KEYWORDS: James Webb Space Telescope, Camera shutters, Space operations, Astronomical imaging, Space telescopes, Telescopes, Spectroscopy, Spectrographs, Staring arrays, Prototyping
We are developing a 2D programmable field masks for Mutli-Object Spectroscopy (MOS) in sparsely populated fields. The device is based on the microshutter array MEMS technology originally developed for JWST NIRSpec. A new fabrication process has been developed to actuate microshutter arrays electrostatically thus eliminating the need for the macroscopic mechanisms and improving the reliability and robustness of the device. The microshutters, made with silicon nitride membranes with a shutter pitch size of 100 μm x 200 μm, rotate on narrow torsion bars. The microshutters are actuated, latched, and addressed electrostatically by applying voltages to the electrodes on the microshutters and the adjacent walls of the array support grid. We have demonstrated the fabrication and operation of the pilot arrays and produced an integrated flight unit that was successfully used on the FORTIS (Far-UV Off Rowland-circle Telescope for Imaging and Spectroscopy) project for suborbital flight in 2019.
We are reporting on the development of the next generation 2D programmable field masks for the UV/visible multi-object spectroscopy. The devices have their legacy in the JWST microshutter NIRSpec magnetically actuated MEMS microshutters. A new fabrication process has been developed to actuate microshutter arrays electrostatically thus eliminating the need for the macroscopic mechanisms and improving the reliability and robustness of the device. The microshutters, made with silicon nitride membranes with a pixel size of 100 x 200 μm^2, rotate on torsion bars. The microshutters are actuated, latched, and addressed electrostatically by applying voltages on the electrodes the front and back sides of the microshutters. We have successfully fabricated and demonstrated actuation and addressing of these devices.
Microshuter arrays are programmable field selector masks for optical spectrocopy based on MEMS technology. The original device was developed as part of the NIRSpec (Near Infrared Spectrometer) instrument for JWST (Jame Webb Space Telescope. The devices were designed for: random access addressing of the individual pixels in large format (365x721 elements), high contrast optical blocking > 1e4 operate in UV and visible, long life time for the operation of 20,000 cycles or more.
We describe our efforts to build a Wide-Field Lyman alpha Geocoronal simulator (WFLaGs) for characterizing the end-to-end sensitivity of FORTIS (Far-UV Off Rowland-circle Telescope for Imaging and Spectroscopy) to scattered Lyman α emission from outside of the nominal (1/2 degree)2 field-of-view. WFLaGs is a 50 mm diameter F/1 aluminum parabolic collimator fed by a hollow cathode discharge lamp with a 80 mm clear MgF2 window housed in a vacuum skin. It creates emission over a 10 degree FOV. WFLaGS will allow us to validate and refine a recently developed scattered light model and verify our scatter light mitigation strategies, which will incorporate low scatter baffle materials, and possibly 3-d printed light traps, covering exposed scatter centers. We present measurements of scattering intensity of Lyman alpha as a function of angle with respect to the specular reflectance direction for several candidate baffle materials. Initial testing of WFLaGs will be described.
KEYWORDS: Camera shutters, James Webb Space Telescope, Space telescopes, Optical fabrication, Magnetism, Telescopes, Microelectromechanical systems, Silicon, Aerospace engineering, Astronomical imaging
Microshutter array (MSA) subsystems were developed at NASA Goddard Space Flight Center as multiobject selectors for the Near-Infrared Spectrograph (NIRSpec) instrument on the James Webb Space Telescope (JWST). The subsystem will enable NIRSpec to simultaneously obtain spectra from >100 targets, which, in turn, increases instrument efficiency 100-fold. This system represents one of the three major innovations on the JWST that is scheduled to be launched in 2018 as the successor to the Hubble Space Telescope. Featuring torsion hinges, light shields, magnetic actuation, and electrostatic latching and addressing, microshutters are designed for the selective transmission of light with high efficiency and contrast. Complete MSA assemblies consisting of 365×171 microshutters were successfully fabricated and tested, and passed a series of critical reviews for programmable 2-D addressing, life tests, and optical contrast tests. At the final stage of the JWST MSA fabrication, we began to develop the next generation microshutter arrays (NGMSA) for future telescopes. These telescopes will require a much larger field of view than JWSTs. We discussed strategies for fabrication of a proof-of-concept NGMSA that will be modular in design and electrostatically actuated. The details of NGMSA development will be discussed in a follow-up paper.
KEYWORDS: Digital image correlation, Sensors, Aluminum, Microelectromechanical systems, Silicon, Camera shutters, Cameras, Finite element methods, Data modeling, Semiconducting wafers
A custom micro-mechanical test system was constructed using off-the-shelf components to characterize the mechanical
properties of microshutters. Microshutters are rectangular microelectromechanical apertures which open and close about
a narrow torsion bar hinge. Displacement measurements were verified using both capacitive and digital image
correlation techniques. Repeatable experiments on Si3N4 cantilever beams verified that the test system operates consistently. Using beam theory, the modulus of elasticity of the low stress Si3N4 was approximately 150 GPa, though significant uncertainty exists for this measurement due primarily to imprecise knowledge of the cantilever thickness. Tests conducted on microshutter arrays concluded that reducing the Si3N4 thickness from 250 nm to 500 nm reduces the torsional stiffness by a factor of approximately four. This is in good agreement with analytical and finite element models of the microshutters.
The Johns Hopkins University sounding rocket group has completed the assembly and calibration of the Far-ultraviolet Off Rowland-circle Telescope for Imaging and Spectroscopy (FORTIS); a sounding rocket borne multi-object spectro-telescope designed to provide spectral coverage of up to 43 separate targets in the 900 - 1800 Angstrom bandpass over a 30′ x 30′ field-of-view. FORTIS is capable of selecting the far-UV brightest regions of the target area by utilizing an autonomous targeting system. Medium resolution (R ~ 400) spectra are recorded in redundant dual-order spectroscopic channels with ~40 cm2 of effective area at 1216 Å. The maiden launch of FORTIS occurred on May 10, 2013 out of the White Sands Missile Range, targeting the extended spiral galaxy M61 and nearby companion NGC 4301. We report on the final flight calibrations of the instrument, as well as the flight results.
The Johns Hopkins University sounding rocket group is entering the final fabrication phase of the Far-ultraviolet Off
Rowland-circle Telescope for Imaging and Spectroscopy (FORTIS); a sounding rocket borne multi-object spectro-telescope
designed to provide spectral coverage of 43 separate targets in the 900 - 1800 Angstrom bandpass over a 30' x 30' field-of-
view. Using "on-the-fly" target acquisition and spectral multiplexing enabled by a GSFC microshutter array, FORTIS
will be capable of observing the brightest regions in the far-UV of nearby low redshift (z ~ 0.002 - 0.02) star forming
galaxies to search for Lyman alpha escape, and to measure the local gas-to-dust ratio. A large area (~ 45 mm x 170 mm)
microchannel plate detector built by Sensor Sciences provides an imaging channel for targeting flanked by two redundant
spectral outrigger channels. The grating is ruled directly onto the secondary mirror to increase efficiency. In this paper, we
discuss the recent progress made in the development and fabrication of FORTIS, as well as the results of early calibration
and characterization of our hardware, including mirror/grating measurements, detector performance, and early operational
tests of the microshutter arrays.
The design of microelectromecanical systems (MEMS) and micro-opto-electromechanical systems (MOEMS) are often
materials-limited with respect to the efficiency and capability of the material. Graphene, a one atom thick honeycomb
lattice of carbon, is a highly desired material for MEMS applications. Relevant properties of graphene include the
material's optical transparency, mechanical strength, energy efficiency, and electrical and thermal conductivity due to its
electron mobility. Aforementioned properties make graphene a strong candidate to supplant existing transparent
electrode technology and replace the conventionally used material, indium-tin oxide. In this paper we present
preliminary results on work toward integration of graphene with MEMS structures.
We are studying mechanical exfoliation of highly ordered pyrolytic graphite (HOPG) crystals by repeatedly applying and
separating adhesive materials from the HOPG surface. The resulting graphene sheets are then transferred to silicon oxide
substrate using the previously applied adhesive material. We explored different adhesive options, particularly the use of
Kapton tape, to improve the yield of graphene isolation along with chemical cross-linking agents which operate on a
mechanism of photoinsertion of disassociated nitrene groups. These perfluorophenyl nitrenes participate in C=C addition
reactions with graphene monolayers creating a covalent binding between the substrate and graphene. We are focusing on
maximizing the size of isolated graphene sheets and comparing to conventional exfoliation. Preliminary results allow
isolation of few layer graphene (FLG) sheets (n<3) of approximately 10μm x 44μm. Photolithography could possibly be
utilized to tailor designs for microshutter technology to be used in future deep space telescopes.
The Johns Hopkins University sounding rocket group is building the Far-ultraviolet Off Rowland-circle Telescope for
Imaging and Spectroscopy (FORTIS), which is a Gregorian telescope with rulings on the secondary mirror. FORTIS will
be launched on a sounding rocket from White Sand Missile Range to study the relationship between Lyman alpha escape
and the local gas-to-dust ratio in star forming galaxies with non-zero redshifts. It is designed to acquire images of a 30'
x 30' field and provide fully redundant "on-the-fly" spectral acquisition of 43 separate targets in the field with a bandpass
of 900 - 1800 Angstroms. FORTIS is an enabling scientific and technical activity for future cutting edge far- and near-uv
survey missions seeking to: search for Lyman continuum radiation leaking from star forming galaxies, determine the
epoch of He II reionization and characterize baryon acoustic oscillations using the Lyman forest. In addition to the high
efficiency "two bounce" dual-order spectro-telescope design, FORTIS incorporates a number of innovative technologies
including: an image dissecting microshutter array developed by GSFC; a large area (~ 45 mm x 170 mm) microchannel
plate detector with central imaging and "outrigger" spectral channels provided by Sensor Sciences; and an autonomous
targeting microprocessor incorporating commercially available field programable gate arrays. We discuss progress to date
in developing our pathfinder instrument.
KEYWORDS: Camera shutters, James Webb Space Telescope, Space telescopes, Optical fabrication, Magnetism, Silicon, Telescopes, Aerospace engineering, Microelectromechanical systems, Indium
We have developed the Microshutter Array (MSA) system at NASA Goddard Space Flight Center (GSFC) as
a multi-object aperture array for the Near Infrared Spectrograph (NIRSpec) instrument on the James Webb
Space Telescope (JWST). The MSA system will enable NIRSpec to simultaneously obtain spectra from more
than 100 targets, which, in turn, increases instrument efficiency one-hundred fold. Consequently, this system
represents one of the three major innovations on the JWST, which has been selected by the National Research
Council's 2001 decadal survey as the top-ranked space-based mission and is scheduled to be the successor to
the Hubble Space Telescope. Furthermore, the MSA system will be one of the first MEMS devices serving
observation missions in space. Microshutters are designed for the selective transmission of light with high
efficiency and contrast and feature torsion hinges, light shields, deep-reactive ion-etched silicon windows,
magnetic actuation, and electrostatic latching and addressing. Complete MSA quadrant assemblies consisting
of 365 x 181 microshutters have been successfully fabricated. The assemblies have passed a series of critical
reviews, which include programmable 2-D addressing, life tests, optical contrast tests, and environmental
tests, required by the design specifications of JWST. Both the MSA and NIRSpec will be delivered to ESA
for final assembly, and JWST is scheduled to launch in 2014. During final assembly and testing of the MSA
system, we have begun to develop the Next Generation Microshutter Arrays (NGMSA) for future telescopes.
These telescopes will require a much larger field of view than JWST's, and we discuss strategies for
fabrication of a proof-of-concept NGMSA which will be modular in design and electrostatically actuated.
A carbon nanotube (CNT) field emission electron gun has been fabricated and assembled as an electron impact
ionization source for a miniaturized time-of-flight mass spectrometer (TOF-MS). The cathode consists of a patterned
array of CNT towers grown by catalyst-assisted thermal chemical vapor deposition. An extraction grid is precisely
integrated in close proximity to the emitter tips (20-35 μm spacing), and an anode is located at the output to monitor the
ionization beam current. Ultra-clean MEMS integration techniques were employed in an effort to achieve three
improvements, relative to previous embodiments: reduced extraction voltage during operation to be resonant with gas
ionization energies, enhanced current transmission through the grid, and a greater understanding of the fundamental
current fluctuations due to adsorbate-assisted tunneling. Performance of the CNT electron gun will be reported, and
implications for in situ mass spectrometry in planetary science will be discussed.
KEYWORDS: Galactic astronomy, Camera shutters, Stars, Sensors, Photons, Telescopes, Near ultraviolet, Ionization, Spectroscopy, James Webb Space Telescope
We explore the design of a space mission called Project Lyman that has the goal of quantifying the ionization history of the universe from the present epoch to a redshift of z ~ 3. Observations from WMAP and SDSS show that before a redshift of z (Symbol not available. See manuscript.) 6 the first collapsed objects, possibly dwarf galaxies, emitted Lyman continuum (LyC) radiation shortward of 912 Å that reionized most of the universe. Theoretical estimates of the LyC escape fraction ( fesc ) required from these objects to complete reionization is fesc ~10%. How LyC escapes from galactic environments, whether it induces positive or negative feedback on the local and global collapse of structures, and the role played by clumping, molecules, metallicity and dust are major unanswered theoretical questions, requiring observational constraint. Numerous intervening Lyman limit systems frustrate the detection of LyC from high z objects. They thin below z ~ 3 where there are reportedly a few cases of apparently very high fesc. At low z there are only controversial detections and a handful of upper limits. A wide-field multi-object spectroscopic survey with moderate spectral and spatial resolution can quantify fesc within diverse spatially resolved galactic environments over redshifts with significant evolution in galaxy assemblage and quasar activity. It can also calibrate LyC escape against Lyα escape, providing an essential tool to JWST for probing the beginnings of reionization. We present calculations showing the evolution of the characteristic apparent magnitude of star-forming galaxy luminosity functions at 900 Å, as a function of redshift and assumed escape fraction. These calculations allow us to determine the required aperture for detecting LyC and conduct trade studies to guide technology choices and balance science return against mission cost. Finally we review our efforts to build a pathfinding dual order multi-object spectro/telescope with a (0.5°)2 field-of-view, using a GSFC microshutter array, and crossed delay-line micro-channel plate detector.
The microshutter array (MSA) is a key component in the James Webb Space Telescope Near Infrared Spectrometer
(NIRSpec) instrument. The James Webb Space Telescope is the next generation of a space-borne astronomy platform
that is scheduled to be launched in 2013. However, in order to effectively operate the array and meet the severe
operational requirements associated with a space flight mission has placed enormous constraints on the microshutter
array subsystem. This paper will present an overview and description of the entire microshutter subsystem including the
microshutter array, the hybridized array assembly, the integrated CMOS electronics, mechanical mounting module and
the test methodology and performance of the fully assembled microshutter subsystem. The NIRSpec is a European
Space Agency (ESA) instrument requiring four fully assembled microshutter arrays, or quads, which are independently
addressed to allow for the imaging of selected celestial objects onto the two 4 mega pixel IR detectors. Each
microshutter array must have no more than ~8 shutters which are failed in the open mode (depending on how many are
failed closed) out of the 62,415 (365x171) total number of shutters per array. The driving science requirement is to be
able to select up to 100 objects at a time to be spectrally imaged at the focal plane. The spectrum is dispersed in the
direction of the 171 shutters so if there is an unwanted open shutter in that row the light from an object passing through
that failed open shutter will corrupt the spectrum from the intended object.
KEYWORDS: James Webb Space Telescope, Spectrographs, Electronics, Galactic astronomy, Near infrared, Astronomical imaging, Camera shutters, Silicon, Space telescopes, Imaging spectroscopy
One of the James Webb Space Telescope's (JWST) primary science goals is to characterize the epoch of galaxy formation in
the universe and observe the first galaxies and clusters of galaxies. This goal requires multi-band imaging and spectroscopic
data in the near infrared portion of the spectrum for large numbers of very faint galaxies. Because such objects are
sparse on the sky at the JWST resolution, a multi-object spectrograph is necessary to efficiently carry out the required
observations. We have developed a fully programmable array of microshutters that will be used as the field selector
for the multi-object Near Infrared Spectrograph (NIRSpec) on JWST. This device allows apertures to be opened at the
locations of selected galaxies in the field of view while blocking other unwanted light from the sky background and bright
sources. In practice, greater than 100 objects within the field of view can be observed simultaneously. This field selection
capability greatly improves the sensitivity and efficiency of NIRSpec. In this paper, we describe the microshutter arrays,
their development, characteristics, fabrication, testing, and progress toward delivery of a flight-qualified field selection
subsystem to the NIRSpec instrument team.
We have developed microshutter array systems at NASA Goddard Space Flight Center for use as multi-object
aperture arrays for a Near-Infrared Spectrometer (NIRSpec) instrument. The instrument will be carried on the
James Webb Space Telescope (JWST), the next generation of space telescope, after the Hubble Space
Telescope retires. The microshutter arrays (MSAs) are designed for the selective transmission of light from
objected galaxies in space with high efficiency and high contrast. Arrays are close-packed silicon nitride
membranes with a pixel size close to 100x200 μm. Individual shutters are patterned with a torsion flexure
permitting shutters to open 90 degrees with minimized stress concentration. In order to enhance optical
contrast, light shields are made on each shutter to prevent light leak. Shutters are actuated magnetically,
latched and addressed electrostatically. The shutter arrays are fabricated using MEMS bulk-micromachining
and packaged utilizing a novel single-sided indium flip-chip bonding technology. The MSA flight system
consists of a mosaic of 2 x 2 format of four fully addressable 365 x 171 arrays. The system will be placed in
the JWST optical path at the focal plane of NIRSpec detectors. MSAs that we fabricated passed a series of
qualification tests for flight capabilities. We are in the process of making final flight-qualified MSA systems
for the JWST mission.
KEYWORDS: Camera shutters, Electrodes, Magnetism, Indium, Silicon, James Webb Space Telescope, Optical fabrication, Metals, Microelectromechanical systems, Space telescopes
A complex MEMS device, microshutter array system, is being developed at NASA Goddard Space Flight
Center for use as an aperture array for a Near-Infrared Spectrometer (NirSpec). The instrument will be
carried on the James Webb Space Telescope (JWST), the next generation of space telescope after Hubble
Space Telescope retires. The microshutter arrays (MSAs) are designed for the selective transmission of light
with high efficiency and high contrast. Arrays are close-packed silicon nitride membranes with a pixel size
close to 100x200 &mgr;m. Individual shutters are patterned with a torsion flexure permitting shutters to open 90
degrees with a minimized mechanical stress concentration. Light shields are made on to each shutter for light
leak prevention so to enhance optical contrast. Shutters are actuated magnetically, latched and addressed
electrostatically. The shutter arrays are fabricated using MEMS bulk-micromachining technologies and
packaged using single-sided indium flip-chip bonding technology. The MSA flight concept consists of a
mosaic of 2 x 2 format of four fully addressable 365 x 171 arrays placed in the JWST optical path at the focal
plane.
KEYWORDS: Camera shutters, Electrodes, Indium, Magnetism, Silicon, James Webb Space Telescope, Optical fabrication, Metals, Microelectromechanical systems, Space telescopes
MEMS microshutter arrays (MSAs) are being developed at NASA Goddard Space Flight Center for use as an aperture
array for the Near-Infrared Spectrometer (NirSpec). The instruments will be carried on the James Webb Space
Telescope (JWST), the next generation of space telescope after Hubble Space Telescope retires. The microshutter arrays
are designed for the selective transmission of light with high efficiency and high contrast. Arrays are close-packed
silicon nitride membranes with a pixel size of 105x204 μm. Individual shutters are patterned with a torsion flexure
permitting shutters to open 90 degrees with a minimized mechanical stress concentration. Light shields are made on each
shutter for light leak prevention to enhance optical contrast. Shutters are actuated magnetically, latched and addressed
electrostatically. The shutter arrays are fabricated using MEMS technologies. Single-side indium flip chip bonding is
performed to attach microshutter arrays to substrates.
We report on methods to minimize thermally-induced deformation in a MEMS-based reconfigurable aperture. The device is an enabling component of the Near-Infrared Spectrometer, a principle instrument on NASA’s James Webb Space Telescope. The Microshutter Array consists of 384x175 individually addressable shutters which can be magnetically rotated 90° into the plane of the array and electrostatically latched open. Each shutter is a 100x200 μm rectangular membrane suspended by a small neck region and torsion flexure. The primary materials in the shutter are a 5000Å Si3N4 layer for mechanical rigidity, 2000Å Al for opacity and electrostatic latching, and 2200Å Co90Fe10 for magnetic actuation. This multi-layer stack presents a challenge due to the operating temperatures required for the device: both room temperature (300K) and cryogenic temperature (30K). Thermal expansion of the materials causes the shutters to bow out of plane excessively, which can prevent actuation of the shutters, cause damage to portions of the array, and allow light leakage around closed shutters. Here we present our investigation of several methods to prevent microshutter bowing including deposition of additional materials on the shutters to create a symmetrical layer stack and replacing the current stack with low-coefficient of thermal expansion materials. Using shutter-size suspended cantilever beams as a rapid-development test bed, we have reduced out-of-plane bowing between 300K and 30K to 10% or better. We are currently applying these results to microshutter arrays to develop shutters that remain flat from room temperature to cryogenic temperature while retaining the required mechanical, optical, and magnetic properties.
KEYWORDS: Camera shutters, Electrodes, Silicon, Metals, Magnetism, James Webb Space Telescope, Optical fabrication, Microelectromechanical systems, Semiconducting wafers, Reactive ion etching
Micro Electromechanical System (MEMS) microshutter arrays are being developed at NASA Goddard Space Flight Center for use as a field selector of the Near Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope (JWST). The microshutter arrays are designed for the spontaneous selection of a large number of objects in the sky and the transmission of light to the NIRSpec detector with high contrast. The JWST environment requires cryogenic operation at 35 K. Microshutter arrays are fabricated out of silicon-on-insulator (SOI) silicon wafers. Arrays are close-packed silicon nitride membranes with a pixel size of 100 x 200 μm. Individual shutters are patterned with a torsion flexure permitting shutters to open 90 degrees with a minimized mechanical stress concentration. Light shields are processed for blocking light from gaps between shutters and frames. The mechanical shutter arrays are fabricated using MEMS technologies. The processing includes multi-layer metal depositions, the patterning of magnetic stripes and shutter electrodes, a reactive ion etching (RIE) to form shutters out of the nitride membrane, an anisotropic back-etch for wafer thinning, followed by a deep RIE (DRIE) back-etch to form mechanical supporting grids and release shutters from the silicon substrate. An additional metal deposition is used to form back electrodes. Shutters are actuated by a magnetic force and latched using an electrostatic force. Optical tests, addressing tests, and life tests are conducted to evaluate the performance and the reliability of microshutter arrays.
KEYWORDS: Camera shutters, James Webb Space Telescope, Electrodes, Silicon, Spectrographs, Magnetism, Prototyping, Failure analysis, Near infrared, Galactic astronomy
The Near Infrared Spectrograph (NIRSpec) for the James Webb Space Telescope (JWST) is a multi-object spectrograph operating in the 0.6-5.0 μm spectral range. One of the primary scientific objectives of this instrument is to measure the number and density evolution of galaxies following the epoch of initial formation. NIRSpec is designed to allow simultaneous observation of a large number of sources, vastly increasing the capability of JWST to carry out its objectives. A critical element of the instrument is the programmable field selector, the Microshutter Array. The system consists of four 175 x 384 close packed arrays of individually operable shutters, each element subtending 0.2” x 0.4”on the sky. This device allows simultaneous selection of over 200 candidates for study over the 3.6’ x 3.6’ field of the NIRSpec, dramatically increasing its efficiency for a wide range of investigations. Here, we describe the development, production, and test of this critical element of the NIRSpec.
We present recent measurements obtained using a new method for characterizing transition edge sensor (TES) calorimeters: We measured the electrical impedance of a TES calorimeter throughout the superconducting to normal metal phase transition. The impedance method enables us to previously measure how the resistance and heat capacity of the TES varied throughout the phase transition. These measurements probe the internal state of oru Mo/Au TES. We also present recent results from measurements of noise in our TESs. Our measurements are instrumental toward understanding and optimizing our TES calorimeters.
We are developing a distributed-readout imaging spectrometer named Position-Sensitive Transition-Edge Sensor (PoST). A PoST is a microcalorimeter capagble of 1D imaging spectroscopy. It consists of two Transition-Edge Sensors (TESs) at each end of a long x-ray absorber. The position of an x-ray absorption event in the PoST is determined from the rise time and relative signal sizes in the two sensors. The energy of the absorbed photon is inferred from the sum of the two pulses. We discuss the modeling, operation, and readout of PoSTs and their application to the Constellation-X mission.
We are developing superconducting direct detectors for submillimeter astronomy that can in principle detect individual photons. These devices, Single Quasiparticle Photon Counter (SQPC), operate by measuring the quasiparticles generated when single Cooper-pairs are broken by absorption of a submillimeter photon. This photoconductive type of device could yield high quantum efficiency, large responsivity, microsecond response times, and sensitivities in the range of 10-20 Watts per root Hertz. The use of antenna coupling to a small absorber also suggests the potential for novel instrument designs and scalability to imaging or spectroscopic arrays. We will describe the device concept, recent results on fabrication and electrical characterization of these detectors, issues related to saturation and optimization of the device parameters. Finally, we have developed practical readout amplifiers for these high-impedance cryogenic detectors based on the Radio-Frequency Single-Electron Transistor (RF-SET). We will describe results of a demonstration of a transimpedance amplifier based on closed-loop operation of an RF-SET, and a demonstration of a wavelength-division multiplexing scheme for the RF-SET. These developments will be a key ingredient in scaling to large arrays of high-sensitivity detectors.
Magnetically actuated MEMS microshutter arrays are being developed at the NASA Goddard Space Flight Center for use in a multi-object spectrometer on the James Webb Space Telescope (JWST), formerly Next Generation Space Telescope (NGST). The microshutter arrays are designed for the selective transmission of light with high efficiency and high contrast. The JWST environment requires cryogenic operation at 45K. Microshutter arrays are fabricated out of silicon-on-insulator (SOI) wafers. Arrays consist of close-packed shutters made on silicon nitride (nitride) membranes with a pixel size of 100 × 100 m. Individual shutters are patterned with a torsion flexure permitting shutters to open 90°, with a minimized mechanical stress concentration. Shutters operated this way have survived fatigue life test. The mechanical shutter arrays are fabricated using MEMS technologies. The processing includes a multi-layer metal deposition, patterning of shutter electrodes and magnetic pads, reactive ion etching (RIE) of the front side to form shutters in a nitride film, an anisotropic back-etch for wafer thinning, and a deep RIE (DRIE) back-etch, down to the nitride shutter layer, to form support frames and relieve shutters from the silicon substrate. An additional metal deposition and patterning has recently been developed to form electrodes on the vertical walls of the frame. Shutters are actuated using a magnetic force, and latched electrostatically. One-dimensional addressing has been demonstrated.
KEYWORDS: Iron, Camera shutters, Silicon, Aluminum, James Webb Space Telescope, Sputter deposition, Spectroscopy, Magnetism, Space telescopes, Semiconducting wafers
The James Webb Space Telescope (JWST), formally Next Generation Space Telescope (NGST), is one of NASA’s challenging projects for advancing the exploration of space. The NGST will be equipped with a Multi-Object-Spectrometer (MOS) that covers the wavelength ranging from 0.6 to 5 micron. To selectively direct light rays from different regions of space into the spectrometer, one approach is to use microshutter arrays serving as the slit mask for the spectrometer. A large format (2Kx1K) individually addressable microshutter array with a lateral pixel size of 100μm x 200μm is being developed and fabricated using MEMS technologies. The microshutter arrays are close-packed silicon nitride membrane cantilevers. A ferromagnetic Co90Fe10 film is deposited on the membranes to magnetically actuate the microshutters. During deposition a Co90Fe10 film is susceptible to develop large tensile stress that can distort the nitride membranes and affect the contrast of the MOS, especially at cryogenic temperatures. In this paper, we discuss how to minimize the film stress. Stress-test cantilevers are micro machined and used in conjunction with Stoney’s formula to determine film stresses. The effects of deposition pressure and power on the Co90Fe10 film, aluminum film and multiple-layer film stress are discussed. It is found that sputter-deposition of Co90Fe10 at low pressure and power results in favor of low tensile stresses in films.
KEYWORDS: Camera shutters, Electrodes, Silicon, Semiconducting wafers, Magnetism, Oxides, Deep reactive ion etching, Etching, Reactive ion etching, Space telescopes
Two-dimensional microshutter arrays are being developed at NASA Goddard Space Flight Center (GSFC) for the Next Generation Space Telescope (NGST) for use in the near-infrared region. Functioning as focal plane object selection devices, the microshutter arrays are 2-D programmable masks with high efficiency and high contrast. The NGST environment requires cryogenic operation at 45 K. Arrays are close-packed silicon nitride membranes with a unit cell size of 100x100 micrometer. Individual shutters are patterned with a torsion flexure permitting shutters to open 90 degrees with minimized mechanical stress concentration. The mechanical shutter arrays are fabricated with MEMS technologies. The processing includes a RIE front-etch to form shutters out of the nitride membrane, an anisotropic back-etch for wafer thinning, and a deep RIE (DRIE) back-etch down to the nitride shutter membrane to form frames and to relieve the shutters from the silicon substrate. A layer of magnetic material is deposited onto each shutter. Onto the side-wall of the support structure a metal layer is deposited that acts as a vertical hold electrode. Shutters are rotated into the support structure by means of an external magnet that is swept across the shutter array for opening. Addressing is performed through a scheme using row and column address lines on each chip and external addressing electronics.
KEYWORDS: Camera shutters, Etching, Semiconducting wafers, Silicon, Deep reactive ion etching, Magnetism, Electrodes, Oxides, Space telescopes, Microelectromechanical systems
Two-dimensional microshutter arrays are being developed at NASA Goddard Space Flight Center for the Next Generation Space Telescope (NGST) for use in the near-infrared region. Functioning as object selection devices, the microshutter arrays are designed for the transmission of light with high efficiency and high contrast. The NGST environment requires cryogenic operation at 45K. Arrays are close-packed silicon nitride membranes with a pixel size of 100 X 100 micrometers . Individual shutters are patterned with a torsion flexure permitting shutters to open 90 degrees with a minimized mechanical stress concentration. The mechanical shutter arrays are fabricated with MEMS technologies. The processing includes a RIE front-etch to form shutters out of the nitride membrane, an anisotropic back-etch for wafer thinning, and a deep RIE (DRIE) back-etch down to the nitride shutter membrane to form frames and to relieve shutters from the silicon substrate. Two approaches for shutter actuation have been developed. Shutters are actuated using either a combined mechanical and electrostatic force or a combined magnetic and electrostatic force. A CMOS circuit embedded in the frame between shutters allows programmable shutter selection for the first approach. A control of row and column electrodes fulfills shutter selection for the second approach.
X-ray microcalorimeters using transition-edge sensors (TES) show great promise for use in astronomical x-ray spectroscopy. We have obtained very high energy resolution (2.8 eV at 1.5 keV and 3.7 eV at 3.3 keV) in a large, isolated TES pixel using a Mo/Au proximity-effect bilayer on a silicon nitride membrane. We will discuss the performance and our characterization of that device. In order to be truly suitable for use behind an x-ray telescope, however, such devices need to be arrayed with a pixel size and focal-plane coverage commensurate with the telescope focal length and spatial resolution. Since this requires fitting the TES and its thermal link, a critical component of each calorimeter pixel, into a far more compact geometry than has previously been investigated, we must study the fundamental scaling laws in pixel optimization. We have designed a photolithography mask that will allow us to probe the range in thermal conductance that can be obtained by perforating the nitride membrane in a narrow perimeter around the sensor. This mask will also show the effects of reducing the TES area. Though we have not yet tested devices of the compact designs, we will present our progress in several of the key processing steps and discuss the parameter space of our intended investigations.
In the X-ray astrophysics community, the desire for wide- field, high-resolution, X-ray imaging spectrometers has been growing for some time. We present a concept for such a detector called a Position-Sensing Transition-edge sensor (PoST). A PoST is a calorimeter consisting of two Transition- Edge Sensors (TESs) on the ends of a long absorber to do one dimensional imaging spectroscopy. Comparing the rise time and energy estimates obtained from each TES for a given event, the position of that event in the PoST is determined. Energy is inferred from the sum of the two signals on the TESs. We have designed 7, 15, and 32 pixel PoSTs using our Mo/Au TESs and bismuth absorbers. We discuss the theory, modeling, operation and readout of PoSTs and the latest results from our development.
KEYWORDS: Camera shutters, Silicon, Semiconducting wafers, Etching, Ions, Deep reactive ion etching, Reactive ion etching, Micromirrors, Astronomical imaging, Spectroscopy
We are developing a lithography process for a 2D array of microshutters which can be used as a high efficiency, high contrast field selection device for a multi-objects spectrometer for the Next Generation Space Telescope. The device is a close- packed array of shutters with an individual shutter size of 100 micrometers square and area filling factor of about 80 percent, produced in a 100 micrometers thick silicon wafer. Our current array size is 128 by 128. Ech shutter made of silicon nitride with an appropriate optical coating, pivots on a torsion flexure along one edge. A CMOS circuit embedded in the frame around the shutters allows individual selection. An original double-shutter mechanism is employed for actuation. Processing includes anisotropic back etching for wafer thinning, a DRIE back etch through the silicon to the mechanical active nitride membrane and a RIE to produce the shutters out of the nitride membrane. Our layout is based on a detailed mechanical analysis for which we determined crucial material parameters experimentally.
COnstellation-X is a cluster of identical observatories that together constitute a promising concept for a next- generation, high-throughput, high-resolution, astrophysical x-ray spectroscopy mission. The heart of the Constellation-X mission concept is a high-quantum-efficiency imaging spectrometer with 2 eV resolution at 6 keV. Collectively across the cluster, this imaging spectrometer will have twenty times the collecting efficiency of XRS on Astro-E and better than 0.25 arc minute imaging resolution. The spectrometer on each satellite will be able to handle count rates of up to 1000 counts per second per imaging pixel for a point source and 30 counts per second per pixel for an extended source filling the array. Focal plane coverage of at least 2.5 arc minutes X arc minutes, comparable to XRS but with a factor of thirty more pixels, is required. This paper will present the technologies that have the potential to meet al these requirements. It will identify the ones chosen for development for Constellation-X and explain why those were considered closer to realization, and it will summarize the results of the development work thus far.
We are developing novel photodetector arrays based on superconducting transition-edge sensor (TES) and pop-up detector (PUD) technologies. The TES has the potential for a new generation of high sensitivity photodetectors from the IR to the x-ray. This is directly due to the sharpness of the resistance change with temperature at the superconducting transition. The TESs are deposited on the PUD arrays and serve as the sensing elements. The PUDs are close-packed, folded membrane arrays that provide the TES substrate and the thermal isolation required by the bolometers and microcalorimeters. This paper presents the processing-related characterization result of preliminary TES and PUD designs. The gaol of this work is to fabricate a new generation of x-ray calorimeters and IR bolometers for space flight projects.
High sensitivity is a basic requirement for a new generation of thermal detectors. To meet the requirement, close-packed, 2D silicon detector arrays have been developed in NASA Goddard Space Flight Center. The goal of the task is to fabricate detector arrays configured with thermal detectors such as IR bolometers and x-ray calorimeters to use in space flight missions. This paper focuses on the fabrication and the mechanical testing of detector arrays in a 0.2 mm pixel size, the smallest pop-up detectors being developed so far. These array structures, nicknamed 'PUDs' for 'Pop-Up Detectors', are fabricated on 1 micrometers thick, single-crystal, silicon membranes. Their designs have been refined so we can utilize the flexibility of thin silicon films by actually folding the silicon membranes to 90 degrees in order to obtain close-packed 2D arrays. The PUD elements consist of a detector platform and two legs for mechanical support while also serving as electrical and thermal paths. Torsion bars and cantilevers connecting the detector platform to the legs provide additional flexures for strain relief. Using micro- electromechanical structure fabrication techniques, including photolithography, anisotropic chemical etching, reactive-ion etching, and laser dicing, we have fabricated PUD detector arrays of fourteen designs with a variation of four parameters including cantilever length, torsion bar length and width, and leg length. Folding test were conducted to test mechanical stress distribution for the array structures. We obtained folding yields and selected optimum design parameters to reach minimal stress levels. Computer simulation was also employed to verify mechanical behaviors of PUDs in the folding process. In addition, scanning electron microscopy was utilized to examine the flatness of detectors and the alignment of detector pixels in arrays. The fabrication of thermistor and heaters on the pop-up detectors is under way, preparing us for the next step of the experiment, the thermal test.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.