This paper presents a novel platform for the efficient analysis, design, and optimization of ideal single-ended Class-E power amplifiers (PAs). It employs a comprehensive time-domain analytical model, which extends the conventional design space by incorporating variable duty cycles, variable voltage switching (VVS), and variable derivative voltage switching (VDS), enabling precise evaluation of key performance parameters such as harmonic efficiency, maximum output power capability, maximum operating frequency, and device stress. To facilitate practical design verification, an open-source, GUI-based CAD tool has been developed, providing researchers with an accessible and interactive environment for analysis and validation. In addition, a Python-based global optimization algorithm is integrated into the framework to automate component selection and enhance design robustness, particularly in scenarios involving finite DC-feed inductance. The accuracy and applicability of the proposed methodology are validated through nonlinear harmonic balance (HB) simulations. The results confirm the model’s ability to predict system behavior with high fidelity, making it a valuable resource for both academic and industrial design applications.

Mctamatcrials and mctasurfaccs hold significant promise for space applications due to their compactness and lightweight characteristics. These devices use nanostructures embedded in their flat surfaces to manipulate the electromagnetic field for various purposes. Among their potential applications, metalenses stand out for their prospective role in the next generation of optical instruments deployed in space. Specifically, they offer considerable advantages for free space optical and quantum communications terminals. In intersatellite free space optical communication links, transmitter pointing errors degrade the performance of the link. Nevertheless, optimizing the shape of the transmitted beam through a metalens can improve the communication link performance. In this study, we delve into the application of metalenses for shaping laser beams in intersatellite optical communication scenarios. We present the preliminary design of the metalens and analyze its performance through numerical simulations, analyzing its feasibility and potential in space-based optical communications.

Purpose: To assesses the link between the in vitro optical properties of the PODFGF multifocal intraocular lens (IOL) and its visual acuity (VA) clinical performance. Setting: The study was conducted at TUDelft (NL), ULiege (BE), the Rothschild Institute (FR), and Beaver-Visitec International (BE). Design: The study analyzed 3 powers of the PODFGF IOL. The in vitro imaging quality was assessed using modulation transfer function (MTF) frequency sweep and through-focus MTF. Multiple figures of merit (FOMs), including MTF at 25-50-100 LP/mm, MTFa, and Strehl ratio, were extracted. Data acquisitions followed 2 ISO norms in green and white light conditions. The correlation with patients’ clinical VA was evaluated. Methods: The methodology had 2 parts: first, characterizing the in vitro properties of the IOL using FOMs, such as MTF, MTFa, and Strehl ratio, with multiple power samples (6 to 35 diopters). The second part analyzed the VA of 413 eyes implanted with FINEVISION-HP (PODFGF). Over 2 years, subjective refraction, uncorrected distance VA, corrected distance VA, uncorrected intermediate VA, distance-corrected intermediate VA, uncorrected near VA, distance-corrected near VA, defocus curve, photopic and mesopic contrast sensitivity, and rotational stability were analyzed. Results: The correlation between in vitro MTFa evaluated from the experimental data on IOLs and the clinical VA performed on implanted patients leads to an accurate prediction of vision capabilities after surgery. Conclusions: This study clinically demonstrates on a large patient cohort that MTFa complements single-frequency MTFs and establishes a mathematical link between MTF at 50 LP/mm, MTFa, and VA. In addition, it connects the 2 ISO model-eye standards and highlights the link between green and white light measurements in accurately predicting VA.

The Ultraviolet Imager (UVI) is one of the instruments of the ESA-CAS Solar wind Magnetosphere Ionosphere Link Explorer (SMILE) joint mission to image Earth's northern auroral regions over the 160-180 nm UV waveband with a 10° × 10° field of view. The UV light is guided to the detector with four thin film-coated mirrors that ensure most of the signal filtering, crucial to achieve a high out-of-band rejection and limit contributions from solar diffusion, dayglow and unwanted atomic spectral lines. In this paper, we present the design and performances of the spectrally selective reflective coating, which is based on an interferential MgF2/LaF3 multilayer stack deposited by ion-assisted electron-beam evaporation. Its peak reflectivity is above 85 % and with an adjustable central wavelength within 1 nm, whereas the out-of-band reflectivity between 120 nm and 155 nm and between 200 nm and 1100 nm remains below 6 % on average. The coating has been space qualified (thermal cycling under vacuum, radiations, UV exposure...) and shows stable performances in conditions representative of the instrument operation environment.

Third-generation gravitational wave detectors will use large mirrors isolated from seismic motion at low frequency, and also cooled down to cryogenic temperatures. To fulfil these two specifications, the E-TEST project explores the possibility of using a purely non-contact radiative cooling strategy. Based on cooling predictions, the paper includes a detailed design of the cryostat and the assembly procedure. A test campaign demonstrated that the proposed strategy succeeded in bringing the temperature of a [Figure presented] dummy mirror down to [Figure presented] in 19 days. These encouraging results are paving the way toward a fully radiative approach for cooling the mirrors of the future Einstein Telescope.

Context. The extreme ultraviolet High-Resolution Imager (HRI_EUV) of the Extreme Ultraviolet Imager (EUI) telescope on board Solar Orbiter observes the solar corona in an ∼5 Å wide passband near 174 Å with unprecedented high spatial resolution. Aims. We aim to perform radiometric cross-calibration of the HRI_EUV and the Atmospheric Imaging Assembly (AIA) telescope in order to allow further mutual analyses of the observational data. Methods. We applied a differential emission measure analysis using quasi-simultaneous images taken in seven spectral channels -HRI_EUV and six channels of AIA -and compared the real and the simulated images. Results. The comparison suggests that the real HRI_EUV images have ~40% larger signal than the simulated images predicted by the differential emission measure analysis. Conclusions. With our method we cannot conclude which instrument has errors in the absolute calibration, as it can be the case for either of them or both of them simultaneously, but to a lesser degree. However, in order to improve the accuracy of simultaneous data analysis, one needs to take this discrepancy into account. We see that introduction of the HRI_EUV signal into the DEM analysis modifies the warm plasma with 1 MK. The ability of the method to reproduce HRI_EUV images using only the AIA data further validates the underlying assumptions and our approach. Lastly, we believe the approach can be used as a strategy to establish a golden reference of contemporary EUV imagers.

One of the most ambitious goals of modern astronomy is to uncover signs of extraterrestrial biological activity, primarily achieved through spectroscopic analysis of light emitted by exoplanets to identify specific atmospheric molecules. Most exoplanets are indirectly identified through techniques like transit or Doppler shift of the host star's flux. Long-term surveys have yielded statistical insights into the occurrence rates of different planet types based on factors such as radius/mass, orbital period, and the spectral type of the host star, initial estimates of terrestrial planets within the habitable zone have also emerged. However, the difficulty of detecting light from these exoplanets leaves much unknown about their nature, formation, and evolution. As the number of rocky exoplanets around nearby stars rises, questions about their atmospheric composition, evolutionary trajectory, and habitability increase. Direct measurement of an cxoplanct's atmospheric composition through its spectral signature in the infrared can provide answers. Measuring the infrared spectrum of these planets poses significant challenges due to the star/planet contrast and very small angular separation from their host stars. Previous research showed that space-based telescopes are mandatory, and unless large primary mirrors (>30m in diameter) can be sent into space, intcrfcrometric techniques become essential. Combining light from distant telescopes with interferometric techniques allows access to information at minimal angular separation, operating within the diffraction limit of individual telescopes. Successful demonstrations of on-ground nulling interferometry open a new era for such space-based missions. They are vital to sidestep and tackle these scientific questions. We recently initiated a new study with the European Space Agency to explore the design parameters and the performances related to an interferometric concept based on a single spacecraft and sparse multiple sub-apertures. Launch constraints are linked to the use of an Ariane 6 launch vehicle. Our parametric study covers a range of 1-4 m for the diameter of the telescope and a 10-60 m baseline. The most promising concept working in the infrared range (3-20μm) will be highlighted. This study is conducted by TUDelft in cooperation with KULeuven, CSL/ULiege, and Amos with the support of the European Space Agency.

Laser satellite communication technologies are promising next-generation communications systems, offering higher data rates, more secure links, and cost-effective operations. One of the remaining challenges to tackle for ensuring sufficient link availability is atmospheric turbulence. While turbulence effects on laser links can be partly compensated for with corrective technologies and algorithms, these methods would benefit from better knowledge of turbulence profiles on the communications channel, both for system design or real-time assistance during operations. As state-of-the-art turbulence profilers are not designed to measure profiles from a laser beam on a moving satellite, this paper proposes a line-of-sight turbulence profiling tool tailored for laser satellite communications. Speckle-based turbulence observation and reconstruction via machine learning uses surrogate learning to build a model that can reconstruct optical turbulence profiles (C_n²(h)) from a single shot measurement of a speckle pattern. In this paper, the first modeling results of this flexible approach demonstrate that eight-layer turbulence profiles can be reconstructed from simulated single speckle images of a star with less than 10% error on the Fried parameter.

The need of atmospheric information with a higher spatial and temporal resolution drives the development of small satellites and satellite constellations to complement satellite flagship missions. Since optical systems are a main contributor to the satellite size, these are the prime candidate for their miniaturization. We present here a novel optical system where the complete spectrometer part of the optical system is compressed in one flat optical element. The element consists of an array of photonic crystals which is directly placed on a detector. The photonic crystals act as optical filters with a tunable spectral transmission response. From the integrated optical signals per filter and the atmosphere model, greenhouse gas concentrations are obtained using computational inversion. We present in this article the instrument concept, the manufacturing and measurement of the photonic crystals, methods for the filter array optimization, and discuss the predicted retrieval performance for the detection of methane and carbon dioxide.

We report observations of stripe-like features in Enceladus’ plumes captured simultaneously by Cassini's VIMS-IR and ISS NAC instruments during flyby E17, with similar patterns seen in VIMS-IR data from flyby E13 and E19. These parallel stripes, inclined at approximately 16°to the ecliptic and 43°to Saturn's ring plane, appear continuous across images when projected in the J2000 frame. A bright stripe, most visible at wavelengths around 5μm, acts as the zeroth-order diffraction peak of a reflection grating with an estimated groove spacing of 0.12–2.60 mm, while adjacent stripes are attributed to higher-order diffraction peaks. We suggest that this light-dispersing phenomenon originates from an inclined periodic structure within Saturn's E ring. This structure, constrained between Saturn's G ring and Rhea's orbit, likely consists of fresh ice particles supplied by Enceladus’ plumes.