14 January 2003 Special LASP Seminar at GSFC 1 JWST's Near-Infrared Detectors: Ultra-Low Background Operation and Testing Bernard J. Rauscher Space Telescope Science Institute
Mar 20, 2016
14 January 2003 Special LASP Seminar at GSFC 1
JWST's Near-Infrared Detectors:Ultra-Low Background Operation and
Testing
Bernard J. RauscherSpace Telescope Science Institute
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Outline• What is a Near-Infrared Array Detector?• JWST Science Drivers• Detector Requirements• Detector testing at STScI/JHU• Optimal Use• Summary
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JWST’s IR Arrays are “Hybrid” Sensors• PN junctions are
“bump bonded” to a silicon readout multiplexer (MUX).
• Silicon technology is more advanced than other semiconductor electronics technology.
• The “bump bonds” are made of indium.
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1.E-04
1.E-03
1.E-02
1.E-01
1.E+00
1.E+01
1.E+02
0.1 1 10
Wavelength [m]
Sign
al [e
-/sec
/pix
]
Zodiacal Light
Sunshield
JWST requirement
JWST goal
R=5
R=1000
JWST Needs Very Good Near Infrared Detectors!• Completing the JWST Design
Reference Mission “on time” requires background limited near-infrared (NIR) broadband imaging
• Zodiacal light is the dominant background component in the NIR
• The total NIR detector noise requirement is therefore =10 e- rms in a t=1000 seconds exposure.
• NIRSpec will probably be detector noise limited. The total noise goal is =3 e- rms per 1000 seconds exposure
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JWST Near Infrared (NIR) Detector Requirements
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Detector Testing at STScI/JHU:Independent Detector Testing Laboratory
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Past and present personnelEddie BergeronData Analyst
Mike TelewiczIntern
Gretchen GreeneMechanical Engineer
Monica RiveraIntern
Russ PeltonTechnician
Tom ReevesLab Technician
Bernie RauscherProject Scientist
Steve McCandlissJHU Lead
Scott FelsIntern
Sito BallezaSystems Engineer
Robert BarkhouserOptical Engineer
Utkarsh SharmaGraduate Student
Ernie MorseData Analyst
Don FigerDirector
Mike ReganSystem Scientist
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Dark Current• Lowest measured dark current is ~0.006 e/s/pixel.
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• Read noise is ~10 e for Fowler-8. (system read noise is ~2.5 e)
IDTL Measurements: Read Noise
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IDTL Measurements: Conversion GainPer correlateddouble sample
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Hawaii 1R with 5 um Cutoff
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IDTL Measurements:Relative and Absolute Quantum Efficiency
Relative Quantum Efficiency for H1RG, 10/18/2002
We are currently working on better calibration to enable measurements of absolute QE vs. wavelength.
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Relative QE Maps• Relative QE maps show significant structure
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IDTL Test System
Hawaii Detector
Hawaii Shirt
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Then & Now
November 2000
November 2002
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IDTL First Light Images
Jan. ‘01 (MUX)
Raytheon ALADDIN
Feb. ‘02 (MUX)
Apr. ‘02 (SCA)
Rockwell HAWAII-1R Rockwell HAWAII-1RG
Jun. ‘02 (MUX) Jul. ‘02 (SCA)
Raytheon SB-304
Nov. ‘02 (MUX)
Rockwell HAWAII-2RG
Jan. ‘03 (MUX)
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IDTL Test SystemLeach II Controller Electronics
Vacuum Hose
He Lines
EntranceWindow
Dewar
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Detector Readout System
Unix Instrument Control Computer
COTS Leach II IR Array Controller
Warm Harness
Cryogenic Harness
Detector Customization Circuit
JWST SCA
T~293 K
T=30-50 K
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An Adaptable Readout System• The only hardware change
required to run a different detector is swap-in a DCC.
• We have DCCs for the following detectors.
– Raytheon• SB-290• SB-304
– Rockwell• HAWAII-1R• HAWAII-1RG• HAWAII-2RG
• Each DCC is a multi-layer PCB. Extensive use of surface mount technology. Includes flexible “neck” to simplify interfacing.
Rockwell HAWAII-2RG Detector Customization Circuit (DCC)
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Close-up ofDetector Customization Circuits
(DCCs)
Rockwell HAWAII-2RG Raytheon SB-290/SB-304
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Optimal Use
• JWST Detector Readout Strategies• Anomalies seen in other instruments• Other effects…• Use of Reference Pixels
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Detector Readout• JWST science requires
MULTIACCUM and SUBARRAY readout.
• Other readout “modes” can be implemented using parameters.– For example, Fowler-8 can be
implemented as MULTIACCUM-2x8.
• Cosmic rays may be rejected either on the ground or on-orbit. MULTIACCUM parameters: texpose = exposure time,
t1 = frame time, and t2 = group time. The small overhead associated with finishing the last group of samples is not included in the exposure time.
MULTIACCUM Detector Readout
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NICMOS Anomalies (& how JWST will avoid them)• Dark current
– JWST detectors already designed to minimize glow
– Careful detector characterization & selection– Do not exceed max temp. requirement!
• Bias drifts– Good electronic design
• Avoid power supply coupling• Avoid ground coupling• Reference pixels will help• Synchronous readout can help
• QE variations– Careful detector characterization & selection
• Amplifier glow– JWST detectors should be much better than
NICMOS
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NICMOS Anomalies: 2• Persistence
– There will be persistence on JWST
– Strongly dependent on detector fabrication process
– Careful detector characterization & selection needed to choose best detectors
– In IDTL, we are exploring mitigation measures
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NICMOS Anomalies: 3• DC bias level drift
– Good electronic design is first line of defense
– Reference pixels should eliminated “Pedestal” drifts.
– Depending on reference pixel layout, reference pixels may help reject “bands”.
• Ghosts– In NICMOS, may result from
ground plane coupling within the MUX.
– Also seen in SIRTF InSb radiation testing.
– Good cable harness and electronic design help
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NICMOS Detector Effects• Linearity
– In NICMOS, ~10% intrinsic non-linearity can be calibrated out to within ~0.2%.
• Well depth– Well-depth is a function of reverse
bias in photo-voltaic detectors.– Well-depth can also depend on
temperature.– In the IDTL, we will study well
depth as a function of reverse bias and temperature.
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NICMOS Detector Effects: 2
• QE– Can depend on
wavelength and temperature.
• Dark current “bump”– This is a curious
effect seen in NICMOS.
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Reference Pixels
Raytheon 2Kx2K NIR Module
Rockwell 2Kx2K NIR Module
• All candidate JWST detectors have reference pixels
• Reference pixels are insensitive to light
• In all other ways, designed to mimic a regular light-sensitive pixel
• NIR detector testing at University of Rochester, University of Hawaii, and in the IDTL at STScI -> reference pixels work!
• Reference pixel subtraction is a standard part of IDTL data reduction pipeline
Raytheon 1024x1024 MIR MUX
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Use of Reference Pixels• JWST’s NIR reference pixels will be grouped in columns and possibly
rows• Most fundamentally
– reference pixels should be read out in exactly the same manner as any “normal” pixel
– Data from many reference pixels should be averaged to avoid adding noise to data
• We have begun to explore how reference pixels should be used. Approaches considered include the following.– Maximal averaging (average all reference pixels together and subtract the
mean)– Spatial averaging– Temporal averaging
• Spatial averaging is now a standard part of IDTL calibration pipeline
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A Picture of IDTL System Noise
• Shorting resistor mounted at SCA location• 1/f “tail” causes horizontal banding.• Total noise is =7 e- rms per correlated double sample.
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Averaging small numbersof reference pixels adds noise
• Averaged the last 4 columns in each row and performed row-by-row subtraction
Before After
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Spatial Averaging• In spatial averaging, data from
many (~64 rows) of reference pixels are used to calibrate each row in the image
• A Savitzky-Golay smoothing filter is used to fit a smooth and continuous reference column
• This reference column is subtracted from each column in the image
• Using this technique, we can remove some 1/f noise power within individual frames
• In practice, this technique works very well
This is a standardpart of the IDTL datacalibration pipeline
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Spatial Averaging: Before & After
Before After
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Temporal Averaging• Dwell on the reference
pixel and sample many times before clocking next pixel
• Potentially removes most 1/f
• Not tried this in IDTL yet. U. Hawaii has reported some problems with reference pixels heating up
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Temporal Averaging: Before & After
Before After
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Summary of Reference Pixel Calibration Methods• Spatial averaging works
well using a Rockwell HAWAII-1RG detector
• Based on conversations with U. Rochester, we foresee no problems with SB-304
• Temporal Averaging is promising. More work needed using real detectors.
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Summary• The Independent Detector Testing Laboratory (IDTL) at STScI/JHU is up
and running• Test results including dark current, read noise, conversion gain,
relative quantum efficiency, and persistence are in good agreement with other JWST test labs
• Reference pixels work and are an invaluable part of the data calibration pipeline
• We have explored three techniques for using reference pixels– Maximal averaging,– Spatial averaging, &– Temporal averaging
• Spatial averaging works well and is robust• Early reports from U. Hawaii using temporal averaging are not
encouraging due to reference pixel self-heating. More work is planned in the IDTL