technology.
• Both the InSb detector arrays from Raytheon and the HgCdTe detector arrays from Rockwell Scientific have demonstrated excellent performance.
• The University of Arizona has selected Rockwell Scientific to produce the NIRCam SCAs and FPAs.
– Congratulations to UH and RSC!