Details of a multispectral imaging radiometer specially designed to retrieve fire characteristics from a nanosatellite platform are presented. The instrument consists of an assembly of three cameras providing co-registered midwave infrared, longwave infrared, and visible image data. Preliminary evaluation of the instrument budgets showed approximately a mass of 12 kg, an envelope of 220×240×200 mm3, and an average power consumption of 13 W. A method was devised to stagger two linear arrays of 512×3 VOx microbolometers in each infrared detector assembly. Investigation of the first completed detector assemblies showed an alignment accuracy better than 10% of pixel pitch and a response uniformity achieved across 92% of the pixels. Effects of the thermal environment seen by the pixels were evaluated to optimize the radiometric packaging design. It was found that the resulting thermal stability of the arrays, combined with the available electronic dynamic range, allows acquisition of targets with temperatures as high as 750 K with the desired accuracy and without saturation. The detector assemblies were able to withstand extreme environments with vibration up to 14 grms and temperatures from 218 to 333 K. Exposing the assembly’s window and bandpass filter to proton and Co-60 gamma radiation with successive dose of 10 krad and 100 Gy resulted in no adverse effect on their transmittance characteristics. Performance characteristics of the assembled midwave and longwave infrared telescopes were consistent with modeling predictions. Results of the point spread function measurement supported the conclusion that the lenses alignment had been achieved within mechanical tolerances for both telescopes.
INO has a wide experience in the design and fabrication of different kinds of microbolometer focal plane arrays (FPAs). In particular, a 512x3 pixel microbolometer FPA has been selected as the sensor for the New Infrared Sensor Technology (NIRST) instrument, one of the payloads of the SACD/Aquarius mission. In order to make the absolute temperature measurements necessary for many infrared Earth observation applications, the microbolometer FPA must be integrated into a package offering a very stable thermal environment. The radiometric packaging technology developed at INO presents an innovative approach since it was conceived to be modular and adaptable for the packaging of different microbolometer FPAs and for different sets of assembly requirements without need for requalification of the assembly process. The development of the radiometric packaging technology has broadened the position of INO as a supplier of radiometric detector modules integrating FPAs of microbolometers inside a radiometric package capable of achieving the requirements of different space missions. This paper gives an overview of the design of INO’s radiometric package. Key performance parameters are also discussed and the test campaign conducted with the radiometric package is presented.
In a typical optical system, optical elements usually need to be precisely positioned and aligned to perform the correct optical function. This positioning and alignment involves securing the optical element in a holder or mount. Proper centering of an optical element with respect to the holder is a delicate operation that generally requires tight manufacturing tolerances or active alignment, resulting in costly optical assemblies. To optimize optical performance and minimize manufacturing cost, there is a need for a lens mounting method that could relax manufacturing tolerance, reduce assembly time and provide high centering accuracy. This paper presents a patent pending lens mounting method developed at INO that can be compared to the drop-in technique for its simplicity while providing the level of accuracy close to that achievable with techniques using a centering machine (usually < 5 μm). This innovative auto-centering method is based on the use of geometrical relationship between the lens diameter, the lens radius of curvature and the thread angle of the retaining ring. The autocentering principle and centering test results performed on real optical assemblies are presented. In addition to the low assembly time, high centering accuracy, and environmental robustness, the INO auto-centering method has the advantage of relaxing lens and barrel bore diameter tolerances as well as lens wedge tolerances. The use of this novel lens mounting method significantly reduces manufacturing and assembly costs for high performance optical systems. Large volume productions would especially benefit from this advancement in precision lens mounting, potentially providing a drastic cost reduction.
Threaded rings are used to fix lenses in a large portion of opto-mechanical assemblies. This is the case for the low cost drop-in approach in which the lenses are dropped into cavities cut into a barrel and clamped with threaded rings. The walls of a cavity are generally used to constrain the lateral and axial position of the lens within the cavity. In general, the drop-in approach is low cost but imposes fundamental limitations especially on the optical performances. On the other hand, active alignment methods provide a high level of centering accuracy but increase the cost of the optical assembly.
This paper first presents a review of the most common lens mounting techniques used to secure and center lenses in optical systems. Advantages and disadvantages of each mounting technique are discussed in terms of precision and cost. Then, the different contributors which affect the centering of a lens when using the drop-in approach, such as the threaded ring, friction, and manufacturing errors, are detailed. Finally, a patent pending lens mounting technique developed at INO that alleviates the drawbacks of the drop-in and the active alignment approaches is introduced. This innovative auto-centering method requires a very low assembly time, does not need tight manufacturing tolerances and offers a very high level of centering accuracy, usually less than 5 μm. Centering test results performed on real optical assemblies are also presented.
The new high precision polarimeter for the “Observatoire du Mont Mégantic” (POMM) is an instrument designed to
observe exoplanets and other targets in the visible and near infrared wavebands. The requirements to achieve these
observation goals are posing unusual challenges to structural and mechanical designers.
In this paper, the detailed design, analysis and laboratory results of the key mechanical structure and sub-systems are
presented.
First, to study extremely low polarization, the birefringence effect due to stresses in the optical elements must be kept to
the lowest possible values. The double-wedge Wollaston custom prism assembly that splits the incoming optical beam is
made of bonded α-BBO to N-BK-7 glass lenses. Because of the large mismatch of coefficients of thermal expansion and
temperatures as low as -40°C that can be encountered at Mont-Mégantic observatory, a finite element analysis (FEA)
model is developed to find the best adhesive system to minimize stresses.
Another critical aspect discussed in details is the implementation of the cascaded rotating elements and the twin rotating
stages. Special attention is given to the drive mechanism and encoding technology. The objective was to reach high
absolute positional accuracy in rotation without any mechanical backlash.
As for many other instruments, mass, size and dimensional stability are important critera for the supporting structure.
For a cantilevered device, such as POMM, a static hexapod is an attractive solution because of the high stiffness to
weight ratio. However, the mechanical analysis revealed that the specific geometry of the dual channel optical layout
also added an off-axis counterbalancing problem. To reach an X-Y displacement error on the detector smaller than 35μm
for 0-45° zenith angle, further structural optimization was done using FEA. An imaging camera was placed at the
detector plane during assembly to measure the actual optical beam shift under varying gravitational loading.
A polarimeter, to observe exoplanets in the visible and infrared, was built for the “Observatoire du Mont Mégantic”
(OMM) to replace an existing instrument and reach 10-6 precision, a factor 100 improvement. The optical and
mechanical designs are presented, with techniques used to precisely align the optical components and rotation axes to
achieve the targeted precision. A photo-elastic modulator (PEM) and a lock-in amplifier are used to measure the
polarization. The typical signal is a high DC superimposed to a very faint sinusoidal oscillation. Custom electronics
was developed to measure the AC and DC amplitudes, and characterization results are presented.
INO has designed, assembled and tested the Raven Multi-Object Adaptive Optics demonstrator calibration unit. This
sub-system consists in a telescope simulator that will allow aligning Raven's components during its integration, testing
its Adaptive Optics performances in the laboratory and at the telescope, and calibrating the Adaptive Optics system by
building the interaction matrix and measuring the non-common path aberrations. The system is presented with the
challenges that needed to be overcome during the design and integration phases. The system test results are also
presented and compared to the model predictions.
The Laser Tomographic Adaptive Optics system for Giant Magellan Telescope (GMT) uses a single conjugated
deformable mirror, the segmented Adaptive Secondary Mirror (ASM), to correct atmospheric wavefront aberrations with
the help of a constellation of six laser beacons equally spaced on the sky. We will present different approaches for the
design of the Laser Guide Star (LGS) Wave Front Sensor (WFS) system for GMT to cover all sodium emission altitudes
and telescope elevations, from 80 km to 200 km range and how the preliminary design was derived from these
approaches. The designed LGS WFS system includes a defocus-compensation mechanism working with a simple
zooming optics to achieve the pupil image with constant pupil size, nearly constant wavefront correction, as well as pupil
distortion correction. Either a trombone-mirror structure or a direct LGS-WFS translation is used for the defocus
compensation, when conjugating the LGS altitudes in the sky. In the designs, a zooming collimator images the ASM in
the GMT at the exit pupil of the LGS WFS system, where the designed lenslet-array is tailored for the selected CCD
format for the required plate scale on the sky. Additionally, we have proposed a novel and simple solution for pupilimage
segmentation when working with smaller CCD arrays. This novel solution consists of a single multi-aperture
blaze grating for pupil segmentation in the system.
KEYWORDS: Sensors, Staring arrays, Gold, Aluminum, Simulation of CCA and DLA aggregates, Indium oxide, Readout integrated circuits, Ultrasonics, Interfaces, Epoxies
The Broadband Radiometer (BBR) is an instrument being developed for the ESA EarthCARE satellite. The BBR
instrument is led by SEA in the UK with RAL responsible for the BBR optics unit (OU) while EADS Astrium is the
EarthCARE prime contractor. The BBR detectors consist of three dedicated assemblies under the responsibility of INO.
The detectors development started in 2008 and led to the design and implementation of a new gold black deposition
facility at INO, in parallel with the preliminary and detailed design phases of the detector assemblies. As of today, two
breadboard models and one engineering model have been delivered to RAL. The engineering qualification model
manufacturing activities are on-going. This paper first provides an overview of the detectors assembly and principles of
operation, with emphasis given to processes developed for the assembly and integration of the detectors. Detector-level
qualification planning is finally discussed.
Representative failure data for structural epoxies can be very difficult to find for the optomechanical engineer. Usually,
test data is only available for shear configuration at room temperature and fast pull rate. On the other hand, the slowly
induced stress at extreme temperature is for many optical systems the worse-case scenario. Since one of the most
referenced epoxy for optical assembly is the 3M™ Scotch-Weld™ Epoxy Adhesive EC-2216 B/A Gray, better
understanding its behavior can benefit a broad range of applications.
The objective of this paper is two-fold. First, review data for critical parameters such as Young's modulus and
coefficient of thermal expansion. Secondly, derive failure criteria from correlation between a thermal stress experiment
and a finite element model.
Instead of pulling out a standard tensile specimen, it is proposed to test thin bondline geometry to replicate an optical
device usage. Four test plates are assembled at the Institut National d'Optique (INO) in Quebec City, Canada with
bondlines of 50 μm and 133 μm. To detect the failure of the epoxy, the low level vibration signature of a cantilever Invar
plate is monitored as temperature changes. Following the finite element analysis, a failure criterion is found to better
match the experimental results than generic lap shear data.
Uncooled microbolometer detectors are well suited for space applications due to their low power consumption while still exhibiting adequate performance. Furthermore, the spectral range of their response could be tuned from the mid- to the far-infrared to meet different mission requirements. If radiometric measurements are required, the radiometric error induced by variation of the temperature of the detector environment must be minimized. In a radiometric package, the detector environment is thermally stabilized by means of a temperature-controlled radiation shield. The radiation shield must be designed to prevent stray radiation from reaching the detector. A radiometric packaging technology for uncooled microbolometer FPAs is presented. The selection of materials is discussed and the final choices presented based on thermal simulations and experimental data. The radiometric stability with respect to stray light and variation of the temperature of the environment as well as the different noise components studied by means of the Allan variance are presented. It is also shown that the device successfully passed the prescribed environmental tests without degradation of performance.
An endoscope capable of Coherent Anti-Stokes Raman scattering (CARS) imaging would be of significant clinical value
for improving early detection of endoluminal cancers. However, developing this technology is challenging for many
reasons. First, nonlinear imaging techniques such as CARS are single point measurements thus requiring fast scanning in
a small footprint if video rate is to be achieved. Moreover, the intrinsic nonlinearity of this modality imposes several
technical constraints and limitations, mainly related to pulse and beam distortions that occur within the optical fiber and
the focusing objective.
Here, we describe the design and report modeling results of a new CARS endoscope. The miniature microscope
objective design and its anticipated performance are presented, along with its compatibility with a new spiral scanningfiber
imaging technology developed at the University of Washington. This technology has ideal attributes for clinical
use, with its small footprint, adjustable field-of-view and high spatial-resolution. This compact hybrid fiber-based
endoscopic CARS imaging design is anticipated to have a wide clinical applicability.
The use of uncooled microbolometer detectors for space infrared (IR) imaging application requires high optical
throughput, which leads to very fast optical design (~f/1). This directly translates into stringent requirements for
components, assembly and alignment. The Institut National d'Optique (INO) in Quebec City, Canada, designed such a
system for the NIRST IR Camera. The instrument is part of the Aquarius/SAC-D satellite, a cooperative mission
conducted jointly by NASA and the Comisión Nacional de Actividades Espaciales (CONAE) of Argentina.
Due to the tight volume and mass allocation, the NIRST camera module is an all refractive design. Since the Camera is
made of two lens barrels co-registered to cover the same ground area at different wavelength bands, it also adds coregistration
alignment constraints.
This paper presents the optomechanical solutions and alignment scheme that enabled the successful design and flight
qualification. Trade-off study between thermally induced stress and structural stiffness of the lens RTV bond is
discussed. Special attention is given to lens subcell alignment integrity under random vibration encountered during
launch. Detailed Finite Element Analysis (FEA) is used to check early design assumptions. Test results of the final
vibration campaign are also presented.
Aquarius/SAC-D is a cooperative international mission conducted jointly by the National Aeronautics and Space
Administration of the United States of America and the Comisión Nacional de Actividades Espaciales of Argentina.
Jointly developed by CONAE and the Canadian Space Agency, the New IR Sensor Technology (NIRST) instrument will
monitor high temperature events. NIRST has one band in the mid-wave infrared and two bands in the thermal infrared.
The baseline design of the NIRST is based on microbolometer technology developed jointly by INO and the CSA. This
paper will first present an overview of the design of the NIRST camera module. The manufacturing and qualification
activities for the Flight Model will be described and key performance parameters, as measured during the verification
campaign, will be reported.
KEYWORDS: Sensors, Staring arrays, Indium oxide, Readout integrated circuits, Gold, Prototyping, Reflectivity, Radiometry, Electronics, Simulation of CCA and DLA aggregates
The Broadband Radiometer (BBR) is an instrument being developed for the ESA EarthCARE satellite. The BBR
instrument objective is to provide top-of-atmosphere (TOA) radiance measurements in two spectral channels, and over
three along-track directions. The instrument has three fixed telescopes (one for each view) each containing a broadband
detector. Each detector consists of an uncooled 30-pixel linear focal plane array (FPA) coated with gold black in order to
ensure uniform spectral responsivity from 0.2 μm to 50 μm. The FPA is hybridized with a readout integrated circuit
(ROIC) and a proximity electronics circuit-card assembly (CCA) packaged in an aluminum base plate with cover. This
paper provides a technical description of the detector design and operation. Performance data at the FPA pixel level as
well as unit-level test results on early prototypes of the detectors are also presented.
INO has extensive experience in the design and fabrication of focal plane arrays (FPAs) of uncooled microbolometers.
In particular, the FPA of 512×3 microbolometers, developed in collaboration with the Canadian Space Agency (CSA),
has been selected for use in the NIRST (New Infrared Sensor Technology) radiometer of the SAC-D Aquarius mission.
The FPA has been designed for pushbroom scanning of the Earth to provide radiometric data in the mid- and long-wave
infrared for the monitoring of fires as well as thermal mapping of ocean temperature. Uncooled microbolometer
detectors are suited for space applications due to their low power consumption while still exhibiting adequate
performance. Furthermore, the spectral range of their response could be tuned from the mid- to the far-infrared to meet
different mission requirements. In order to ensure that the detector receives only the thermal contribution from the
desired target and to minimize radiometric error due to variation of the temperature of the surrounding during the
measurements, a radiometric package is required. In a radiometric package the detector environment is thermally
stabilized by means of a temperature controlled radiation shield. The radiation shield should also be designed to prevent
stray radiation from reaching the detector.
Under the Space Technology Development Program of the CSA, INO has designed, assembled and tested a radiometric
package in order to characterize its performance and compatibility with the space environment. The operating spectral
band is defined by the spectral characteristics of a bandpass filter placed in front of the FPA. For typical space missions,
the package must pass standard environmental tests without degradation of its performance (thermal cycling from -55 to
+85 °C according to MIL-STD-810, random acceleration up to 14 G RMS from 20-2000 Hz and shock up to 75 G). In
order to ensure reliability in those conditions while maintaining optimum performance, an adequate selection of
materials is necessary.
In this paper, INO's radiometric packaging technology for uncooled microbolometer FPA's will be presented. The
selection of materials will be discussed and the final choices presented based on thermal simulations and experimental
data. The effects of different design parameters on the performance, such as material, shape and thickness of radiation
shield and choice of adhesive have been studied. An instantaneous noise equivalent temperature difference (NETD) of
~ 20 mK was obtained under the measurement conditions (broadband LWIR, 140 ms integration time, f/1 optics,
characterization in flood exposure). The design of the package reduced the contribution of environmental temperature
variations on the offset of the sensor. The equivalent response of the package varied less than 0.08 °C per degree of
variation of the temperature of the package. The package also showed low sensitivity to stray radiation as a result of the
effectiveness of the radiation shield design. The device successfully passed the prescribed environmental tests without
degradation of performance.
The advent of wide-field imagers on large telescopes (Megacam at CFHT, Suprime-Cam at Subaru, and others)
with degree-wide fields of view is largely motivated by a renewed interest in our own solar system, in the history
of the Milky Way and its neighbors, and in the large-scale structure of the Universe. Smaller, university-based
telescopes can of course also benefit from wide-field imagery. We present in this paper the design and first
results of Panoramix-II, the new wide-field imager of the Mont Megantic Observatory (OMM). This instrument
is conceptually a focal reducer designed to image and correct the F/8 cassegrain focal plane of the telescope onto
a pair of 2KX4K EEV detectors. The camera is optimized for the SLOAN g' (410-550 nm), r' (550-690 nm), i'
(690-850 nm) and z' (850-950 nm) wave bands. The sky will be imaged onto the focal plane at an image scale
of 0.52 arcsecond per 13.5 μm pixel. The design image quality is 1.00 arcsecond 50% diffraction encircled
energy over the central 35 arcmin field and no images worse than 1.25 arcsecond over the 49 arcminute diameter
camera field. The optical design distortion at the corners is less than 1%. The Panoramix-II camera has a filter
wheel at the internal stop. Panoramix-II can also support the FaNTOmM photon-counting camera used in
conjunction with a Fabry-Perot interferometer to provide spectrometric data.
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