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Cosmic Origins (COR)Strategic Technology

Development Portfolio

December 2014

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Current COR Technology Development Portfolio

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Key Collaborators:• Prof. Gary Varner, U. Hawaii• Dr. Oswald Siegmund, U.C. Berkeley

Applications:• High performance UV(1-300nm) detector for astrophysics, planetary,

solar, heliospheric, or aeronomy missions• Particle or time of flight detector for space physics missions• Fluorescense lifetime imaging (FLIM) for biology• Neutron radiography/tomography for material science

Cross Strip MCP Detector Systems for Spaceflight

Approach:• We will develop the ASIC in stages, by designing the four major

subsystems (amplifier, GHz analog sampler, ADC and output multiplexor) using sophisticated simulation tools for CMOS processes. Small test runs of the more intricate and untested designs can be performed through shared access of CMOS foundry services to mitigate risk. We plan 2 runs of the full up GRAPH design (CSA preamp and "HalfGRAPH"). In parallel, we will design and construct an FPGA readout circuit for the ASIC as well as a 50mm XS MCP detector that can be qualified for flight use.

PI: John Vallerga/U.C. Berkeley

Recent Accomplishments: • 50 mm detector design and fabrication complete• Confirmed detector performance with PXS electronics• Designed, fabricated and tested first half-GRAPH1 ASIC • Design and fabrication of FPGA board( Jan. 2015)• Design and fab of second version of both ASICs (Dec 2014)• Successful thermal test of detector (-30ºC to +55ºC) Aug. 2014

Significance of Work:• A new ASIC with amplifiers a factor of 5 faster yet with similar

noise characteristics as existing amplifier ASIC• GHz analog sampling and a low power ADC per channel• FPGA control of ASIC chip(s)

TRLin = 4 TRLcurrent = 4 TRLtarget = 6

Objectives and Key Challenges:• Cross strip (XS) MCP photon counting UV detectors have

achieved high spatial resolution (12µm) at low gain (500k) and high input flux (MHz) using laboratory electronics and decades old ASICs. We plan to develop new ASICs (“GRAPH”) that improve this performance, which includes amps and ADCs in a small volume, mass and power package crucial for spaceflight and demonstrates its performance to TRL 6.

Existing 19” rack mounted XS electronics

Two small, low mass, low power ASIC and FPGA boards qualified for flight

Current Funded Period of Performance:• May 1, 2012 – Feb 29, 2016

Next Milestones: • Successful thermal test of detector (-30ºC to +55ºC) Aug. 2014• Vibration test of detector (14.1 grms) Dec. 2014• Environmental tests of Detector + ASICs (Spring 2015)

Description and Objectives:

Approach:

Collaborators:

Accomplishments:

• Development of high reflectivity coatings to increase system throughput, particularly in the far-UV (FUV) spectral range

• Study other dielectric fluoride coatings and other deposition technologies such as Ion Beam Sputtering (IBS) that is expected to produce the nearest to ideal morphology optical thin film coatings and thus low scatter.

• Javier del Hoyo, Steve Rice and Felix Threat (551)• Jeff Kruk and Charles Bowers (665)

• Application of these enhanced mirror coating technology will enable FUV missions to investigate the formation and history of planets, stars, galaxies and cosmic structure, and how the elements of life in the Universe arose.

Enhanced MgF2 and LiF Over-coated Al Mirrors for FUV Space Astronomy

• Retrofit a 2 meter coating chamber with heaters/thermal shroud to perform Physical Vapor Depositions at high temperatures (200-300 C) to further improve performance of Al mirrors protected with either MgF2 or LiF overcoats.

• Optimize deposition process of lanthanide trifluorides as high-index materials that when paired with either MgF2 or LiF will enhance reflectance of Al mirrors at Lyman-alpha.

• Establish the IBS coating process to optimize deposition of MgF2 and LiF with extremely low absorptions at FUV wavelengths.

Applications:

PI: Manuel A. Quijada/Code 551

• Performed end-to-end testing of the 3-step Physical Vapor Deposition (PVD) coating process in 2 meter chamber to enable 1+meter class mirrors with either Al+MgF2 or Al+LiF coatings for FUV applications

• Completed characterization of lanthanide trifluorides (GdF3 and LuF3) to pair them with low-index MgF2 layers to produce narrow-bands dielectric reflectors at FUV wavelengths

• Production of mirrors with reflectance over 90% in FUV for ICON and GOLD projects.

Key challenge/Innovation:• Achieving high reflectivity (> 90-95%) in the 90 to 250 nm range• Scaling up coatings to large diameter (1+meter) mirror substrates

TRLin = 3 TRLout = 4Development Period:

Oct. 1, 2011 – Sept. 30, 2014

Various test runs to produce coatings with over 90% reflectance for ICON optics in FUV

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Ultraviolet Coatings, Materials and Processes for Advanced Telescope Optics

PI: Bala K. Balasubramanian/JPL

TRLin = 3 TRLcurrent est. by PI = 3 TRLtarget = 5

Objectives and Key Challenges:• “Development of UV coatings with high reflectivity (>90-95%),

high uniformity (<1-0.1%), and wide bandpasses (~100 nm to 300-1000 nm)” is a major technical challenge as much as it is a key requirement for cosmic origins program and for exoplanet exploration program. This project aims to address this key challenge and develop feasible technical solutions.

Significance of Work:• Materials and process technology are the main challenges.

Improvements in existing technology base and significant innovations in coating technology such as Atomic Layer Deposition will be developed.

Approach:• A set of experimental data are being developed with MgF2, AlF3

and LiF protected Al mirrors in the wavelength range 100 to 1000 nm for a comprehensive base of measured data to enable full scale developments with chosen materials and processes.

• Enhanced coating processes including Atomic Layer Deposition (ALD) will be studied.

Key Collaborators:• Stuart Shaklan (JPL), Nasrat Raouf (JPL), Shouleh Nikzad (JPL),

John Hennessy (JPL)• Manuel Quijada (GSFC) • Paul Scowen (ASU), James Green (Univ of Colo)

Current Funded Period of Performance:• Jan 2013 – Dec 2015

Recent Accomplishments: A coating chamber has been upgraded with sources, temperature

controllers and other monitors to produce coatings of various materials. Measurement tools are also established now at JPL and at GSFC.

Initial samples of protected Al with LiF and AlF3 have been produced and measured with encouraging results for further improvements

ALD coating process tools and process for MgF2 and AlF3 have been developed at JPL and are being optimized

Next Milestones:• Reach ~ 90% reflectivity in the 100 to 200nm band (2015) • Produce & test mirror coupons representing a meter-class mirror (2015)

Application:• The technology to enable future astrophysics and exoplanet missions

that aim to capture key spectral features from far UV to near infra red.• ATLAST, EXEP Missions

ALD chamber at JPL 1.2m coating chamber at Zecoat Corp

Balasubramanian / JPL

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Objectives and Key Challenges:• Half of the electromagnetic energy emitted since the big bang lies in

the far-IR. Large-format far-IR imaging arrays are needed to study galaxy formation and evolution, and star formation in our galaxy and nearby galaxies. Polarization-sensitive arrays can provide critical information on the role of magnetic fields.

• We will develop and demonstrate far-IR arrays for these applications

Application:• SOFIA instruments• Balloon payloads• Future space mission, e.g., SAFIR/CALISTO• Ground-based telescopes• Cameras and spectrometers (low NEP lab demo)• Potential impact on mm-wave CMB instrumentation

Kinetic Inductance Detector Arrays for Far-IR Astrophysics

Approach:• Raise the TRL of these detectors so investigators may confidently

propose them for a variety of instruments:o Ground telescope demo, 350 mm, 3 x 10-16 W Hz-1/2

o Lab demo for SOFIA, 90 mm, 1.7 x 10-16 W Hz-1/2

o Lab demo for balloon, 350 mm, 7 x 10-17 W Hz-1/2

o Lab demo for space, 90 mm, 5 x 10-19 W Hz-1/2

PI: Jonas Zmuidzinas/Caltech

Recent Accomplishments: Successful 350 mm telescope demo at the Caltech

Submillimeter Observatory (image above) Photon-noise-limited 350 mm lens-coupled arrays Operation of detector in dark w/ NEP≈2x10-19 WHz-1/2

Significance of Work:• Far-IR arrays are in high demand but are difficult to fabricate, and

therefore expensive and in short supply. Our solution is to use titanium nitride (TiN) and aluminum absorber-coupled, frequency-multiplexed kinetic inductance detectors.

Current Funded Period of Performance:• March 2013 – February 2016

Demo at CSO:350 mm image of Sgr B2

TRL In = 3 TRL PI-Asserted = 3, 6 TRL Target= 4-6

Key Collaborators:• Goutam Chattopadhyay, Peter Day, Darren Dowell, Rick Leduc (JPL)• Pradeep Bhupathi, Matt Holllister, Attila Kovacs, Chris

McKenney(Caltech)

Next Milestones:• First optical tests of space-sensitivity arrays (Jan 2015)

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Key Collaborators:• Chris Martin, Caltech, David Schiminovich, Columbia

University, Paul Scowen, Arizona State University, Michael Hoenk, JPL

High Efficiency Detectors in Photon Countingand Large FPAs

Application:• Large aperture UV/Optical Telescope, Explorers,

Spectroscopy missions, UV/Optical imaging

PI: Shouleh Nikzad/JPL

TRLin = 4 TRLcurrent = 4 TRLtarget = 5-6

Approach: • Develop and produce 2 megapixel AR-coated, delta doped

electron multiplied CCDs (EMCCDs) using JPL’s 8-inch capacity silicon molecular beam epitaxy (MBE) for delta doping and atomic layer deposition (ALD) for AR coating. Perform relevant environment testing, perform system-level evaluation on sky to validate performance over a wide range of signal level.

Objectives and Key Challenges:• High efficiency, high stability imaging arrays that affordable and

stable are an efficient and cost effective way to populate UV/Optical focal planes for spectroscopic missions and 4m+ UV/O telescope as stated in the NWNH 2009

Significance of Work:• Atomic-level control of back illuminated detector surface and

detector/AR coating interface produces high efficiency detectors with stable response and unique performance advantages even in the challenging UV and FUV spectral range

Current Funded Period of Performance:• Jan 2013 – Dec 2015

Recent Accomplishments:• Demonstrated 2 megapixel arrays with high QE (reflection limited)• Demonstrated 2 Mpixel arrays with high external QE (focused on

FIREBall and broadband) • Characterize & Validate the performance (iterative, first in FY14Q1) • Total Dose Radiation • Further evaluate performance (FY14Q2, FY15Q4)

Next Milestones:• On-sky observation (FY15 Q4)• Evaluate performance in astrophysics-relevant and mission-relevant

environments. (FY15Q3, FY15) – FIREBall flight

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Objectives and Key Challenges:• Heterodyne technology is necessary to answer fundamental

questions such as how do stars form? How do circumstellar disks evolve and form planetary systems? What controls the mass-energy-chemical cycles within galaxies?

• We will develop a 16-pixel heterodyne receiver system to cover both the C+ and the O+ lines.

Key Collaborators:• Paul Goldsmith (Science Lead), Jon Kawamura, Jose Siles,

Choonsup Lee, Goutam Chattopadhyay (all JPL); Frank Chang (UCLA), Sander Weinreb (Caltech)

Application:• Heterodyne array receivers for future suborbital and space

missions• Array receivers for CCAT submillimeter telescope

A Far-Infrared Heterodyne Array Receiver for C+ and OI Mapping

Approach:• Utilize JPL developed membrane diode process to construct

tunable sources in the 1.9-2.06 THz range• Utilize novel waveguide based active device power combining

schemes to enhance power at these frequencies• Design and build compact silicon micromachined based housing

for HEB mixer chips• Utilize CMOS technology for backends/synthesizer• Characterize and test multi-pixel receivers to validate stability

and field performance

PI: Dr. Imran Mehdi/JPL

Recent Accomplishments:• System design (completed)

16-pixel 1.9 THz all solid-state LO source

Significance of Work:• Lack of solid-state sources in the THz range is perhaps the single

most important challenge towards implementing array receivers• Low power backend spectrometers• Multi-pixel receiver characterization and calibration protocols

TRLin = 3 TRLcurrent = 4 TRLtarget = 5

1.9 THz diode

Current Funded Period of Performance:• Jan 2014-Dec 2016

Next Milestones:• 4-pixel LO chain with 70-76 GHz amplifiers (Sept 2015)• 4-pixel Mixer block (Sept 2015)• Back end spectrometer (Dec 2015)• 16-pixel LO chain (May 2016)• 16-pixel receiver (Dec 2016)

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Objectives and Key Challenges:• Mature the TRL of key technology challenges for the primary

mirror of future large-aperture Cosmic Origin UVOIR space telescopes

• Include monolithic and segmented optics design paths• Conduct prototype development, testing and modeling• Trace metrics to science mission error budget

Key Collaborators:• Dr. Scott Smith, Ron Eng, Mike Effinger/ NASA MSFC• Bill Arnold/Defense Acquisition Inc., Gary Mosier/GSFC• Dr. Marc Postman/STScI, Laura Abplanalp, Gary Matthews, Rob

Egerman/Exelis

Application:• Flagship optical missions• Explorer type optical missions• Department of Defense and commercial observations

Advanced Mirror Technology Development

Approach:• Provide guidance & risk reduction for science community to

make an informed decision for the 2020 Decadal.• Advance key technology required to enable 4 different

implementation paths.• Develop science and engineering requirements for traceable

mirror systems and determine their associated mass. Then select a launch system or down-size the mirror systems and science requirements.

PI: Phil Stahl/MSFC

Significance of Work:• Deep core concept design traceable to 4m mirror• 4m to 8m mirror and support structure point design that would

meet launch vehicle and science requirements

TRLin = varies from TRL3 to TRL5.5 pending technologyTRLcurrent = varies from TRL3 to TRL5.5 pending technologyTRLtarget = half step increase

Current Funded Period of Performance:• Sept 2011 – Sept 2016

Recent Accomplishments:• Generated preliminary 4m point design• Presented 9 presentations at Tech Days conference• Continued to expand Mirror Modeling code functionality • Assessed TRL using the TRL Calculator

Actuator Designed, Fabricated

and Tested at Exelis

Next Milestones:• Award Exelis Phase 2 contract/December 2014• Complete MOR pathfinder specimen fabrication & test• Complete 1.5m mirror design

Development of Digital Micro-Mirror Device Arrays for Use in Future Space Missions

PI: Zoran Ninkov/Rochester Institute of Technology

Objectives and Key Challenges :• There is a need for a technology to allow for selection of targets

in a field of view that can be input to an imaging spectrometer for use in remote sensing and astronomy.

• We are looking to modify and develop Digital Micromirror Devices (DMD) for this application.

Significance of Work :• Existing DMDs need to have the commercial windows replaced

with appropriate windows for the scientific application desired.

Approach:• Use available 0.7 XGA DMD devices to develop window removal

procedures and then replace delivered window with a hermetically sealed UV transmissive one of Magnesium Fluoride and HEM Sapphire one. Test and evaluate such devices and also Cinema DMDs.

Key Collaborators:• Sally Heap, Manuel Quijada (NASA/GSFC)• Massimo Robberto (STScI)• Alan Raisanen (RIT)

Current Funded Period of Performance:• May 2014 – May 2016

Recent Accomplishments:• 0.7 XGA DMDs ordered and delivered (Dec 2014)• MgF2 and HEM Sapphire windows ordered (Aug 2014)• DMD de-lidded at RIT sent to GSFC for characterizationNext Milestones• UV-test XGA DMD at GSFC (March 2015)• Re-windowed DMDs from L-1 Technology (May 2015)• Cinema DMD and electronics delivery (July 2015)Application:• Can be used in any hyper-spectral imaging mission.• Galaxy Evolution Spectroscopic Explorer

TRL In = 4 TRL Current = 4 TRL Target= 5

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DMD

DMD with one mirror segment removed showing driver

Close-up of mirror segment driver

DMD with all mirror segments removed