Next generation of astronomical instrumentation for space telescopes requires Micro-Opto-Electro- Mechanical Systems (MOEMS) with remote control capability and cryogenic operation. MOEMS devices have the capability to tailor the incoming light in terms of intensity and object selection with programmable slit masks, in terms of phase and wavefront control with micro-deformable mirrors, and finally in terms of spectrum with programmable diffraction gratings. Applications are multi-object spectroscopy (MOS), wavefront correction and programmable spectrographs. We are engaged since several years in the design, realization and characterization of MOEMS devices suited for astronomical instrumentation.
Based on the micro-electronics fabrication process, Micro-Opto-Electro-Mechanical Systems (MOEMS) are under study in order to be integrated in next-generation astronomical instruments for ground-based and space telescopes. Their main advantages are their compactness, scalability, specific task customization using elementary building blocks, and remote control. At Laboratoire d’Astrophysique de Marseille, we are engaged since several years in the design, realization and characterization of programmable slit masks for multi-object spectroscopy and micro-deformable mirrors for wavefront correction. First prototypes have been developed and show results matching with the requirements.
We are developing MEMS-based programmable reflective slit masks for future generation infrared multi-object
spectroscopy (MOS) for space and ground-based telescopes. These devices are composed of monocrystalline silicon
micromirrors of size 200 × 100 um2 which can be tilted by electrostatic actuation yielding a tilt-angle of 20°. An
electromechanical clamping mechanism has been demonstrated providing uniform tilt-angle within one arc minute
precision over the whole array (5 × 5 micromirrors). Slit masks of different sizes have been produced; the largest one
measures 25 × 22 mm2 and is composed of 20'000 micromirrors. Thanks to the architecture and the fabrication process
of these slit masks; the micromirror peak-to-valley deformation (PTV) is uniform over the device and was measured
being below 10 nm for uncoated micromirror. A slit mask of size 5 × 5 micromirrors was successfully tested in cryogenic
conditions at 92 K; the micromirrors were actuated before, during and after the cryogenic experiment. To achieve for the
large arrays a better fabrication yield and a higher reliability, the architecture, the process flow, the assembly and the
electronics are being optimized. Optical characterizations as well as experiments of the large devices are underway.
Multi-object spectroscopy (MOS) is a powerful tool for space and ground-based telescopes for studying the formation of
galaxies. This technique requires a programmable slit mask for astronomical object selection. A first sample of MEMS-based
programmable reflective slit masks with elements of size 200×100 μm2 has been successfully tested in cryogenic
conditions at 92 K. Devices of larger size were microfabricated, the largest chip measures 25×22 mm2 and is composed
of 200×100 electrostatic actuated micromirrors. These devices are composed of two chips: the electrode chip and the
mirror chip, which are processed separately and assembled consecutively. The mirror chip is bonded on top of the
electrode chip and microfabricated pillars on the electrode chip provide the necessary spacing between the two parts. A
process flow utilizing refilling techniques based on borophosphosilicate glass (BPSG) deposition and reflow was
developed. Programmable reflective slit masks based on this fabrication process were microfabricated and characterized.
These devices exhibit a micromirror deformation of 11 nm peak-to-valley and an actuation voltage of 145 V for a tilt
angle of 9°. Preparation of samples for MOS experiments are underway.
Next-generation infra-red astronomical instrumentation for space and ground-based telescopes requires MOEMS-based
programmable slit masks for multi-object spectroscopy (MOS) which has to work in cryogenic environment. A first
prototype of micromirror arrays (MMA) of 5×5 single-crystal silicon micromirrors was successfully designed,
fabricated and tested. 100×200 μm2 micromirrors can be tilted by electrostatic actuation yielding 20° mechanical tiltangle.
The MMA were successfully actuated before, during and after cryogenic cooling, below 100 K. A MMA is
composed of two different chips fabricated on silicon on insulator (SOI) wafers: the mirror chip and the electrode chip.
The array was obtained by assembling these two chips. For the assembly step of large array (100×200 micromirrors) we
needed high precision alignment as well as the suppression of manual handling. Therefore we developed a technique of
assembly for such devices and we designed and fabricated a dedicated XYZ tip/tilt stage. This stage allows aligning the
electrodes towards the micromirrors with a micrometer precision. Large MMA of 100×200 micromirrors, measuring
22 mm×25 mm, for large field of view were microfabricated and assembled using the above setup. No additional
deformations were observed due to the assembly step. The peak to valley (PTV) deformation of the micromirrors was
found to be 14 nm PTV. The first actuation tests were carried out.
We are developing a linear array of micromirrors designed for optical, femtosecond laser pulse shaping. It is a bulkmicromachined
device, capable of retarding or diminishing certain laser frequencies in order to perform phase and amplitude modulation within a frequency band spanning the UV to the near-infrared. The design consists of a linear array of mirrors fixed on either side by springs. They feature two degrees of freedom: Out-of-plane motion for phase shifting and
rotational motion for binary amplitude modulation, both realized using vertical comb drives. The first applications will include femtosecond discrimination experiments on biomolecules.
We are developing single-crystalline silicon micromirror arrays (MMA) for future generation infrared multiobject
spectroscopy (IR MOS). The micromirrors are 100μm × 200μm in size and can be tilted by electrostatic actuation
yielding a tilt-angle of 20°. Arrays of 5x5 micromirrors were gold-coated and tested at below 100K. The coated and
uncoated micromirrors are optically flat (peak-to-valley deformation < λ/20 for λ > 1μm) at room temperature
and in cryogenic environment. Successful actuation has been done at room temperature and at temperatures
below 100K. Large arrays of 200x100 micromirrors are being fabricated and an actuation scheme for extremely
large arrays has been developed.
We report on micromirror arrays being developed for use as
reflective slit masks in multiobject spectrographs for astronomical applications.
The micromirrors are etched in bulk single crystal silicon,
whereas cantilever-type suspension is realized by surface micromachining.
One micromirror element is 100200 m in size. A system of multiple
landing beams is developed, which electrostatically clamps the mirror
at a well-defined tilt angle when actuated. The mechanical tilt angle
obtained is 20 deg at a pull-in voltage of 90 V. Measurements with an
optical profiler show that the tilt angle of the actuated mirror is stable with
a precision of one arc minute over a range of 15 V. This electrostatic
clamping system provides uniform tilt angle over the whole array: the
maximum deviation measured between any two mirrors is as low as one
arc minute. The surface quality of the mirrors in the actuated state is
better than 10 nm peak-to-valley and the local roughness is around 1-nm
rms. Cryogenic testing shows that the micromirror device is functional at
temperatures below 100 K.
Next generation of infra-red astronomical instrumentation for space telescopes as well as ground-based extremely large
telescopes requires MOEMS devices with remote control capability and cryogenic operation, including programmable
multi-slit masks for multi-object spectroscopy (MOS).
For the complete testing of these devices, we have developed in parallel and coupled a high-resolution Twyman-Green
interferometer and a cryogenic-chamber for full surface and operation characterization. The interferometer exhibits a
nanometer accuracy by using phase-shifting technique and low-coherence source. The cryogenic-chamber has a
pressure as low as 10e-6 mbar and is able to cool down to 60K. Specific interfaces minimizing stresses for vacuum and
cryo have been set.
Within the framework of the European program on Smart Focal Planes, micro-mirrors have been selected for generating
MOEMS-based slit masks. A first 5×5 micro-mirror array (MMA) with 100×200μm2 mirrors was successfully
fabricated using a combination of bulk and surface silicon micromachining. They show a mechanical tilting angle of
20° at a driving voltage below 100V, with excellent surface quality and uniform tilt-angle. The mirrors could be
successfully actuated before, during and after cryogenic cooling. The surface quality of the gold coated micro-mirrors at
room temperature and below 100K, when they are actuated, shows a slight increase of the deformation from 35nm
peak-to-valley to 50nm peak-to-valley, due to CTE mismatch between silicon and gold layer. This small deformation is
still well within the requirement for MOS application.
We are developing micromirror arrays (MMA) for future generation infrared multiobject spectroscopy (MOS)
requiring cryogenic environment. So far we successfully realized small arrays of 5×5 single-crystalline silicon
micromirrors. The 100μm ×200μm micromirrors show excellent surface quality and can be tilted by electrostatic
actuation yielding 20° mechanical tilt-angle. An electromechanical locking mechanism has been demonstrated
that provides uniform tilt-angle within one arc minute precision over the whole array. Infrared MOS requires
cryogenic environment and coated mirrors, silicon being transparent in the infrared. We report on the influence
of the reflective coating on the mirror quality and on the characterization of the MMA in cryogenic environment.
A Veeco/Wyko optical profiler was used to measure the flatness of uncoated and coated mirrors. The uncoated
and unactuated micromirrors showed a peak-to-valley deformation (PTV) of below 10nm. An evaporated 10nm
chrome/50nm gold coating on the mirror increased the PTV to 35nm; by depositing the same layers on both
sides of the mirrors the PTV was reduced down to 17nm. Cryogenic characterization was carried out on a
custom built interferometric characterization bench onto which a cryogenic chamber was mounted. The chamber
pressure was at 10e-6 mbar and the temperature measured right next to the micromirror device was 86K. The
micromirrors could be actuated before, during and after cryogenic testing. The PTV of the chrome/gold coated
mirrors increased from 35nm to 50nm, still remaining in the requirements of < lambda/20 for lambda=1μm.
We report on micromirror arrays being developed for object selection in Multi Object Spectrographs for astronomical
applications. The micromirrors are etched in bulk single crystal silicon whereas the cantilever type
suspension is realized by surface micromachining. One micromirror element is 100μm × 200μm in size. The
micromirrors are actuated electrostatically by electrodes located on a second chip. The use of silicon on insulator
(SOI) wafers for both mirror and electrode chip ensures thermal compatibility for cryogenic operation. A system
of multiple landing beams has been developed, which passively locks the mirror at a well defined tilt angle
when actuated. The mechanical tilt angle obtained is 20° at a pull-in voltage of 90V. Measurements with an
optical profiler showed that the tilt angle of the actuated and locked mirror is stable with a precision of one arc
minute over a range of 15V. This locking system makes the tilt angle merely independent from process variations
across the wafer and thus provides uniform tilt angle over the whole array. The precision on tilt angle from
mirror to mirror measured is one arc minute. The surface quality of the mirrors in actuated state is better than
10nm peak-to-valley and the local roughness is around 1nm RMS. Preliminary cryogenic tests showed that the
micromirror device sustains 120K without any structural damage.
Devices based on SOI technology are subject to bow due to residual stress induced by the buried oxide. We have
designed and fabricated a compact tunable piston tip-tilt mirror device in which the shape and the arrangement of the
suspension beams result in both a reduced stress in the suspension beams and an optically flat mirror. The piston tip-tilt
mirror is characterized by an accurate vertical displacement of up to 18 &mgr;m @ 80 V with good repeatability, and a tip-tilt
of up to 2 mrad @ 50 V.
We report on micromirror arrays being developed for the use as reflective slit mask in Multi Object Spectrographs
for astronomical applications. The micromirrors are etched in bulk single crystal silicon whereas the cantilever
type suspension is realized by surface micromachining. One micromirror element is 100μm x 200μm in size. The
micromirrors are actuated electrostatically by electrodes located on a second chip. The use of silicon on insulator
(SOI) wafers for both mirror and electrode chip ensures thermal compatibility for cryogenic operation. A system
of multiple landing beams has been developed, which passively locks the mirror at a well defined tilt angle when
actuated. The mechanical tilt angle obtained is 20o at a pull-in voltage of 90V. Measurements with an optical
profiler showed that the tilt angle of the actuated and locked mirror is stable with a precision of one arc minute
over a range of 15V. This locking system makes the tilt angle merely independent from process variations across
the wafer and thus provides uniform tilt angle over the whole array. The precision on tilt angle from mirror to
mirror measured is one arc minute. The surface quality of the mirrors in actuated state is better than 10nm
peak-to-valley and the local roughness is around 1nm RMS.
KEYWORDS: Micromirrors, Mirrors, Astronomical imaging, Molybdenum, Electrodes, James Webb Space Telescope, Space telescopes, Spectrographs, Telescopes, Microopto electromechanical systems
Next generation MOS for space as well as ground-based instruments, including NIRSpec for JWST, require a
programmable multi-slit mask. A promising solution is the use of MOEMS-based devices such as micromirror arrays
(MMA) or micro-shutter arrays (MSA). Both configurations allow remote control of the multi-slit configuration in real
time. Engaged in the design studies for NIRSpec, we have developed different tools for the modelling and the
characterization of these devices. Since, we have continued our studies with commercial TI MMA and we show that in
a 20° ON-OFF configuration, the 3000 contrast requirement is fulfilled for any F# of 8m-class telescopes as well as
future ELT's.
Within the framework of the JRA on Smart Focal Planes, micro-mirrors have been selected in order to get a first
demonstrator of a European MOEMS-based slit mask. We have fixed several key parameters: one micromirror per
astronomical object, high optical contrast of at least 3000, tilting angle of 20°, fill factor of more than 90%, size of a
micro-element around 100 × 200 μm2, driving voltage below 100V. The MMA would also work in a wide range of
temperature down to cryogenic temperatures.
Based on these parameters, we have designed a new MMA architecture, using a combination of bulk and surface
micromachining. A first small test array of micro-mirrors was successfully fabricated and shows the desired mechanical
tilting angle of 20° at a driving voltage of about 100V. Preliminary measurements show a surface quality better than
lambda/20. Assembly of small test arrays with their electrode chips and design of larger arrays are under way.
Programmable multi-slit masks are required for next generation Multi-Object Spectrograph (MOS) for space as well as for ground-based instruments. A promising solution is the use of MOEMS devices such as micromirror arrays (MMA) or micro-shutter arrays (MSA), which both allow the remote control of the multi-slit configuration in real time. In the present work we developed and microfabricated a novel micro mirror array suited for this application. The requirements are: high contrast, optically flat (λ/20) mirrors in operation, high fill factor, uniform tilt angle over the whole array and low actuation voltage. In order to fulfill these requirements we use a combination of bulk and surface micromachining in silicon. The mirrors are actuated electrostatically by a separate electrode chip. The mirrors are defined by deep reactive ion etching in the 10μm thick device layer of a silicon-on-insulator (SOI) wafer, whereas the suspension of the mirrors is defined by a patterned poly-silicon layer hidden on the backside of the mirrors. The mirror size is 100 x 200 μm2 and the dimensions of a typical cantilever suspension are 100 x 5 x 0.6 μm3. On a separate SOI wafer the electrodes and the spacers are processed by using a self aligned delayed mask process. The first results on the mirror chips show that the micromirrors can easily achieve the desired mechanical tilt angle of more than 20° associated with a good surface quality, which is necessary for a high contrast spectroscopy.
A novel concept for video-rate parallel acquisition of optical coherence tomography imaging is presented based on in-pixel demodulation. The main restrictions for parallel detection such as data rate, power consumption, circuit size and poor sensitivity are overcome with a smart pixel architecture incorporating an offset compensation circuit, a synchronous sampling stage, programmable time averaging and random pixel accessing, allowing envelope and phase detection in large 1D and 2D arrays.
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