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Design, scientific goals, and performance of the SCExAO survey for planets around accelerating stars
Enhancing phase retrieval with domain adaptation: bridging the gap between simulations and real data
These 3D waveguide tricouplers are fabricated using the femtosecond laser direct-write technique. This process involves a tightly focused laser to modify the refractive index of a boro-aluminosilicate glass sample, creating optical waveguides. We present a rigorous optimisation of the tricouplers which includes a numerical solution to coupled-mode equations to obtain coupling coefficients and propagation constants that are used to optimise the fabrication process for the J (1.1 μm - 1.4 μm) and H (1.5 μm - 1.8 μm) wavelength bands. Furthermore, the polarisation behaviour, the wavelength behaviour and interferometric performance has been investigated to create an accurate transfer matrix of the device.
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.
To directly image and characterize exoplanets, many developments of high-contrast imaging (HCI) systems are ongoing for current ground-based telescopes as well as future extremely large telescopes and space-based telescopes. Despite recent developments in HCI, the contrast of the HCI systems is limited by non-common path aberrations (NCPAs) and residual errors of the adaptive optics (AO) system. In order to overcome these limitations, HCI systems need focal plane wavefront sensing and control (FPWFS&C) techniques.
We present the implementation of two FPWFS&C techniques, electric field conjugation (EFC) and spatial linear dark field control (LDFC), on the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument. First, we generate a half-dark hole in the focal plane image using EFC. Once the bright field and dark field (dark hole) have been established by EFC, as a second step, we deploy spatial LDFC to maintain the contrast of the half-dark hole generated by EFC. We could also use EFC to preserve the contrast of the dark hole, but it requires field modulation, which interferes with the science image acquisition. Because of this reason, we use spatial LDFC as an alternative way to maintain the contrast without modulation.
In actual demonstrations, we obtained a dark hole contrast of ∼2×10−7 with a classical Lyot coronagraph of 114 mas diameter, at a 1550 nm wavelength using EFC. This result is the first EFC implementation and the deepest contrast obtained on the SCExAO testbed. Using spatial LDFC, we also ideally removed focal plane speckles generated by static phase error and restored the initial contrast. Our results provide a promising path forward to generating the high-contrast dark hole using EFC and stabilizing the contrast of the dark hole without interrupting the science acquisition using spatial LDFC.
Linearized Analytical Phase Diversity : towards lab and on-sky demonstration on the Subaru Telescope
SCExAO, an instrument with a dual purpose: perform cutting-edge science and develop new technologies
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