Earth Science Technology Office - QWEST and …...2010/02/24 · QWEST and HyTES: Two New...
Transcript of Earth Science Technology Office - QWEST and …...2010/02/24 · QWEST and HyTES: Two New...
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QWEST and HyTES: Two New Hyperspectral Thermal Infrared Imaging
Spectrometers for Earth Science Simon Hook, PI
Jet Propulsion Laboratory, California Institute of Technology
Task Manager: Bjorn Eng Optics: Zakos Mouroulis, William Johnson Detectors: Sarath Gunapala, Cory Hill, David Ting Gratings: Dan Wilson Mechanical: William Johnson Thermal: Chris Paine, Andy Lamborn Science: Vince Realmuto, Simon Hook Data recording and storage: Bjorn Eng
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 2
Outline • Science goals and task objectives • Technical developments to date
– System design – Optics – Detectors – Mechanical – Thermal – Data recording and storage
• Radiometric analysis of QWEST • Summary and Conclusions
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 3
Overall Science Goal and Objective
• Provide precursor high spectral and spatial resolution thermal infrared data for the NRC Recommended HyspIRI mission and for use in Earth Science Studies.
• Build and deploy an airborne Hyperspectral Thermal Emission Spectrometer (HyTES) with 512 pixels across track with pixel sizes in the range of 5 to 50 m depending on aircraft flying height and 256 spectral channels between 7.5 and 12 µm.
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Copyright 2009 California Institute of Technology. Government sponsorship acknowledged. 4
NRC Decadal Survey HyspIRI Visible ShortWave InfraRed (VSWIR) Imaging Spectrometer
+ Multispectral Thermal InfraRed (TIR) Scanner
VSWIR: Plant Physiology and Function Types (PPFT)
Multispectral TIR Scanner
RedtidealgalbloominMontereyBay,CA
Mapofdominanttreespecies,BartlettForest,NH
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged.
5
HyspIRI Thermal Infrared Multispectral (TIR) Science Measurements
Science Questions: TQ1. Volcanoes/Earthquakes (MA,FF) – How can we help predict and mitigate earthquake and volcanic hazards through
detection of transient thermal phenomena? • TQ2. Wildfires (LG,DR) – What is the impact of global biomass burning on the terrestrial biosphere and
atmosphere, and how is this impact changing over time? • TQ3. Water Use and Availability, (MA,RA) – How is consumptive use of global freshwater supplies responding to changes in climate
and demand, and what are the implications for sustainable management of water resources?
• TQ4. Urbanization/Human Health, (DQ,GG) – How does urbanization affect the local, regional and global environment? Can we
characterize this effect to help mitigate its impact on human health and welfare? • TQ5. Earth surface composition and change, (AP,JC) – What is the composition and temperature of the exposed surface of the Earth? How do
these factors change over time and affect land use and habitability?
Measurement:
• 7 bands between 7.5-12 µm and 1 band at 4 µm
• 60 m resolution, 5 days revisit
• Global land and shallow water
Volcanoes
Urbanization
Water Use and Availability
Surface Temperature Evapotranspiration
Andean volcano heats up
Multispectral Scanner
Schedule: 4 year phase A-D, 3 years operations
High Heritage
TIR
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 6
Volcanoes
How can we help predict and mitigate earthquake and volcanic hazards through detection of transient thermal phenomena?
Wildfires
What is the impact of global biomass burning on the terrestrial biosphere and atmosphere, and how is this impact changing over time?
Water Use and Availability
How is consumptive use of global freshwater supplies responding to changes in climate and demand, and what are the implications for
sustainable management of water resources?
Urbanization
How does urbanization affect the local, regional and global environment? Can we characterize this effect to help mitigate its impact
on human health and welfare?
Land surface composition and change
What is the composition and temperature of the exposed surface of the Earth? How do these factors change over time and affect land use and
habitability?
Thermal Imaging Spectroscopy for Earth Science
Thermal spectroscopy acquires both the emission from the target source object as well as reflected and/or transmitted emission from surrounding and/or foreground objects.
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 7
Steamboat Springs
8 16
11b 12
18
Map Color Legend
Silica-rich (Opal, Quartz, Alunite)
Clay-rich (Kaolinite, Montmorillonite, Muscovite, Illite)
Em
issi
vity
(offs
et fo
r cla
rity)
Wavelength (mm) 8 10 11 12
0.7
0.8
0.9
1.0
9 Wavelength (mm)
8 10 11 12 9
Site 16
Site 8
Site 11b
Site 18 Alunite
Quartz
Opal
Montmorillonite
Kaolinite
0.5 km N
Emissivity plots derived from spectra
Thermal Imaging Spectroscopy for Earth Science
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 8
HyTES Task Objectives
• Develop a calibrated, airborne imaging spectrometer operating between 7.5 and 12 µm with 256 spectral channels
• Develop an initial overall system design – Optical design – Thermal/mechanical design – Data acquisition and recording system
• Evaluate key design elements using the existing JPL Quantum Well Earth Science Testbed (QWEST), in particular 7.5-12 µm QWIP FPA
• Design and fabricate: – Overall system, Optics, Detectors, Grating, Mechanical, Thermal, Data recording
and storage • Assemble, test and calibrate in the laboratory • Complete aircraft-integration • Deploy from an airborne platform over test sites in Western USA • Provide data to HyspIRI Study Group
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 9
System Design
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 10
HyTES System Block Diagram
The HyTES airborne instrument is a mechanically cooled system consisting of a vacuum chamber, cryocoolers, thermal radiation shields, telescope/relay, and spectrometer
The mechanical coolers are a design change from the original proposal
100 K
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 11
HyTES cryovacuum package • Mechanical components:
– mechanical cryocoolers (2) – vacuum enclosure – floating radiation shields (2) – thermal isolation struts – QWIP focal plane array with positioning assembly – spectrometer – telescope and relay optics
• Temperature requirements: – QWIP FPA <40 K for dark current supression – Spectrometer <100 K for background supression – Relay optics <250 K with stability restrictions – Telescope ~room temperature
• Chose to cool the optical instrument to 100 K – single mechanical assembly is highly desirable for
alignment – cold relay eliminates temperature variation concerns
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 12
Optics
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 13
Parameter Value
Spectral range 7.5-12 mm
Spectral channels (sampling) 256 (17.6 nm)
Field of view 48.3o
IFOV (pixel subtense) 1.44 mrad
Spatial elements 512
First order specifica.ons
Fore-optics Spectrometer
Telescope
Relay Grating Dyson Block
HyTES Optics
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 14
Telescope
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 15
HyTES Telescope
Telescope section with rays traced from ground.
Telescope with rays traced from NADIR
Optical Surface A
Optical Surface B
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 16
HyTES Telescope
Section showing HyTES telescope. The telescope is all-
aluminum, diamond-turned, athermal, “snap-together” design.
No real technical hurdles. Diamond turning process is well
defined.
Numerous accessories are also part of the design including: • Aperture baffle
• 2 Internal baffles • Rear slot baffle
• Precision made large shim
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 17
HyTES Telescope
Telescope design provides a direct connection to the relay housing
Relay Housing Telescope
Shim connector
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 18
Spectrometer (Slit, Dyson Block and Grating)
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HyTES Spectrometer-Block monolithic ZnSe block
spectrum
slit
70 mm
grating
Optical prescription
HyTES Spectrometer delivered in May 2010
Copyright 2010 California Institute of Technology. Government sponsorship acknowledged.
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 20
HyTES Concave Grating
Incident
-1 Order
HyTES Spectrometer Ray Trace Grating
Wavelength Range 7.5 - 12 µm
Incident angle ~17.9 deg
Diffraction order -1
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HyTES Concave Grating Design Simulation
• High efficiency across the band • Polarization sensitivity should not be an issue due
to the expected unpolarized TIR radiation • Anomalies in the 7.7 to 7.9 µm region are due to
the +2 and -4 diffraction orders becoming evanescent (cut-off) and coupling energy out of the -1 order. If there is a range of incident angles, the anomalies will be less sharp
Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 21
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Fabricated 7.5 to 12 µm HyTES Grating
• Grating successfully fabricated (ZnSe substrate, grooves etched in PMMA resist, gold reflective coating)
• Measured blaze angle is ~13.1° (9% deeper than 12° design) – will decrease efficiency at 7.5 µm and increase efficiency at 12 µm as simulated above
Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 22
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HyTES Slit Design The slit was made using Reactive ion etching (RIE) of silicon nitride (Si3N4) films formed by low pressure chemical vapor deposition (LPCVD) Usually, the silicon nitride is grown on a silicon wafer at a high temperature, 815 C or so. The recipe is adjusted so that when it comes down to room temperature, the nitride is under light tensile stress (50-100 Mpa).
Thickness of substrate: 1mm
Outer dimensions: cut to 1.0” x 1.5”
Clear aperture: 20mm x 39µm
SEM of JPL slit shows high edge quality.
Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 23
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 24 24
Detectors
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Detector Array Plan
1024x1024 pixel single-band QWIP FPA
• HyTES will use a 1024x1024 pixel array covering the 7.5-12µm spectral band (typical array shown at top right)
• A two-band quantum well infrared photodetector (QWIP) array has been selected as the detector array material
• JPL has fabricated and delivered similar large area and multi-band (dual color, three color and four color) arrays in the past
• This is not a commercially available technology, and only JPL delivers large format, high performance multi-band QWIP arrays
• The detector array has the following requirements:
• 1kx1k format, SBF 184 ROIC • Minimum operating temperature 40K • Performance such that in each of the 2-
column averages in the 7.5-12µm band the NEDT is less than 200 mK
λ4-5µm 8-9µm
10-12µm 14-15µm
Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 25
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Detector Array Design
• The detector array will be processed as two separately optimized spectral bands, which together cover the entire 7.5-12µm spectral range
• This is the first time a high-performance QWIP array has been used in a hyperspectral application
• The spectral responsivity for the two bands designed for HyTES are shown here and together cover the 7.5-12µm band
• This customized array response is made possible by a design and fabrication method which allows many separate bands to be grown and processed monolithically on the same semiconductor wafer (an example with multiple bands is shown on the right)
Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 26
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FPA Fabrication • A cross section of the two-band quantum well infrared photodetector
(QWIP) used as the detector material is shown below • This is similar to the previous three-band design but much simpler to
process • Roughly half of the array will respond in the 7.5-10µm range, and the
other half will cover the 10-12 range
HyTES pixel design – cross-sectional zoom at the transition point, showing two bands with
¼ lamda gratings on each
10-12 mm
7.5-10 mm
Top-down view of FPA
λ
spatial
Long wavelength band
10-12 mm
Short-middle w
avelength band 7.5-10 m
m
Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 27
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Detector Design Status
• The measured dual band response is shown at right
• The measured spectra meet specifications
• Several samples were optimized in the November 2009 -January 2010 time frame to optimize the detector performance and balance the response for a single bias
• These experimental results were used to model the system performance using a QWIP detector array
• Initial wafers were grown at JPL and eight additional 100mm wafers have been delivered to JPL from an outside vendor
Experimental data on final test detectors
Bias 1.35V, 40K operation, 200x200µm squares
Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 28
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System Modeling
Modeling shows the system with a QWIP array based on this design meets specifications in the 7.5-12µm band
The new, optimized two-color version exhibits a smoother transition between bands than the original three-color version and meets spec (NEDT < 200mK) throughout the 7.5-12µm band
Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 29
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Initial HyTES wafer
• This wafer was competed at the end of May and shipped for hybridization. All layers met processing design spec and should yield excellent arrays
Twelve 1kx1k HyTES arrays on 4” GaAs wafer
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 31
Mechanical
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Telescope
Relay Spectrometer
Floating Shields (2) Stabilizing Struts (3)
Mechanical Cryocoolers
Vacuum Backplate
Nadir-pointing window
FPA
Vacuum Frontplate
HyTES Mechanical
32 Slit Grating
Cylindrical Vacuum Shell
Copyright 2010 California Institute of Technology. Government sponsorship acknowledged.
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 33
Opto-Mechanical
FPA
Kinematic stand-off
HyTES Mechanical
• Matching coefficient of thermal expansion (CTE) between optics and mechanical components to minimize inherent stresses caused by thermal soak
• Kinematic mounting allows minimization of stress in optical and mechanical members in all degrees of freedom
• Kinematic mounting used whenever possible to compensate for low to high CTE metal materials.
Kinematic struts
Spectrometer Housing
Relay Housing
Telescope Housing
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 34
Existing QWEST mechanical housing
HyTES Spectrometer Heritage Mechanical Design
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 35
Successful QWEST alignment technique to be reused for HyTES.
Alignment mechanism utilizes in a warm environment the spherical surface on both
Monolithic ZnSe block and grating
Spectrometer Alignment
Monolithic ZnSe Block Single scaffolding member shown for reference (to be removed once epoxy cures)
Diffraction grating
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Thermal
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Thermal system design
• HyTES flight design will use two identical CryoTel GTs – one cooling only the QWIP array at 40 K – one cooling the Dyson spectrometer, relay optics, and telescope at ~100 K,
and intercepting radiated and conducted parasitics to 40 K
• Heat rejection from cryocoolers via circulating-fluid chiller (as is being done on other JPL airborne instruments)
• HyTES will be designed for easy replacement of a cryocooler, should one fail during the instrument lifetime
– these are commercial, not long-life space, cryocoolers, as appropriate for an airborne developmental program
JPL - 2/24/2010
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 38
HyTES cryovacuum package • Mechanical components:
– mechanical cryocoolers (2) – vacuum enclosure – floating radiation shields (2) – thermal isolation struts – QWIP focal plane array with positioning assembly – spectrometer – telescope and relay optics
• Temperature requirements: – QWIP FPA <40 K for dark current supression – Spectrometer <100 K for background supression – Relay optics <250 K with stability restrictions – Telescope ~room temperature
• Chose to cool the optical instrument to 100 K – single mechanical assembly is highly desirable for
alignment – cold relay eliminates temperature variation concerns
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 39
Data Recording and Storage
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Vacuum Vessel
Flight PC Streams5 S/W
FPIE
61.5MBps
RAID Disk Array SAS/SATA 1000 GB (removable)
DVR Express CLSAS Camera Link (LVDS)
31.2576MHz
Ancillary Data Acquisition & Control
100 baseT
Aircraft Station
TBD
2 heaters Heater Control LS340
10 sensors
TBD
FPA
Operator
Spectrometer
Telescope
System Electronics - Data and Control
Cryocoolers (x2)
2 RS-232 4.8Kbps
~4 MHz
CMIGITS III GPS/IMU
RS-232 TBD Kbps
Time Mark 1 Hz/1us res
GPS Data & Time Mark Dist
RS-232 TBD Kbps
Cover Drive
Window Cover
open/closed
RS-232 TBD Kbps
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Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. 41
Data Products
• Raw data from FPA with interleaved GPS and engineering data (L0)
• Geo-located Radiance at sensor (L1) • Future derived products
– Surface Radiance – Surface Emissivity – Surface Temperature
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Radiometric Analysis of QWEST
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Dewar
Fore-Optics
Cavity Blackbody
Lab Test Procedure
• Cycle Blackbody Through Temperatures of 10, 25, and 30 °C
• Blackbody DN’s at 10 and 30 °C used to Calculate 2-Point Calibration Coefficients
• Calculate Radiance and Brightness Temperature for Blackbody at 25 °C
QWEST Lab Setup
43
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QWEST Temperature Linearity
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Lab Test Results 8 January 2008
• Brightness Temperature Within 1 °C of 25 °C (Black-body Set Point)
• Sensitivity (NEDT, Modeled as Standard Deviation) Better than 0.2 °C Between 8.0 – 8.6 µm
• Single-Layer QWIP Detector Array: Substantial Drop in Sensitivity for λ > 8.75 µm
QWEST NEdT of 8-9 um QWIP
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Lab Test Results Using 7.5-9.5µm portion
of 3-color QWIP
Noise equivalent temperature difference. The distribution is shown for all spectral channels irrespective of blackbody temperature measured. Measurements were made for a calibrated blackbody between 5C and 40C.
QWEST NEdT of 3-color QWIP
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QWEST Spectral Accuracy
Spatial Positions
Spec
tral C
hann
els
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Lab versus QWEST
Emissivity of a sample of Quartz measured in the lab.
Apparent emissivity of quartz as measured by QWEST in direct sunlight.
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Summary • The QWEST testbed has demonstrated the utility of QWIP
technology for Hyperspectral TIR measurements. – Two arrays have been tested, a single-color 7.5-9 µm device and a 3-
color 7.5-12 µm device
• HyTES implements the technology from QWEST in a cryo-cooled airborne instrument
– HyTES 1Kx1K FPA expected in June 2010 – Completed Optical and Mechanical/Thermal Design and reviews – Procured cryo-coolers, masks, wafers, vacuum chamber – Procurements of Dyson block and fore-optics complete
• Established key component performance with QWEST • Developed test and alignment procedures from QWEST