Most optical shops are now equipped with 5-axes grinding and polishing machines for manufacturing freeform optics. It can be advantageous to define off-axis parabolic (OAP) and ellipsoidal (OAE) mirrors as freeforms to ease their design, specification and fabrication as stand-alone wedge-less mirrors. This paper describes an algorithm generating the surface sag and sphere departure point clouds from the conjugation distances and fold angle of the mirror.
We describe the process through which stray light analysis should be performed in optical systems involving image slicers. We detail how scattering models should be used depending on how the image slicer assembly will be fabricated. Our work describes how to determine all ray paths, compute cross-talk on the pupil mirrors due to scattering, quantify the ghost images’ intensity, and determine baffle positions. In the example given, an ABg model is applied to all mirror arrays separately, before considering their contributions altogether. We also consider diffraction due to the image slicer’s narrow slice apertures, which contribute to unwanted light in the system by causing cross-talk on the pupil mirrors. Using Fourier optics, this quantity is computed and compared with cross-talk caused by scattering. Our work represents a useful asset for optical engineers who work on image slicer-based systems and want to analyze stray light, by providing a clear and exhaustive procedure to follow to obtain accurate estimates.
NRC’s NEW-EARTH Lab has demonstrated in the laboratory a Self-Coherent Camera (SCC) concept combined with a Tilt-Gaussian-Vortex focal plane mask (FPM). This speckle suppression technique, a.k.a. Fast Atmospheric SCC Technique (FAST), can enhance the contrast up to 100 times. Based on this success, NRC is now building SPIDERS, a visitor instrument for Subaru telescope to be installed on the infrared Nasmyth platform behind AO188 and the new Subaru Beam Switcher. The beam can be either shared between SPIDERS and SCExAO for simultaneous observations or sent entirely to only one instrument. SPIDERS should also benefit from the upcoming AO188 deformable mirror (DM) upgrade (64x64 actuators) turning A188 to AO3k. The key-components of SPIDERS are an ALPAO DM468, used as a second-stage AO correction, a pupil apodizer mask, a Tilt-Gaussian FPM, a Lyot stop, a beam-splitter feeding (i), a C-RED2 camera imaging a 5” FoV in narrow bands and (ii), an imaging Fourier-Transform Spectrograph and a SAPHIRA camera for spectroscopy up to R~20,000 over a 3.3” FoV. SPIDERS optical design is fully reflective up to the FPM to avoid chromatic aberrations and reduce the number of surfaces. Two off-axis ellipsoid mirrors are enough to form the pupil planes required on the DM and the apodizer mask, and the f/64 focus on the FPM. Only lenses are used from the FPM up to the C-RED2 camera to mitigate the sensitivity of the SCC to vibrations. The Lyot stop reflects the blocked light to a camera acting as a Low-Order Wavefront Sensor complementing the SCC focal plane wavefront sensing.
As part of the Keck All-sky Precision Adaptive optics (KAPA) project a laser Asterism Generator (AG) is being implemented on the Keck I telescope. The AG provides four Laser Guide Stars (LGS) to the Keck Adaptive Optics (AO) system by splitting a single 22W laser beam into four beams of equal intensity. We present the design and implementation of the AG for KAPA. We discuss the optical design and layout, the details of the mechanical design and fabrication, and the challenges of designing the assembly to fit into the limited available space on the Keck telescope.
NIRPS is a near-infrared (YJH bands), fiber-fed, high-resolution precise radial velocity (PRV) spectrograph installed at the ESO 3.6-m telescope in La Silla, Chile. Using a dichroic, NIRPS will be operated simultaneously with the optical HARPS PRV spectrograph and will be used to conduct ambitious planet-search and characterization surveys. NIRPS aims at detecting and characterizing Earth-like planets in the habitable zone of low-mass dwarfs and obtain high-accuracy transit spectroscopy of exoplanets. The spectrograph is compact for better thermal stability. Using a custom R4 grating in combination with a state-of-the-art Hawaii4RG detector, the instrument provides a high resolution and high stability over the range of 950-1800 nm. This paper focuses on the lens and optomechanical design, assembly, and test of NIRPS’s spectrograph. Some performance tests conducted at Université Laval (Canada) during the integration and at La Silla during commissioning are presented
NIRPS is an infrared precision Radial Velocity (pRV) spectrograph covering the range 950 nm-1800 nm. NIRPS uses a high-order Adaptive Optics (AO) system to couple the starlight into a fiber corresponding to 0.4" on the sky as efficiently or better than HARPS or ESPRESSO couple the light in a 1.0" fiber. This allows the spectrograph to be very compact, more thermally stable, and less costly. Using a custom tan(θ)=4 dispersion grating in combination with a start-of-the-art Hawaii4RG detector makes NIRPS very efficient with complete coverage of the YJH bands at just under 100 000 resolution. On the ESO 3.6-m telescope, NIRPS and HARPS are working simultaneously on the same target, building a single powerful high-resolution, high-fidelity spectrograph covering the 0.37-1.8 µm domain. NIRPS will complement HARPS in validating Earth-like planets found around G and K-type stars whose signal is at the same order of magnitude than the stellar noise. While the telescope-side AO system was installed on the ESO 3.6-m telescope in 2019, the infrared cryogenic spectrograph has been integrated at the telescope in early-2022 and has had first light in June 2022. Results from the first light mission show that NIRPS performs very nicely, that the AO system works up to magnitude I=14.5, that the transmission matches requirements and that the RV stability of 1 m/s is within reach While performance assessment is ongoing, NIRPS has demonstrated on-sky m/s-level stability over a night and <3 m/s level over two weeks. Limitations on the RV performances arise from modal noise that can be mitigated through better scrambling strategies. Better performances are also expected following a grating upgrade in July 2022; these will be tested in late-2022.
The first generation of ELT instruments includes an optical-infrared high resolution spectrograph, indicated as ELT-HIRES and recently christened ANDES (ArmazoNes high Dispersion Echelle Spectrograph). ANDES consists of three fibre-fed spectrographs (UBV, RIZ, YJH) providing a spectral resolution of ∼100,000 with a minimum simultaneous wavelength coverage of 0.4-1.8 µm with the goal of extending it to 0.35-2.4 µm with the addition of a K band spectrograph. It operates both in seeing- and diffraction-limited conditions and the fibre-feeding allows several, interchangeable observing modes including a single conjugated adaptive optics module and a small diffraction-limited integral field unit in the NIR. Its modularity will ensure that ANDES can be placed entirely on the ELT Nasmyth platform, if enough mass and volume is available, or partly in the Coudé room. ANDES has a wide range of groundbreaking science cases spanning nearly all areas of research in astrophysics and even fundamental physics. Among the top science cases there are the detection of biosignatures from exoplanet atmospheres, finding the fingerprints of the first generation of stars, tests on the stability of Nature’s fundamental couplings, and the direct detection of the cosmic acceleration. The ANDES project is carried forward by a large international consortium, composed of 35 Institutes from 13 countries, forming a team of more than 200 scientists and engineers which represent the majority of the scientific and technical expertise in the field among ESO member states.
NIRPS (Near Infra-Red Planet Searcher) is an AO-assisted and fiber-fed spectrograph for high precision radial velocity measurements in the YJH-bands. NIRPS also has the specificity to be an SCAO assisted instrument, enabling the use of few-mode fibers for the first time. This choice offers an excellent trade-off by allowing to design a compact cryogenic spectrograph, while maintaining a high coupling efficiency under bad seeing conditions and for faint stars. The main drawback resides in a much more important modal-noise, a problem that has to be tackled for allowing 1m/s precision radial velocity measurements. In this paper, we present the NIRPS Front-End: an overview of its design (opto-mechanics, control), its performance on-sky, as well as a few lessons learned along the way.
The Gemini Infrared Multi-Object Spectrograph (GIRMOS) is an adaptive optics-fed multi-object integral field spectrograph with a parallel imaging capability. The instrument is composed of four separate but identical spectrographs, giving it the ability to observe four objects simultaneously. Each slicer-based integral field spectrograph offers capabilities over three different fields of view (FOVs) and spatial sampling scales: 1.0”x1.0”, 2.1”x2.1” and 4.2”x4.2” out of a 2’ diameter field-of-regard, associated with samplings of 25 mas (mode 1), 50 mas (mode 2) and 100 mas (mode 3), respectively. Spectral resolutions of R=3000 and R=8000 are available in Y, J, H and K bands from 0.95 to 2.4 µm. To achieve spatial sampling requirements, the integral field unit (IFU) is designed as a 42-slices advanced image slicer. In this paper, the preliminary optical design and performances of the GIRMOS image slicer are presented, as well as the first diamond-turned prototype. The design is optimized for both optical performance and manufacturability by opting for a staircase arrangement that delivers diffraction-limited image quality while minimizing slice width losses due to diamond turning. Stray light and slice diffraction effects are also taken into account and reported.
We present the detailed performance of the preliminary end-to-end optical design of GIRMOS that is designed to take advantage of the multi-object adaptive optics corrected field at the Gemini North telescope. GIRMOS’s optical design consists of object selection pick-offs, adaptive optics, and four identical Integral-Field Spectrographs (IFSes), which employ image slicers to arrange the integral field along a slit. Each IFS can image the individual FOV of 1.0x1.0”, 2.0x2.0”, 4.0x4.0” over a 2’ diameter field-of-regard at different spatial sampling. The pick-offs can also be configured in close-packed arrangement to image a single field. Spectral resolutions of R~3000 and 8000 are available in 0.95-2.4 μm.
We proposed a model to estimate surface topography and transition edge width in diamond-turned non-circular compound freeform optics featuring right angle transitions. The method serves as comparison basis between both full and split radius tools and takes into consideration basic cutting and tooling parameters relevant to a raster tool path, along with multiple variables, such as material response and defects, tool wear, and spindle vibrations. Principles are applied to a set of adjacent rectangular surfaces of different tilts. Fabrication tests validating the model show good agreement between the proposed calculations and the experimental results and offer insight on how and when both tip geometries should be used. We represent a useful asset for optical engineers who want to determine which diamond tips choose for their freeform applications. It can also be employed to assess the attainable surface quality and width of edge transitions in compound freeform designs before manufacturing them.
We present unique optomechanical designs allowing precise fabrication and alignment of diamond-turned aluminum image slicers through preformed monolithic blocks and, most importantly, sub-group assemblies. This last approach reduces manufacturing time and risks while resulting in more alignment flexibility when compared to the traditional monolithic slicer build. We describe all optomechanical parts included in the process, as well as the selection of tooling and machining parameters to obtain good surface quality results on the first groups of slices for the GIRMOS (Gemini InfraRed Multi-Object Spectrograph) instrument image slicer.
In order to study distant galaxies and extra-solar planets, image slicers are now widely used in most integral field spectrographs (IFSes). Nonetheless, their multiple small tilted surfaces make them particularly difficult to manufacture, but equipment such as that of AOFI (Advanced Optical Fabrication Infrastructure) of University Laval eases this process. In this regard, the AOFI team has been tasked with the fabrication and characterization of the image slicer of the GIRMOS (Gemini Infra-Red Multi-Object Spectrograph) instrument. However, first attempts to produce small slicer prototypes have shown an issue with a monolithic diamond turning approach: manufacturing time. To address this matter and minimize tool wear while achieving good surface quality and optical performance, we have developed a unique manufacturing procedure, based on aluminum mechanical sub assemblies. This paper discusses this strategy and the metrology tests that were then applied to the image slicer of GIRMOS, including the analyses of surface roughness and other parameters such as tilts, curvature and active area.
The Gemini Infrared Multi-Object Spectrograph (GIRMOS) is an adaptive optics-fed multi-object integral field spectrograph with a parallel imaging capability. GIRMOS implements multi-object adaptive optics (MOAO) for each of its spectrographs by taking advantage of the infrastructure offered by Gemini upcoming wide-field AO facility at Manua Kea. The instrument offers the ability to observe four objects simultaneously within the Gemini-North AO (GNAO) system’s field-of-regard or a single object by tiling the four fields that feed light to four separate spectrographs. Each integral field spectrograph has an independent set of selectable spatial scales (0.025", 0.05", and 0.1" /spaxel) and spectral resolution (R 3,000 and 8,000) within an operating band of 0.95 2.4µm. These spatial scales correspond to indvidual spectrograph fields of view of 1x1", 2X2" , and 4x4", respectively. GIRMOS’s imager offers Nyquist sampling of the diffraction limit in H-band over a 85x85" imaging field. The imager can function in a parallel data acquisition mode with just minor vignetting spectroscopic pick- offs when they are deployed.
In this paper we discuss the mechanical design of the GIRMOS Cryostat. GIRMOS is an adaptive optics fed multi-object Integral-Field Spectrograph with a parallel imaging capability and will be installed at the Gemini North Observatory. This instrument includes four separate identical spectrograph channels arranged symmetrically around the central axis of the instrument which provide it its multiplexing capability. Each spectrograph channel starts off at the object selection mechanism. The object selection mechanism contains four motorized fold mirror assemblies which scan the incoming light from the telescope to look at four separate objects simultaneously or combine their efforts to look at a single object in a tiled mode. Each of the four individual beams from the object selection system are then directed into the instrument dewar via separate entrance windows. Within the dewar each IFS beam moves through an anamorphic relay, an optical image slicer assembly and eventually makes it to a Spectrograph unit. All of these assemblies are located on a single cold bench within the dewar. The instrument imager is located along the central axis of the dewar and is housed in the cold bench as well. In this paper we will provide some details regarding the Cryostat design, the mechanical packaging of the IFS and imager along with some of the thermal load mitigation techniques employed. We will also discuss some key performance requirements that were expected from the Cryostat and the design choices we made in order to achieve them.
We discuss the preliminary end-to-end optical design of an infrared multi-object integral-field spectrograph (GIRMOS) that is designed to take advantage of the multi-object adaptive optics corrected field at the Gemini telescope. GIRMOS’s optical design consists of object selection pick-offs, an adaptive optics (AO) system, and four identical Integral-Field Spectrographs (IFSes), which employ an image slicer to arrange the integral field along a slit. Each IFS can pick off the individual FOV of 1.0x1.0”, 2.0x2.0”, 4.0x4.0” over a 2’ diameter field-of-regard, at a spatial sampling of 25mas, 50mas, and 100mas, respectively. The pick-offs can also be configured in close-packed arrangement to image a single field. Spectral resolutions of R~3000 and 8000 are available in Y, J, H, and K-bands from 0.95 to 2.4μm.
KEYWORDS: Spectrographs, Telescopes, Lanthanum, Planets, Spectroscopes, Exoplanets, Aerospace engineering, Space operations, James Webb Space Telescope
NIRPS is a near-infrared (YJH bands), fiber-fed, high-resolution precision radial velocity (pRV) spectrograph currently under construction for deployment at the ESO 3.6-m telescope in La Silla, Chile. Through the use of a dichroic, NIRPS will be operated simultaneously with the optical HARPS pRV spectrograph and will be used to conduct ambitious planet-search and characterization surveys through a 720-night of guaranteed time allocation. NIRPS aims at detecting and characterizing Earth-like planets in the habitable zone of low-mass dwarfs and obtain high-accuracy transit spectroscopy of exoplanets. Here we present a summary of the full performances obtained in laboratory tests conducted at Université Laval (Canada), and the first results of the on-going on-sky commissioning of the front-end. Science operations of NIRPS is expected to start in late-2020, enabling significant synergies with major space and ground instruments such as the JWST, TESS, ALMA, PLATO and the ELT.
Image slicers have become a standard equipment in the field of astronomical spectroscopy. They are now widely used in most integral field spectrographs (IFSes) in order to detect and characterize distant galaxies or extra- solar planets. However, they are notoriously difficult to manufacture due to their multiple small tilted surfaces, but equipment such as that of AOFI (Advanced Optical Fabrication Infrastructure) of Universite Laval eases the process. In this regard, the team at AOFI has been tasked with the fabrication of the image slicer for the GIRMOS instrument. This paper presents the characterization of diamond turned RSA-6061 and AA-6061 T6 aluminum, and the definition of the different machining parameters, such as step size and tool radius, that could improve the surface quality of an aluminum image slicer. It also discusses the fabrication of the first prototypes at AOFI, that will eventually prove useful in the fabrication of the image slicer for GIRMOS, effectively lowering its risks.
Funding opportunities in science are essential to the research and development ecosystem. Numerous and competitive, the vast majority focus on scientific accomplishment. While the advancement of science remains a top priority, some funding agencies started to reshape their programs to include strict training requirements, from training plans included in proposals to regular evaluations of training progress. At the centre of this change is the recognition of the universities and colleges educational mission through research, and the need for a highly qualified workforce serving industry, science, and research. It is this need for applied research training, expressed by the Canadian aerospace community, that led to the creation of the Canadian Space Agency’s FAST (Flights and Fieldwork for the Advancement of Science and Technology) funding activity in 2011. Among the three main objectives of the 2017 opportunity, two target training the next and current generations of scientists and engineers for space-related areas in Canada by (1) developing and maintaining a critical mass of researchers, and (2) increasing the level of student employability by exposing them to practical experiences. In this paper, we report about the context behind CSA FAST’s creation, the funding opportunity model, and the impact of the funding activity. Concrete results are also shown for the HiCIBaS project, funded by CSA FAST 2015, an ambitious balloon-borne mission with an optical payload for wavefront sensing and exoplanet imaging that was led by 5 graduate students as part of their master’s program, and that culminated with a stratospheric balloon flight in August 2018.
HiCIBaS-LOWFS is a spatially modulated pyramid wavefront sensor to be used on the HiCIBaS project, a high-contrast imaging balloon borne telescope, as a fine pointing and atmospheric turbulence sensor. Since the project will be using a relatively small telescope on a limited budget, creative solutions must be developed to respond to the requirements for such systems. For example, we need a linear response to large error in order to be able to correct for pointing error in a photon-limited regime caused by the telescope small size. Most solutions aren't well suited for the optical design in HiCIBaS since the high-contrast coronagraph and the Low-Order Wavefront Sensor (LOWFS) both run as separate instruments. The design is centered around the modification of existing pyramid wavefront sensor by adding static, spatial modulation to an otherwise unmodulated system. The spatial modulation is achieved by adding an axicon (a conical optical element) at an imaged telescope pupil plane. This has for effect to add a very large non- common path aberration between the imaging plane and the wavefront sensor. This has for effect to shape the point-spread function incident on the pyramid to a ring shape, which minimize diffraction effect on the apex of imperfect pyramids. We present the first lab results involving the wavefront sensor and its performances for wavefront reconstruction and pointing accuracy. We also discuss the first on-sky results that were recorded with the 1.6-m telescope at the Observatoire du Mont-Megantic in Qubec, Canada using Universite Lavals optical AO test-bench. These results pave the way to the design and integration of the wavefront sensor in the context of the HiCIBaS project.
The HiCIBaS (High-Contrast Imaging Balloon System) project aims at launching a balloon borne telescope up to 36km to test high contrast imaging equipment and algorithms. The payload consists of a off the shelf 14-inch telescope with a custom-built Alt-Az mount. This telescope provides lights to two sensors, a pyramidal low order wave front sensor, and a coronagraphic wavefront sensor. Since the payload will reach its cruise altitude at about midnight mission, two target stars have been designated for observations, Capella as the night target, and Polaris as the early morning target. Data will be collected mainly on the magnitude of atmospheric and gondola’s turbulences, the luminosity of the background. The whole system is already built and ready to ship to Timmins for the launch in mid-August 2018.
We discuss the optical design of an infrared multi-object integral-field spectrograph (IRMOS) that is designed to take advantage of the multi-object adaptive optics corrected field at the Gemini telescope. The IRMOS is designed for the Gemini Telescope, so we call this instrument GIRMOS. The GIRMOS has four identical Integral-Field Spectrographs (IFSes), which employ a unique slicer design to arrange the integral field along a slit to obtain two-dimensional spectroscopy. Each IFS can pick off the individual fields of view of 1.0x1.0”, 2.1x2.1”, 4.2x4.2” over a 2’ diameter fieldof- regard, at the spatial sampling scales of 25mas, 50mas, and 100mas, respectively. Spectral resolutions of R~3000 and 8000 are available in J, H, and K-bands from 1.0 to 2.4μm. The primary design constraints are associated with diffractive effects from the grating and spectrograph camera.
NIRPS (Near Infra Red Planet Searcher) is a new ultra-stable infrared ( YJH) fiber-fed spectrograph that will be installed on ESO’s 3.6-m telescope in La Silla, Chile. Aiming at achieving a precision of 1 m/s, NIRPS is designed to find rocky planets orbiting M dwarfs, and will operate together with HARPS (High Accuracy Radial velocity Planet Searcher). In this paper we describe NIRPS science cases, present its main technical characteristics and its development status.
The use of Lagrangian platforms and of Autonomous Underwater Vehicles (AUVs) in oceanography has increased rapidly over the last decade along with the development of improved biological and chemical sensors. These vehicles provide new spatial and temporal scales for observational studies of the ocean. They offer a broad range of deployment and recovery capabilities that reduce the need of large research vessels. This is especially true for ice-covered Arctic ocean where surface navigation is only possible during the summer period. Moreover, safe underwater navigation in icy waters requires the capability of detecting sea ice on the surface (ice sheets). AUVs navigating in such conditions risk collisions, RF communication shadowing, and being trapped by ice keels. In this paper, an underwater sea-ice detection apparatus is described. The source is a polarized continuous wave (CW) diode-pumped solid-state laser (DPSS) module operating at 532 nm. The detector is composed of a polarizing beam splitter, which separates light of S and P polarization states and two photodetectors, one for each polarized component. Since sea-ice is a strong depolarizer, the ratio P/S is an indicator of the presence or absence of sea-ice. The system is capable of detecting sea-ice at a distance of 12m. This apparatus is designed to be used by free drifting profiling floats (e.g., Argo floats), buoyancy driven vehicles (e.g., sea gliders) and propeller-driven robots (e.g., Hugin class AUV).
Since 1st light in 2002, HARPS has been setting the standard in the exo-planet detection by radial velocity (RV) measurements[1]. Based on this experience, our consortium is developing a high accuracy near-infrared RV spectrograph covering YJH bands to detect and characterize low-mass planets in the habitable zone of M dwarfs. It will allow RV measurements at the 1-m/s level and will look for habitable planets around M- type stars by following up the candidates found by the upcoming space missions TESS, CHEOPS and later PLATO. NIRPS and HARPS, working simultaneously on the ESO 3.6m are bound to become a single powerful high-resolution, high-fidelity spectrograph covering from 0.4 to 1.8 micron. NIRPS will complement HARPS in validating earth-like planets found around G and K-type stars whose signal is at the same order of magnitude than the stellar noise. Because at equal resolving power the overall dimensions of a spectrograph vary linearly with the input beam étendue, spectrograph designed for seeing-limited observations are large and expensive. NIRPS will use a high order adaptive optics system to couple the starlight into a fiber corresponding to 0.4” on the sky as efficiently or better than HARPS or ESPRESSO couple the light 0.9” fiber. This allows the spectrograph to be very compact, more thermally stable and less costly. Using a custom tan(θ)=4 dispersion grating in combination with a start-of-the-art Hawaii4RG detector makes NIRPS very efficient with complete coverage of the YJH bands at 110’000 resolution. NIRPS works in a regime that is in-between the usual multi-mode (MM) where 1000’s of modes propagates in the fiber and the single mode well suited for perfect optical systems. This regime called few-modes regime is prone to modal noise- Results from a significant R and D effort made to characterize and circumvent the modal noise show that this contribution to the performance budget shall not preclude the RV performance to be achieved.
With the upcoming construction of ELTs, several existing technologies are being pushed beyond their performance limit and it became essential to develop and evaluate alternatives. We present a specifically designed focal plane box which will allow to evaluate, directly on-sky, the performance of a number of next generation adaptive optics related technologies The system will able us to compare the performance of several new wavefront sensors in contrast to a Shack-Hartman wavefront sensor. The system has been designed for the "Observatoire du Mont Mégantic" (OMM) which hosts a telescope having a 1.6-meter diameter primary. The OMM telescope, located halfway between Montreal and Quebec City, is known to be an excellent location to develop and test precursor instruments which can then be upscaled to larger telescopes (ex. SPIOMM which led to SITELLE at the CFHT). We present the results of the first run made at the telescope and also identify problems that were encountered. We also propose a series of modifications to the system that will help to solve these issues.
The SITELLE Imaging Fourier Transform Spectrometer was successfully commissioned at the Canada France Hawaii Telescope starting in July 2015. Here we discuss the commissioning process, the outcome of the early tests on-sky as well as the ensuing work to optimize the modulation efficiency at large optical path difference and the image quality of the instrument.
We present the integration status for 'imaka, the ground-layer adaptive optics (GLAO) system on the University of Hawaii 2.2-meter telescope on Maunakea, Hawaii. This wide-field GLAO pathfinder system exploits Maunakea's highly confined ground layer and weak free-atmosphere to push the corrected field of view to ∼1/3 of a degree, an areal field approaching an order of magnitude larger than any existing or planned GLAO system, with a FWHM ∼ 0.33" in the visible and near infrared. We discuss the unique design aspects of the instrument, the driving science cases and how they impact the system, and how we will demonstrate these cases on the sky.
WFIRST-AFTA is the NASA’s highest ranked astrophysics mission for the next decade that was identified in the New
World, New Horizon survey. The mission scientific drivers correspond to some of the deep questions identified in the
Canadian LRP2010, and are also of great interest for the Canadian scientists. Given that there is also a great interest in
having an international collaboration in this mission, the Canadian Space Agency awarded two contracts to study a
Canadian participation in the mission, one related to each instrument. This paper presents a summary of the technical
contributions that were considered for a Canadian contribution to the coronagraph and wide field instruments.
The Near Infrared Imager and Slitless Spectrograph (NIRISS) Optical Simulator (NOS) is a
laboratory simulation of the single-object slitless spectroscopy and aperture masking interferometry modes of the
NIRISS instrument onboard the James Webb Space Telescope (JWST). A transiting exoplanet can be simulated
by periodically eclipsing a small portion (1% - 10ppm) of a super continuum laser source (0.4 μm - 2.4 μm) with
a dichloromethane filled cell. Dichloromethane exhibits multiple absorption features in the near infrared domain
hence the net effect is analogous to the atmospheric absorption features of an exoplanet transiting in front of its
host star. The NOS uses an HAWAII-2RG and an ASIC controller cooled to cryogenic temperatures. A separate
photometric beacon provides a flux reference to monitor laser variations. The telescope jitter can be simulated
using a high-resolution motorized pinhole placed along the optical path. Laboratory transiting spectroscopy data
produced by the NOS will be used to refine analysis methods, characterize the noise due to the jitter, characterize
the noise floor and to develop better observation strategies. We report in this paper the first exoplanet transit
event simulated by the NOS. The performance is currently limited by relatively high thermal background in the
system and high frequency temporal variations of the continuum source.
Many wavefront sensors have been developed over the years, but most are not well suited for the photon-limited regime of coronagraphs designed for 10-9 contrast ratios and small inner working angles (IWAs). To meet current coronagraphs low-order wavefront sensing requirements, it is essential to have a method that offers high sensitivity and preferably a linear response. We propose an innovative low-order wavefront sensor (LOWFS) design that is both achromatic and near free of non-common path aberrations (NCPAs).
With the upcoming construction of Extremely Large Telescopes, several existing technologies are being pushed beyond their performance limit and it becomes essential to develop and evaluate new alternatives. The "Observatoire du Mont Mégantic" (OMM) hosts a telescope having a 1.6-meter diameter primary. The OMM telescope is known to be an excellent location to develop and test precursor instruments which are then upscaled to larger telescopes (ex. SPIOMM which led to SITELLE at the CFHT). We present a specifically designed focal plane box for the OMM which will allow to evaluate, directly on-sky, the performance of a number of next generation adaptive optics related technologies The system will able us to compare the performance of several new wavefront sensors in contrast with the current standard, the Shack-Hartman wavefront sensor.
Astronomy with ground-layer adaptive optics systems will push observations with AO to much larger fields of view than previously achieved. Observations such as astrometry of stars in crowded stellar fields and deep searches for very distant star-forming galaxies pushes the systems to the widest possible fields of view. Optical turbulence profiles on Maunakea, Hawaii suggest that such a system could deliver corrected fields of view several tens of arcminutes in size at resolutions close to the free-atmosphere seeing. We present the status of a pathfinder wide field of view ground-layer adaptive optics system on the UH2.2m telescope that will demonstrate key cases and serve as a test bed for systems on larger telescopes and for systems with even larger fields of view.
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.
SITELLE is an imaging FTS that will become a guest instrument at the Canada-France-Hawaii telescope (CFHT) by the
end of 2014. This paper describes the final optical design of SITELLE, shows how the compliance of the sub-optical
components with the design was evaluated, and presents results of the measured optical quality.
KEYWORDS: Cameras, Polarization, Circular polarizers, Magnesium, Real time imaging, Prototyping, Signal detection, Target detection, Light sources, Light sources and illumination
Extensive peer reviewed scientific research has demonstrated the utility of polarization difference imaging (PDI) to reveal subtle surface details and textures in poor lighting conditions caused by fog, smoke, clouds or turbid water. We present sample results of a new real time PDI camera showing the ability of the camera to enhanced imaging harsh environments, particularly in turbid water.
We present progress towards the development of a woofer-tweeter adaptive optics (AO) system using the first 37
actuators of a 91-actuator magnetic-liquid deformable mirror (MLDM) and a magnetic 97-actuator DM from ALPAO.
The MLDM, which has both very large single-actuator and inter-actuator strokes, but a low bandwidth, is used as
woofer, whereas the high bandwidth and lower stroke ALPAO DM is used as tweeter. The ALPAO DM should improve
the bandwidth of the MLDM while the MLDM will allow correction of strong aberrations.
With the growing number of complex-shaped lenses, aspheric and freeform surfaces, the demand for an appropriate and
cost effective measurement technique to test these high quality components is still very high. Ferrofluid deformable
mirrors (FDMs) offer a promising alternative. However, high accuracy profiles produced by FDMs have only been
demonstrated in a closed-loop system which is inappropriate for metrology applications as it requires an additional
measurement instrument and complicates the setup. Consequently, a FDM open-loop driving technique which maintains
good precision while being simple, robust and stable, is required. In the following paper, we present a new active null
test system based on a FDM for the testing of deep aspheric surfaces. We show a new driving method which provides an
accurate open-loop operation mode of a FDM. We demonstrate that the method gives a significant improvement in
comparison with the normalized influence function method. The results are promising enough to consider an active null
test configuration for measuring optical components having high sag departures or complicated continuous profiles.
Many technical improvements have been made since we first introduced deformable mirrors that use magnetic liquids
(ferrofluids) whose surface are shaped by arrays of small electric coils. We present recent advances and experimental
results of a 91-actuator magnetic liquid deformable mirror that uses a novel technique that linearizes their response by
placing the array of actuators inside a strong and uniform magnetic field. We show that this improved ferrofluid
deformable mirror (FDM) can produce inter-actuator strokes of over 10 μm, is capable of generating wavefront having
peak-to-valley amplitudes of over 60 μm, and predict that amplitudes greater than 100 μm are achievable. We also
present experimental results showing that these improved FDMs are good candidates for astronomical, vision science,
and optical testing applications.
The new giant telescopes can be compared to space projects. They will require ground-based test
support equipment to fully characterize the optical sub-system functionalities and performances
before costly commissioning on the telescope. The support equipment must be designed to reproduce
the telescope or the front optical system's aberrated wavefront. We show that the aberrated
wavefront can be generated at low cost by a magnetic liquid deformable mirror. A prototype 91-
actuator liquid deformable mirror having a diameter of 33 mm was built and used to simulate the
off-axis aberrated CFHT's primary mirror up to 0.5 degrees FOV.
We present the research status of a deformable mirror made of a magnetic liquid whose surface is actuated by a
triangular array of small current carrying coils. We demonstrate that the mirror can correct a 11 μm low order aberrated
wavefront to a residual RMS wavefront error 0.05 μm. Recent developments show that these deformable mirrors can
reach a frequency response of several hundred hertz. A new method for linearizing the response of these mirrors is also
presented.
We give a progress report on an application of a new class of versatile optical elements pioneered by our
laboratory: By coating liquids we create reflective surfaces that can be shaped by rotation into a parabolic
mirror. Coated ferrofluids can also be shaped with magnetic fields.
Low cost is what makes rotating mercury LM Telescopes interesting. However, they are limited by the
fact that they cannot be tilted. We are now working on a new generation of LMs that can be tilted. The goal is
to produce large inexpensive LMTs that can be tilted by at least twenty degrees. Early work demonstrated a
tilted LM that used a high viscosity liquid. An extrapolation law, confirmed by our experiments, shows that it
should be possible to tilt LMs by twenty degrees, assuming a liquid having a few times the viscosity of
glycerin. Rotating nanoengineered LMTs are interesting even without tilting, since their lower weight would
make then less costly than Hg mirrors and high viscosity makes them less sensitive to winds.
We have made two major recent technological breakthroughs: We have made a robotic machine which
is capable of producing the large quantities of coating material required for large mirrors. We have also
developed a technique that allows us to coat the appropriate class of liquids by simply spraying the
nanoengineered coating on them. In this contribution, we present optical tests of our liquids as well as optical
shop tests of rotating mirrors.
We give a progress report on a new class of versatile optical elements pioneered by our laboratory. By coating ferromagnetic liquids we create reflective surfaces that can be shaped with magnetic fields, allowing us to make complex wavefronts that can vary rapidly in time. This new technology is capable of achieving complex surfaces that cannot be obtained with existing technology. The short-term objective is to perfect the technology for adaptive optics for both astronomical and ophthalmology applications. We have made a functional 112 actuator deformable mirror and characterized the ferrohydrodynamic response of the actuators. We have used high speed sensors to analyze the mirror surface subject to transient and periodic driving forces. We have developed algorithms to shape the surfaces. We have made new types of ferrofluids that are easier to coat with our nanoengineered layers. Theoretical model shown how the mirror parameters can be tuned as function of the applications. Challenges in design are outlined, as are advantages over traditional deformable mirrors.
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