Vortex phase masks have been shown to be an efficient means to reduce the blinding stellar light in high-contrast imaging instruments. Once placed at the focal plane of the telescope, the helical phase ramp of a vortex phase mask diffracts the light of a bright on-axis source outside the re-imaged telescope pupil, while transmitting the light of a faint off-axis companion nearly unaffected. The Annular Groove Phase Mask (AGPM) is a broadband metasurface implementation of a vector vortex phase mask using the artificial birefringence of a circular subwavelength grating etched onto a diamond substrate. To date, the AGPM design has been optimized using rigorous coupled-wave analysis (RCWA), which is a valid tool to simulate periodic straight gratings. However, we have now reached a performance level where the curvature of the grating lines at the center becomes a limiting factor. Here, we use a finite-difference time-domain (FDTD) method to correctly describe the AGPM performance, including the effect of the curved grating close to its center. We confirm the validity of this simulation framework by comparing its predictions with experimental results obtained on our infrared coronagraphic test bench, and we show that RCWA fails at reproducing correctly the central AGPM performance, confirming the need for a full 3d simulation tool such as FDTD. Finally, we use FDTD to optimize the grating parameters at the AGPM center, and conclude with a new optimal design.

@en

With the advent of 30- to 40-m class ground-based telescopes in the mid-2020s, direct imaging of exoplanets is bound to take a new major leap. Among the approved projects, the Mid-infrared Extremely Large Telescope (ELT) Imager and Spectrograph (METIS) instrument for the ELT holds a prominent spot; by observing in the mid-infrared regime, it will be perfectly suited to study a variety of exoplanets and protoplanetary disks around nearby stars. Equipped with two of the most advanced coronagraphs, the vortex coronagraph and the apodizing phase plate, METIS will provide high-contrast imaging (HCI) in L-, M- and N-bands, and a combination of high-resolution spectroscopy and HCI in L- and M-bands. We present the expected HCI performance of the METIS instrument, considering realistic adaptive optics residuals, and investigate the effect of the main instrumental errors. The most important sources of degradation are identified and realistic sensitivity limits in terms of planet/star contrast are derived.@en

This article [J. Astron. Telesc. Instrum. Syst. 6(3), 035005 (Sep 24, 2020) DOI: 10.1117/1.JATIS.6.3.035005] as originally published omitted three authors as well as three references. The omitted authors produced the Apodizing Phase Plate design used in the paper’s end-to-end simulations. This contribution was provided by David Doelman, Emiel Por, and Frans Snik, all of Leiden University. They have been added as authors on the paper, as listed above. The following acknowledgment also has been added to the published paper: “The research of DD and FS leading to these results has received funding from the European Research Council under ERC Starting Grant agreement 678194 (FALCONER).” Additionally, three references were omitted from the paper when it was published. They are listed below: 61. G. Otten et al., “Performance characterization of a broadband vector Apodizing Phase Plate coronagraph,” Opt. Express 22(24), 30287 (2014). 62. G. Otten et al., “The vector apodizing phase plate coronagraph: prototyping, characterization and outlook,” Proc. SPIE 9151, 91511R (2014). 63. E. Por, “Optimal design of apodizing phase plate coronagraphs,” Proc. SPIE 10400, 104000V (2017). All versions of the article were corrected on 15 October 2020. The article appears correctly in print.

@en