The Evanescent Wave Coronagraph (EvWaCo) exploits the frustration of the total internal reflection (FTIR) between a prism and a lens put in contact. The starlight is transmitted through the contact area while the light from the companion is reflected. An EvWaCo prototype, equipped with an adaptive optics (AO) system, will be installed at the 2.4m Thai National Telescope as an on-sky demonstrator of the EvWaCo mask’s achromatic capabilities while testing new AO control techniques. To characterize the Extreme Adaptive Optics System (XAO) for this prototype, we developed a bench equipped with a DM192 ALPAO deformable mirror, a 15×15 sub-apertures Shack-Hartmann wavefront sensor (SH-WFS), and a two-track phase plate simulating an average seeing of 1.4" at the Thai National Telescope, and the best seeing at 1.00". Following our previous communications on the characterization of the DM and the phase plate, we present how we calibrate the sensor for the WFS and the interaction matrix. This paper presents preliminary results obtained from experiments after closing the loop using a leaky integrator.
The Evanescent Wave Coronagraph uses a focal plane mask comprising a lens and a prism placed in contact so that frustrated total internal reflection can occur - the principle governing starlight attenuation. This type of Lyot coronagraph has three main capabilities: i) the mask adapts itself to the wavelength, ii) the size of the mask is adjustable by pressure adjustment, and iii) both the light coming from the star and companion can be collected simultaneously. Previous experimental results, obtained without adaptive optics and in unpolarized light, showed a raw contrast of 10−4 at 3 λ/D in the I-band and at 4 λ/D in the R-band. Its performance has been limited so far by uncorrected residual aberrations of the optical bench that generate speckles close to the inner working angle. To study the mask performances close to the diffraction limit and compare them with theoretical models, a deformable mirror is installed in the optical path of the testbed to perform wavefront correction. In this work, we report the results obtained in the laboratory using this upgraded setup. We show the preliminary results of correcting the non-common path aberrations using the scientific camera as the wavefront sensor and compare them with expected theoretical performances. The corrections are applied after finding the optimal commands that maximize the variance at the detector plane.
The Evanescent Wave Coronagraph (EvWaCo) is a type of Lyot coronagraph that uses an achromatic focal plane mask comprising a lens and a prism in contact. The National Astronomical Research Institute of Thailand (NARIT) plans to install an EvWaCo prototype equipped with an adaptive optics system (AO) to correct the aberrated wavefront in real-time at the unused left Nasmyth port of the Thai National telescope. To prepare for this installation, a large adapter with a diameter of 1.3 m and twelve carbon fiber poles serve as the supporting beams to hold the prototype. This work focuses on the mechanical design and testing of the large adapter, considering the prototype requirements and installation limitations. In particular, mechanical deformations and stress distributions are analyzed under survival conditions. The maximum weight of the prototype is 200 kg, and a folding mirror installed in a translation stage is placed inside the large adapter. The structural optimization uses the finite element method to deal with the constraints and ensures a high performance. The carbon fiber poles comprise carbon fiber-reinforced polymer (CFRP) that reduce the weight by approximately 30% compared to an all-aluminum structure. Each carbon fiber pole weighs about 1.75 kg, and our testing results show that it can support up to eight times the prototype's weight. The epoxy adhesive, used to join different materials, can withstand a pull-out strength of up to three times the prototype's weight. The installation of this adapter is expected to start by the end of 2024.
The Fourier Transform Spectrograph (FTS) stands as a powerful tool for astronomers in characterizing the composition of celestial bodies through their emitted light. In this study, we introduce the development and initial performance evaluation of a fiber-fed FTS, specifically tailored for solar observations within the 600-1000 nm wavelength range. To improve measurement precision, we integrated a stabilized He-Ne laser as a metrology wavelength source. This setup generates a monochromatic interferogram in parallel with the scientific interferogram, allowing for adaptive correction of the instrument's non-linear scan characteristics that affect the phase information of the scientific interferogram. For wavelength calibration, we employed well-defined oxygen (O2) lines as a reference. The comparison of the solar spectrum measured with our system against a simulated model showed good agreement affirming the system's efficacy. Additionally, we discuss the wavelength calibration using O2 lines in the telluric region, offering insights into the system's repeatability. The analysis of the Fe-I absorption line within these lines further enabled us to determine the Sun's rotational velocity.
The National Astronomical Research Institute of Thailand, together with the Institut d’Optique Graduate School and Centre de Researche Astrophysique de Lyon, has been developing the Evanescent Wave Coronagraph (EvWaCo) a new kind of Lyot coronagraph that uses a lens and prism placed in contact as its focal plane mask. By the principle of frustrated total internal reflection, EvWaCo enables an achromatic rejection and ability to collect the light from the star and the companion. An EvWaCo prototype equipped with adaptive optics will be installed at the Thai National Telescope as an on-sky demonstrator. This demonstrator will work on a 1.2 × 0.8 m2 elliptical sub-aperture of the Thai National Telescope to reach a raw contrast of 10−4 at 3λ/D over the wavelength range [600 nm, 900 nm]. The completed optical design contains all the essential light path channels in high contrast imaging fitted inside a 960 mm×960 mm optical breadboard, namely the guiding camera channel, companion channel, star channel, and wavefront sensing channel. We also show the results of the tolerancing and straylight analysis.
The Fourier transform spectrograph (FTS) is one important tool that has been used to analyze and characterize the radiated energy distribution of the stellar objects through an atmosphere. Most of the current spectrographs were installed at the telescope focal plane of the telescope, which required the space and complexity of alignments. The implementation of a fiber to feed the light from the telescope has been implemented to overcome those limitations. However, a small flux due to the single point field of view becomes a main challenge of this system. In this work, we report the development of the laboratory prototype of a fiber-fed FTS by using off-the-shelf components specifically designed for the Thai National Telescope (TNT). The method used to process the data relies on the cubic spline interpolation for resampling of both scientific and metrology interferograms and producing the spectrum from the raw measurements. The current maximum optical path difference is about 30 mm with an achievable spectral resolving power higher than 19,000 based on the instrument line shape of the system. The results obtained by concentrating the Sun light with the signal-to-noise-ratio (SNR) greater than 20 are presented. We also present the preliminary results of the low flux detection from a dim halogentungsten source comparable to the magnitude of a bright star in the order of a few nano-watts. The implementation of a phase-lock amplifier has been investigated to detect the signal and improve the signal-to-noise-ratio of the spectrum.
The Center for Optics and Photonics of the National Astronomical Research Institute of Thailand, together with the Institut d’Optique Graduate School and the Centre de Recherche Astrohpysique de Lyon (CRAL), is currently developing the Evanescent Wave Coronagraph (EvWaCo). The coronagraph relies on the tunneling effect to produce a fully achromatic focal plane mask (FPM) with an adjustable size. The full instrument comprises a coronagraph and adaptive optics system that will be mounted on the Thai National Telescope and is specified to reach a raw contrast of 10−4 at an inner working angle of 3 Airy radii. The coronagraph will be used to perform high contrast observations of stellar systems during on-sky observations over the spectral domain [600 nm, 900 nm]. In this paper, we present the opto-mechanical design of the EvWaCo prototype and the performance measured in laboratory conditions. We also discuss the potential applications for space-based observations and the development plan under this project in the next five years.
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