The goal of the CHara ARray Integrated Optics Testbench (CHARIOT) is to establish a fully characterized (nulling) interferometry setup for on-sky tests of novel astrophotonic 2D or 3D beam combiners for the interferometry community worldwide. CHARIOT is planned for four telescope beams covering the J-, H-, and K-bands with plug-and-play fiber interfaces. Verifying novel astrophotonics on-sky with CHARIOT will enable the development of components and advances in instruments in many fields, including nulling and spectro-interferometry.
A photonic integrated circuit (PIC) is a lightweight, compact alternative to bulk optics. The Fibered Imager foR a Single Telescope (FIRST) instrument, is a spectro-interferometer performing pupil remapping and designed to operate in the 600 to 800nm visible wavelength range. It is installed on the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument’s platform at the Subaru telescope. In the integrated optical version of FIRST (FIRST PIC), the interferometric combination of the beams occurs by the pairwise combination of five sub-apertures to achieve 20 baselines. This paper introduces a PIC design with novel components for splitting and pairwise coupling the light for FIRST PIC, fabricated and packaged by LioniX International. A high index difference between the waveguide fundamental mode and cladding material was selected to allow compact circuits with prospects of increasing the number of combined sub-apertures with designs of much greater complexity. The high confinement waveguides were simulated to produce approximately 50% injection loss, a tapering system in both height and width to a low confinement waveguide at the PIC interface ameliorated the loss. The optimised throughput prediction is estimated at 80%. Standard couplers and splitters are expected to have high losses due to fabrication tolerances, and due to the high confinement, standard couplers’ performance is highly dependent on the wavelength. Presented here are novel component designs to replace them. Tapered directional couplers, which maintain an acceptable coupling ratio over the entire bandwidth, and tri-couplers, with higher throughput than conventional splitters but high intolerance to fabrication issues, were designed and fabricated for this purpose. The designs and individual experimental verification will be discussed, focusing on polarization and wavelength response. The full combination of components was used to create a five sub-aperture combiner for FIRST. Cross-talk between crossed waveguides was measured independently for the two polarisations. The cross-coupling over the full bandwidth was measured as low as 2% in one polarization, without active subtraction for scattered light to confirm the light in the ports was guided from the cross-coupling, and as low as 8% in the other. Additional work, and potential refinement of the photonic chip components, are required to differentiate the scattered light from the cross-talk to ensure it is reduced in both polarisations.
The Fiber Imager foR a Single Telescope (FIRST) is a visible spectro-interferometer (600-760 nm, R~400) installed on the Subaru telescope's extreme adaptive optics platform (SCExAO). It provides high-precision spatial coherence measurements with high angular resolution (~8 mas at 656 nm, ~1% coherence accuracy) by combining light from sub-apertures of the telescope pupil. We present two upgrades of the instrument towards H𝛼 detection of protoplanets. We report on the integration of a new 4000-resolution spectrograph and on the sensitivity of the instrument. We also present the characterisation of a high performance visible photonic integrated circuit prototype used for the interferometric combination of 5 sub-apertures.
FIRST (Fibered Imager foR a Single Telescope instrument) is an on-sky instrument at SUBARU Telescope that enables high-contrast imaging and spectroscopy, thanks to a unique combination of pairwise combination of sub-apertures using a Photonic Integrated Circuit that allows spatial filtering by single-mode waveguides and cross-dispersion in the visible (~ 600-800 nm), a high-efficiency alternative to sparse aperture masking. To reduce crosstalk observed in planar PICs, and therefore increase the instrument’s stability and sensitivity, we have designed and fabricated a series of 3D laserwritten optical PICs with 5T beam combiners. Different laser powers were used to address different single-mode spectral ranges. The multi-aperture beam combiner consists of five input waveguides spaced by 250 μm. Each input is split into four waveguides and the twenty channels undergo pairwise recombination, using Y-junctions, to produce ten outputs. In this work, we present the interferometric performances of these 3D PICs when exposed to a point-like light source (single star) or a two-points-like light source (binary) on the FIRST/SUBARU instrument replica built at LESIA – Observatoire de Paris.
In previous work, we identified the optimal 5T 3D device, as being single-mode between 550-800 nm and showing good internal transmission in all input channels, above 45% at 635nm. The internal transmission (sum of the output values obtained for the four waveguides of the 1x4 splitter as normalized to the output signal obtained from the straight waveguide used as a reference) was measured. Two inputs achieved 80% transmission. The PIC was installed in the FIRST/SUBARU optical bench simulator at LESIA, to inject light into five inputs simultaneously and scan the fringes using independent MEMS segments, inducing a relative OPD modulation. The results of this study, comparing the signature obtained for a single source (star) as compared to a binary, will be presented in this work. We will show that both polarizations are guided, with no crosstalk, and analyze the interferometric performances as a function of the source type, showing that the binary companion can be detected.
FIRST (Fibered Imager foR a Single Telescope instrument) is a post-AO instrument that enables high-contrast imaging and spectroscopy at spatial scales below the diffraction limit. FIRST achieves sensitivity and accuracy through a unique combination of sparse aperture masking, spatial filtering by single-mode fibers and cross-dispersion in the visible. On-sky commissioning data taken with the instrument installed on the SCExAO platform at the 8-m Subaru telescope show the detection of several stellar companions, including two binary systems with an angular separation of 0.6 λ/D (11mas). Even at such a close separation, FIRST delivers information on the companion spectrum, providing valuable constraints on the stellar parameters, such as the effective temperatures and surface gravity. As a spectro-interferometer fed by a highly effective AO system such as SCExAO, FIRST offers unique capabilities in the context of the spectral characterization of close companions. The discussion concludes with insights into the future of the FIRST instrument, with the move to visible photonic technologies and further advancements in the instrument's capabilities to detect newly formed exoplanets.
FIRST is a post Extreme Adaptive-Optics (ExAO) spectro-interferometer operating in the Visible (600-800 nm, R∼400). Its exquisite angular resolution (a sensitivity analysis of on-sky data shows that bright companions can be detected down to 0.25λ/D) combined with its sensitivity to pupil phase discontinuities (from a few nm up to dozens of microns) makes FIRST an ideal self-calibrated solution for enabling exoplanet detection and characterization in the future. We present the latest on-sky results along with recent upgrades, including the integration and on-sky test of a new spectrograph (R∼3,600) optimized for the detection of Hα emission from young exoplanets accreting matter.
Integrated optics are used to achieve astronomical interferometry inside robust and compact materials, improving the instrument’s stability and sensitivity. To perform differential phase measurements at the Hα line (656.3 nm) with the 600- to 800-nm spectro-interferometer fibered imager for a single telescope (FIRST), a photonic integrated circuit (PIC) is being developed in collaboration with TEEM Photonics. This PIC performs the interferometric combination of the beams coming from subapertures selected in the telescope pupil, thus implementing the pupil remapping technique to restore the diffraction limit of the telescope. In this work, we report on the latest developments carried out within the FIRST project to produce a high-performance visible PIC. The PICs are manufactured by TEEM Photonics, using their technology based on K + : Na + ion exchange in glass. The first part of the study consists in the experimental characterization of the fundamental properties of the waveguides, to build an accurate model, which is the basis for the design of more complex functions. In the second part, theoretical designs and their optimization for three types of combiner architectures are presented: symmetric directional coupler, asymmetric directional couplers, and ABCD cells, including achromatic phase shifters.
Laboratory testbeds are an integral part of conducting research and developing technology for high-contrast imaging and extreme adaptive optics. There are a number of laboratory groups around the world that use and develop resources that are imminently required for their operations, such as software and hardware controls. The CAOTIC(Community of Adaptive OpTics and hIgh Contrast testbeds) project is aimed to be a platform for this community to connect, share information, and exchange resources in order to conduct more efficient research in astronomical instrumentation, while also encouraging best practices and strengthening cross-team connections. In these proceedings, we present the goals of the CAOTIC project, our new website, and we focus in particular on a new approach to teaching version control to scientists, which is a cornerstone of successful collaborations in astronomical instrumentation.
FIRST (Fibered Imager foR a Single Telescope instrument) is an instrument that enables high contrast imaging and spectroscopy, thanks to a unique combination of sparse aperture masking, spatial filtering by single-mode waveguides and cross-dispersion in the visible. In order to increase the instrument’s stability and sensitivity, we propose an active hybrid photonic beam combiner. The device consists on a 5T integrated optics beam combiner. The idea is to split the architecture in two parts: A first part, concerning input beam splitting and active phase modulation, requiring relatively simple optical circuits (Y junctions and straight waveguides) is obtained in an electro-optic crystal (Lithium Niobate). A second part, where the complex beam recombination of all the split inputs is achieved (for N inputs, N(N-1)/2 recombinations). This stage implies many waveguide crossings, bendings and lengthy waveguides. Therefore, a high transmission, high confining glass is used. In both cases, classical lithography and ion in-diffusion techniques are used to fabricate the waveguides. Both stages have been optimized in terms of mode matching and single mode spectral bandwidth. They have been assembled together and with input/output fibered V-grooves. The work presented here consists on the characterization of the hybrid 5T beam combiner on the optical bench simulator of the FIRST/SUBARU instrument that is developed at LESIA. We will present results in terms of transmission, polarization and active phase modulation, showing that with relative low voltages, active fringe scan is achieved directly on-chip, at frequencies only limited by the readout time of the camera.
FIRST (Fibered Imager foR a Single Telescope instrument) is an instrument that enables high contrast imaging and spectroscopy, thanks to a unique combination of sparse aperture masking, spatial filtering by single-mode waveguides and cross-dispersion in the visible. In order to increase the instrument’s stability and sensitivity, we have designed and fabricated a 3D laser-written optical chip 5T beam combiner. The multi-aperture beam combiner consists of 5 input waveguides spaced by 250um. Each input is split into 4 waveguides. A pairwise recombination scheme with Yjunctions produces/leads to 10 outputs (127um separation, compatible with commercial V-grooves). In this work, we present the experimental characterization of the chip: transmission performance, polarization issues and single mode spectral range. The targeted single mode spectral range must cover 550-800nm. Different optical powers for laser writing are used to finely tune the ideal single-mode behavior of the waveguides, ranging from 220 to 270mW. A straight waveguide was used as a reference, imprinted close to the first interferometric channel. Using different lasers (635nm, 780nm and 980nm) as well as wideband sources, we have been able to characterize the spectral transmission, the polarization behavior (TE/TM) and the interferometric contrast. The chip was inserted in the FIRST/SUBARU optical bench simulator at LESIA, in order to inject the 5 inputs simultaneously and scan the fringes using 4 independent MEMS, inducing a relative OPD modulation. Preliminary results show very good transmission for such a complex chip: all input channels are above 45% at 635nm (comparing the injected single mode with the sum of the 4 corresponding outputs), with two inputs reaching 80%. A huge advantage of this technology is to avoid the crosstalk due to in-plane waveguide crossings, and we show that no crosstalk is indeed observed. Both polarizations are transmitted, without noticeable birefringence. However, perfect vertical alignment of the outputs is difficult to obtain, and must be optimized prior to any connectorization to fiber bundles.
Integrated optics are used to achieve astronomical interferometry inside robust and compact materials, improving the instruments stability and sensitivity. In order to perform differential phase measurements at the Hα line (656.3nm) with the 600-800nm spectro-interferometer FIRST, a photonic integrated circuit (PIC) is being developed. This PIC performs the visible combination of the beams coming from the telescope pupil sub-apertures. In this work, TEEM Photonics waveguides fabricated by K+ : Na+ ion exchange in glass are characterized in terms of single-mode range and mode field diameter. The waveguide diffused index profile is modeled on Beamprop software. FIRST beam combiner building blocks are simulated, especially achromatic directional couplers and passive π/2 phase shifters for a potential ABCD interferometric combination.
FIRST is a post Extreme Adaptive-Optics (ExAO) spectro-interferometer based on pupil remapping using single-mode fibers. Installed on the SCExAO platform at the Subaru Telescope, it operates in the Visible (600-800nm, R 400) and demonstrated companion detection below the telescope diffraction limit. As an interferometric device, FIRST is sensitive to phasing problems in the telescope pupil. This is particularly interesting to measure discontinuous aberrations, invisible to the ExAO sensors. Recent developments aimed to measure upstream aberrations directly from the same interferometric signal used for scientific data analysis. A key limitation to this new capability is the fiber thermal and mechanical instabilities, inducing up to 1 micron drift over a few seconds. We propose to use a metrology laser source, allowing to discriminate FIRST instrumental effects from all the upstream aberrations. We present the integration of this setup and the on-sky demonstration of the method.
FIRSTv2 (Fibered Imager foR a Single Telescope version 2) is the upgrade of a post-AO spectro-interferometer (FIRST) that enables high contrast imaging and spectroscopy at spatial scales below the diffraction limit of a single telescope. It aims at using a photonic chip beam combiner, allowing the measurement of the complex visibility for every baseline independently thus improving the dynamic range. I will report on the first on-sky results obtained with several prototype chips integrated at the Subaru Telescope on unresolved and binary stars, for the first time in the visible.
Post Extreme Adaptive-Optics (ExAO) spectro-interferometers design allows high contrast imaging with an inner working angle down to half the theoretical angular resolution of the telescope. This regime, out of reach for conventional ExAO imaging systems, is obtained thanks to the interferometric recombination of multiple sub-apertures of a single telescope, using single mode waveguides to remove speckle noise. The SCExAO platform at the Subaru telescope hosts two instruments with such design, coupled with a spectrograph. The FIRST instrument operates in the Visible (600-800nm, R~400) and is based on pupil remapping using single-mode fibers. The GLINT instrument works in the NIR (1450-1650nm, R~160) and is based on nulling interferometry. We present here how these photonic instruments have the unique capability to simultaneously do high contrast imaging and be included in the wavefront sensing architecture of SCExAO.
The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument is a high-contrast imaging system installed at the 8-m Subaru Telescope on Maunakea, Hawaii. Due to its unique evolving design, SCExAO is both an instrument open for use by the international scientific community, and a testbed validating new technologies, which are critical to future high-contrast imagers on Giant Segmented Mirror Telescopes (GSMTs). Through multiple international collaborations over the years, SCExAO was able to test the most advanced technologies in wavefront sensors, real-time control with GPUs, low-noise high frame rate detectors in the visible and infrared, starlight suppression techniques or photonics technologies. Tools and interfaces were put in place to encourage collaborators to implement their own hardware and algorithms, and test them on-site or remotely, in laboratory conditions or on-sky. We are now commissioning broadband coronagraphs, the Microwave Kinetic Inductance Detector (MKID) Exoplanet Camera (MEC) for high-speed speckle control, as well as a C-RED ONE camera for both polarization differential imaging and IR wavefront sensing. New wavefront control algorithms are also being tested, such as predictive control, multi-camera machine learning sensor fusion, and focal plane wavefront control. We present the status of the SCExAO instrument, with an emphasis on current collaborations and recent technology demonstrations. We also describe upgrades planned for the next few years, which will evolve SCExAO —and the whole suite of instruments on the IR Nasmyth platform of the Subaru Telescope— to become a system-level demonstrator of the Planetary Systems Imager (PSI), the high-contrast instrument for the Thirty Meter Telescope (TMT).
FIRST (Fibered Imager foR a Single Telescope instrument) is an instrument that enables high contrast imaging and spectroscopy, thanks to a unique combination of sparse aperture masking, spatial filtering by single-mode waveguides and cross-dispersion in the visible. In order to increase the instrument’s stability and sensitivity, we proposed a new series of photonic beam combiners. The idea is to achieve phase modulation inside an optical chip and get rid of external delay lines, and improve the transmission by using novel techniques that will allow for beam combination in 3D, avoiding planar X-crossings and large bending radii observed in planar integrated optics instruments, between first and last inputs to combine, when the inputs separation is large (i.e. in 9 telescopes beam combiners). In a previous paper [4] we presented first prototypes of beam combiners for FIRST/SUBARU 9T. Planar 2D concepts were studied, but transmission was low due to the high number of crossings and the sharp bending angles needed to achieve beam combination within the length of the wafer. In this paper we will present our recent results on improved designs concerning: A) A hybrid Lithium-Niobate active beam splitter and phase modulator (9T, 1x8), coupled to a passive glass beam combiner (72x36, by pairs). B) A full passive device (5T splitter+beam combiner) and C) a narrow 5T splitter + phase modulator based on lithium niobate, to reduce the bending losses and optimize the overall transmission once coupled to the passive combiner. A comparative analysis of different performances will be presented.
FIRST, the Fibered Imager foR a Single Telescope, is a spectro-imager using single-mode fibers for pupil remap- ping, allowing measurements beyond the telescope diffraction limit. Integrated on the Subaru Coronagraphic Extreme Adaptive Optics instrument at the Subaru Telescope, it benefits from a very stable visible light wave- front allowing to acquire long exposure and operate on significantly fainter sources than previously possible. On-sky results demonstrated the ability of the instrument to detect stellar companions separated 43mas in the case of the Capella binary system. A similar approach on an extremely large telescope would offer unique scientific opportunities for companion detection and characterization at very high angular resolution.
FIRST (Fibered Imager foR a Single Telescope instrument) is a post-AO instrument that enables high contrast imaging and spectroscopy at spatial scales below the diffraction limit. FIRST achieves sensitivity and accuracy by a unique combination of sparse aperture masking, spatial filtering by single-mode fibers and cross-dispersion in the visible. The telescope pupil is divided into sub-pupils by an array of microlenses, coupling the light into single-mode fibers. The output of the fibers are rearranged in a non redundant configuration, allowing the measurement of the complex visibility for every baseline over the 600-900 nm spectral range. A first version of this instrument is currently integrated to the Subaru Extreme AO bench (SCExAO). This paper focuses on the on-going instrument upgrades and testings, which aim at increasing the instrument’s stability and sensitivity, thus improving the dynamic range. FIRSTv2’s interferometric scheme is based on a photonic chip beam combiner. We report on the laboratory characterization of two different types of 5-input beam combiner with enhanced throughput. The interferometric recombination of each pair of sub-pupils is encoded on a single output. Thus, to sample the fringes we implemented a temporal phase modulation by pistoning the segmented mirrors of a Micro-ElectroMechanical System (MEMS). By coupling high angular resolution and spectral resolution in the visible, FIRST offers unique capabilities in the context of the detection and spectral characterization of close companions, especially on 30m-class telescopes.
The segmented pupil experiment for exoplanet detection (SPEED) facility aims to improve knowledge and insight into various areas required for gearing up high-contrast imaging instruments adapted to the unprecedented high angular resolution and complexity of the forthcoming extremely large telescopes (ELTs). SPEED combines an ELT simulator, cophasing optics, wavefront control and shaping with a multi-deformable mirror (DM) system, and optimized small inner-working angle (IWA) coronagraphy. The fundamental objective of the SPEED setup is to demonstrate deep contrast into a dark hole optimized for small field of view and very small IWA, adapted to the hunt of exoplanets in the habitable zone around late-type stars. SPEED is designed to implement an optimized small IWA coronagraph: the phase-induced amplitude apodization complex mask coronagraph (PIAACMC). The PIAACMC consists in a multi-zone phase-shifting focal plane mask (FPM) and two apodization mirrors (PIAA-M1 and PIAA-M2), with strong manufacturing specifications. Recently, a first-generation prototype of a PIAACMC optimized for the SPEED facility has been designed and manufactured. The manufacturing components exhibit high optical quality that meets specifications. In this paper, we present how these components have been characterized by a metrological instrument, an interferential microscope, and then we show what is yielded from this characterization for the FPM and the mirrors. Eventually, we discuss the results and the perspectives of the implementation of the PIAACMC components on the SPEED setup.
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.