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TELEDYNE’S HIGH PERFORMANCE INFRARED DETECTORS FOR SPACE
MISSIONSPaul Jerram and James
BeleticICSO October 2018
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Teledyne Imaging SensorsCamarillo, California(Design, Fab, I&T)
Teledyne Judson TechnologiesMontgomeryville, Pennsylvania
(Design, Fab, I&T)
Teledyne DALSAWaterloo, Ontario (Design, I&T)Bromont, Quebec (CCD fab)
Teledyne e2v Space ImagingChelmsford, England (Design, Fab, I&T)
Grenoble, France (Design, I&T)
• Teledyne utilizes leading CMOS foundries for fabrication of CMOS image sensors
• Including staff who work in machine vision (locations not shown on map), Teledyne employs 100 CMOS image designers and 7 CCD designers
Teledyne High Performance Image Sensors
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Micro‐CamTM
Infrared Microscope Camera
High Speed (1600 Hz)Long‐Wave IR camera for Lab Instrumentation
Photodiode Thermoelectricallycooled packaging
320×256 Array
1‐D Photodiode Array
Space Flight PackagingNASA JWST 4 Mpixel
Aircrew Laser Eye Protection
High Speed Camera for Tactical Application
Compact Camera Electronics
Custom Visible & IR Arrays for DoD Space Applications
• Infrared and visible sensors• Custom cameras• Focal plane electronics• Laser eye protection & sensor protection• Infrared detectors, photodiodes & arrays• Detector packaging• Custom sensors for tactical and space • Infrared cameras• Camera electronics• Integration and test of IR camera systems
16 Million Pixel Infrared Astronomy
Array
Teledyne Image Sensors ‐ Products
Teledyne’s High Performance IR Sensors for Space Missions
4Tunable Wavelength: Unique property of HgCdTeHg1-xCdxTe Modify ratio of Mercury and Cadmium to
“tune” the bandgap energy
G. L. Hansen, J. L. Schmidt, T. N. Casselman, J. Appl. Phys. 53(10), 1982, p. 7099
5.3
HgCdTe crystal is grown by MBE on CdZnTe Substrates xTxxxEg 211035.5832.081.093.1302.0 432
Teledyne’s High Performance IR Sensors for Space Missions
Readout CircuitInput signal
• Flux – object and backgroundOperating Mode
• Integration time• Frame readout time• Shutter (rolling, snapshot)• Multiple storage cells per pixel• Windows • Reset (pixel, line, global)• Event driven
Interface• Input (analog, digital)• Output (analog, digital)• # of readout ports
Environment• Temperature• Radiation
Other Requirements• Linearity• Anti-blooming
The functionality (“the brains”) of a CMOS‐based
sensor is provided by the readout circuit
Detector• Wavelength (λ)• Quantum Efficiency• Dark current & Noise• Radiation environment• Persistence
Hybrid CMOS Image Sensor
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Note that the incident photons must first pass through the CdZnTe substrate
Cosmic rays in the CdZnTe substrate give fluorescence that creates signal in the HgCdTe
The substrate will also decrease QE below 1.3µm
Substrate removed HgCdTe
p-type HgCdTe
epoxyROIC input
indium bump
silicon multiplexer
OutputSignal
p-type HgCdTe
Bulk n-type HgCdTe
CdZnTe Substrate
Incident PhotonsCosmic Ray
NB schematic is not to scale
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Note that the incident photons must first pass through the CdZnTe substrate
Cosmic rays in the CdZnTe substrate give fluorescence that creates signal in the HgCdTe
The substrate will also decrease QE below 1.3µm
Substrate removed HgCdTe
p-type HgCdTe
epoxyROIC input
indium bump
silicon multiplexer
OutputSignal
p-type HgCdTe
Bulk n-type HgCdTe
The substrate is removed down to the HgCdTe layer
An AR Coating can now be applied to give excellent QE down to below 400nm
IncidentPhotons
AR Coating
Teledyne’s High Performance IR Sensors for Space Missions
JPL AVIRIS‐NG Imaging Spectrometer
JPL AVIRIS‐NG Imaging Spectrometer
380 nm
2510 nm
Atmospheric water vapor absorption bandsat 1400 and 1900 nm
Substrate removed HgCdTe Provides Simultaneous UV‐Vis‐IRLight Detection
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• For high flux (300K scenes), will double operating temperature
• Less expensive cooling options• Longer cooler operating lifetime• Able to operate LWIR with mini cryo-coolers
• For low flux applications• Lower dark current at standard oper. Temp.• Higher operating temperature• Longer cooler operating lifetime
• Status• Demonstrated 10X to 100X reduction in dark
current• LWIR 128x128, 1280x480, and 640x512
arrays have been tested• MWIR operated up to 250K• LWIR operated up to 160K
• Strong funding for development• Developing partnerships with aerospace
primes for system insertion• Will utilize for commercial instrumentation
products
Teledyne’s high quality HgCdTe is getting even better!Applications will soon benefit from a major reduction in HgCdTe dark current
Promise of Fully Depleted HgCdTe
Teledyne’s High Performance IR Sensors for Space Missions
Optimized for imaging spectrometers (hyperspectral imaging)Programmable, digital input: clocks and biases generated on‐chipAnalog output, one output every 160 columns (10 MHz pixel rate)Snapshot, integrate‐while‐read, nearly 100% duty cycleCTIA unit cell
+ 30 x 30 micron pixel pitch+ High linearity (>99% linear over full range)+ Full well sizes (700 ke‐, 1 Me‐, or 5 Me‐)
Formats (columns by rows; spatial by spectral pixels)+ 640 × 480 Delivered in 2012+ 1280 × 480 Delivered in 2014+ 1600 × 480 ROICs fabricated
Focal plane electronics (16 bit, 10 MHz ADCs, CameraLink interface)Windowing available in row directionFrame readout time scales with number of rows read out
+ Row readout time is 16.8 microsec+ Full‐frame rate (480 rows) is 125 Hz+ Half‐frame rate (240 rows) is 250 Hz
Low power: 90, 150, 180 mW for CHROMA 640, 1280 and 1600 formatsPerformance (advertised specs):
Focal PlaneElectronics (FPE)
CHROMA 1280×480Sensor Chip
Assembly (SCA)
Available support equipment:– Focal Plane Electronics (FPE):
engineering/lab grade only– Flex Cables: warm and cold cables,
engineering/lab grade only
CDS Noise Well = 0.7M e‐
CDS Noise Well = 1M e‐
CDS Noise Well = 5M e‐
CHROMA‐320 120 e‐ 145 e‐ 600 e‐ 70 14.4 x 19.4 2
CHROMA‐640 120 e‐ 145 e‐ 600 e‐ 90 24.4 x 19.5 4
CHROMA‐1280 120 e‐ 145 e‐ 600 e‐ 150 43.2 x 19.6 8
CHROMA‐1600 120 e‐ 145 e‐ 600 e‐ 180 52.8 x 19.7 10
Array FormatWell capacity & Readout Noise Power
dissipation at 125 Hz [mW]
ROIC dimensions
[mm]
No. Outputs
Actual noise performance is 15%-20% lower (better) than listed above10
CHROMA used by:• Several JPL spectrometers
• CLARREO Pathfinder on ISS
CHROMATM (Configurable Hyperspectral Readout for Multiple Applications)
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GeoSnap3K×3K
CHROMA‐D1K×512
CHROMA‐D3K×512
GeoSnap2K×2K
GeoSnap / CHROMA‐D Design• 18 micron pitch pixel• CTIA unit cell with 2 gains / full well
• 100 ke- and 1 Me- or 180 ke- and 2.7 Me-• Stitchable design, up to 3K×3K pixels• Snapshot, integrate while read• Fully digital chip, 14 bit ADCs• Full frame rate: 120 Hz for 2K×2K, 250 Hz for 3K×512• ROIC formats fabricated: 2K×2K, 2K×512, 3K×512• Focal plane arrays made and tested with several types of detectors:
• Visible (Silicon), MWIR (5.3 µm HgCdTe), VLWIR (14.5 µm HgCdTe)
ROIC Focal Plane Module
• ROIC passed radiation tests (no latchup)• GeoSnap 2K×2K space flight package developed• GeoSnap 2K×2K in production (TRL 6)• Being used for Visible, MWIR, VLWIR • CHROMA‐D 2K×512 and 3K×512 being developed for Earth Science applications
GeoSnap‐18 (Stichable to 3k x 3k)
Detectors and missions
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• Euclid is the European Space Agency’s next flagship astronomy mission.
• Target launch date is 2021.• Euclid has a 1.2‐m diameter large field of view telescope with visible and infrared arrays produced by Teledyne:
• 600 million visible pixels• 36 4K×4K (16 Mpix) CCDs
• 64 million infrared pixels• 16 H2RG (4 Mpix) SWIR arrays• 16 SIDECAR ASIC modules
• Largest IR focal plane array when it launches• 24 flight candidate H2RGs delivered to NASA• NASA tested and delivered 20 flight grade H2RG arrays to ESA, all of which greatly exceed requirements
Quantum Efficiencyof 24 flight candidate H2RGs
Measured by Goddard SFC Detector Characterization Laboratory
Teledyne Visible and IR detectors for Euclid
Teledyne Imaging Sensors H2RG
2K×2K pixels, 18µm pitch
e2v CCD 273‐84
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Dark Current at 100KMedian = 0.012 e‐/pix/sec
More than 5X betterthan specification (0.07 e‐/pix/sec)
2.3 µm cutoff wavelength
Readout NoiseMedian = 6.8 e‐
40% better than specification (11.5 e‐)
H2RG IR Detectors for Euclid
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• H4RG‐10: 4K×4K pixels, 10 µm pixel pitch
• Technology Maturation (2014‐2018) achieved all goals• Reduced H4RG‐10 noise• Increased operability of 16 megapixel IR arrays• Demonstrated H4RG‐10 flight performance• Demonstrated yield for flight production• Made the arrays flatter (smaller peak‐to‐valley)• Reduced image persistence
• Flight Production commenced in June 2018
2.4 meter telescope
Measured by the Detector Characterization Lab, Goddard Space Flight Center
NASA WFIRST Mission
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JUICE MAJISVIS‐IR Spectrometer
JUICE MAJISVIS‐IR Spectrometer
Jupiter + Ganymede, Calisto & Europa
Trojan Asteroids
LucyL’RalphVis‐IR
spectrometer
LucyL’RalphVis‐IR
spectrometer
• 1 H2RG MWIR array
• MWIR CHROMA‐A 320×480
• Focal Plane Electronics
Europa ClipperMISEVis‐IR
spectrometer
Europa ClipperMISEVis‐IR
spectrometer
Europa Image Here
Europa
Missions for Jupiter and it’s neighborhood
• 1 H1RG SWIR array• 1 H1RG MWIR array• 2 SIDECAR ASIC Modules
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Image Sensor RequirementsWavelength (µm) 6 – 10
Operating temperature range (K) 35 – 40 Integration time (s) 10
Dark current (e‐/s/pixel) <200Read noise (correlated double sample; e‐) <30
Quantum efficiency (%) >60Well depth (e‐) >45,000
Pixel operability (%) (with all above properties) >90
• NEOCam will fly two mosaics• 2K×8K MWIR (5 µm cutoff)• 2K×8K LWIR (10 µm cutoff)
• MWIR H2RG produced for several years for ground-based astronomy and JWST
• LWIR now made in 2K×2K format (H2RG)• Largest high performance LWIR
detectors ever made• Each mosaic will be 4 H2RGs
• Mission will fly 8 H2RGs and 8 SIDECAR ASIC modules
• Teledyne has developed a new H2RG package and qualified to TRL-6
• Active program of continued development
NEOCam Asteroid Survey Mission
Teledyne’s High Performance IR Sensors for Space Missions
Calibrated Radiance SpectraAVIRIS-NGImaging Cube
Instrument Calibration LAEGERN Test Site
380 to 2510 nm5 nm resolution
Avaris‐NG First Measurements in EuropeSwitzerland June 2018
Teledyne’s High Performance IR Sensors for Space Missions
• 256×256 pixels• 40 micron pixel pitch• 8 spectral channels (4 to 12 µm)• Full well optimized per channel• 4 rows (selected) read out per channel• 30,000 Hz frame rate• Developed for HySpIRI TIR• Being deployed in ECOSTRESS,
installed on the ISS
JPL FPA measurements (William Johnson & the PHyTIR team)• Cutoff wavelength = 12.9 µm• Operating temp = 60 K• Dark current = 183 e-/pix/sec (spec is <283 e-/pix/sec)• Full well optimized per channel, from 6 to 8 million electrons
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High Speed MWIR‐LWIR Multi‐Spectral Focal Plane Array
First light results from ECOSSTRESS. Showing the temperature variation over LA at different times of the day.
The ECOsystem SpaceborneThermal Radiometer Experiment on Space Station (ECOSTRESS) will measure the temperature of plants and use that information to better understand how much water plants need and how they respond to stress
Image Courtesy NASA/JPL‐Caltech
ECOSTRESS first results
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If you are interested in this technology please come and
talk to Teledyne‐e2v about how we can meet your needs
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