Wales 247’s Post

A scheme of optical frequency thinning based on MZM modulator The optical frequency dispersion can be used as a liDAR light source to simultaneously emit and scan in different directions, and it can also be used as a multi-wavelength light source of 800G FR4, eliminating the MUX structure. Usually, the multi-wavelength light source is either low power or not well packaged, and there are many problems. The scheme introduced today has many advantages and can be referred to for reference. Its structure diagram is shown as follows: The high-power DFB laser light source is CW light in time domain and single wavelength in frequency. After passing through a modulator with a certain modulation frequency fRF, sideband will be generated, and the sideband interval is the modulated frequency fRF. The modulator uses a LNOI modulator with a length of 8.2mm, as shown in Figure b. After a long section of high-power phase modulator, the modulation frequency is also fRF, and its phase needs to make the crest or trough of the RF signal and the light pulse relative to each other, resulting in a large chirp, resulting in more optical teeth. The DC bias and modulation depth of the modulator can affect the flatness of the optical frequency dispersion. Mathematically, the signal after the light field is modulated by the modulator is: It can be seen that the output optical field is an optical frequency dispersion with a frequency interval of wrf, and the intensity of the optical frequency dispersion tooth is related to the DFB optical power. By simulating the light intensity passing through MZM modulator and PM phase modulator, and then FFT, the optical frequency dispersion spectrum is obtained. The following figure shows the direct relationship between optical frequency flatness and modulator DC bias and modulation depth based on this simulation. #Optical #photonics #semiconductor #Optics #opticalcenter #SiliconPhotonics #photodetectors #optomechanics #laser Read more: https://lnkd.in/eJzS2xP9

int main() {    // Telescope parameters    Telescope telescope(1000.0, 200.0); // Focal length = 1000 mm, Aperture = 200 mm    // Camera parameters    Camera camera(36.0, 24.0, 4000, 3000); // Sensor size = 36mm x 24mm, 4000x3000 pixels    // Simulated star positions (in mm on the sensor plane)    vector<pair<double, double>> stars = {        {10.0, 5.0},  // Star 1        {15.0, 10.0}, // Star 2        {20.0, 15.0}, // Star 3        {5.0, 20.0},  // Star 4        {30.0, 20.0}  // Star 5    };    // Capture image    camera.captureImage(stars);    // Display the captured image    camera.displayImage();    return 0; } This example provides a basic framework for modeling a telescope camera in C++. You can extend it to include more advanced features, such as image processing, advanced optics simulation, and integration with real telescope hardware for data acquisition.

Excited to share our latest publication in Optica! Our team has developed a high-performance room-temperature avalanche photodiode (APD) capable of detecting extended shortwave infrared (eSWIR) wavelengths up to 2.75 μm. This breakthrough demonstrates significant advancements in material engineering and device performance, offering potential for wide-ranging applications in remote sensing, LiDAR, and optical communications in the eSWIR region. Key highlights of the work: Innovative Materials: The APD uses an In0.22Ga0.78As0.19Sb0.81 absorber with a bandgap of 0.45 eV, combined with an Al0.9Ga0.1As0.08Sb0.92 multiplication region. This unique combination enables room-temperature operation with high sensitivity. Exceptional Performance: The device achieved a peak external quantum efficiency (EQE) exceeding 50% at the punch-through voltage (~2 μm wavelength) and a maximum multiplied EQE of over 2000% at 2 μm, with a low excess noise factor of 4.5 at a multiplication of M = 20. Reduced Operating Voltage: With a low breakdown voltage of 18.9 V, this APD design is compatible with ROIC design. This work highlights the potential of eSWIR detectors to operate efficiently at room temperature, reducing the need for cooling systems and paving the way for compact, high-sensitivity detection solutions. We are thrilled to see the possibilities this innovation brings to fields like free-space optical communications and advanced imaging technologies. Thanks to our collaborators from the University of Sheffield, Lancaster University, Heriot-Watt University, and Amethyst Research Ltd., for their contributions to this milestone achievement. Read more about our findings in Optica: https://lnkd.in/eNYNTFP4 #ResearchInnovation #Photonics #InfraredDetection #OpticalTechnology

The Rubin Observatory LSST Camera is the largest digital camera ever constructed. At about 5.5 ft (1.65 m) by 9.8 ft (3 m), it's roughly the size of a small car and weighs almost 6200 lbs (2800 kg). It is a large-aperture, wide-field optical imager capable of viewing light from the near ultraviolet to near infrared (0.3-1 μm) wavelengths. The LSST Camera is designed to provide a 3.5-degree field of view, with its 10 μm pixels capable of 0.2 arcsecond sampling for optimized pixel sensitivity vs pixel resolution. The image surface is flat with a diameter of approximately 25.2 in (64 cm). The detector format employs a mosaic of 189 16-megapixel silicon detectors arranged on 21 "rafts" to provide a total of about 3.2 gigapixels. The camera includes a filter-changing mechanism and shutter. It is positioned in the middle of the telescope where cross sectional area is constrained by optical vignetting (edge darkening) and heat dissipation must be controlled to limit lens-deforming thermal gradients in the incoming light. The LSST Camera will produce data of extremely high quality with minimal downtime and maintenance. Source : https://lnkd.in/g6aQjqrb #GigapixelGalaxy #CosmicCarCamera #RubinObservatoryRevelation #SkySurveyor #AstrolmagingRevolution #StellarSight #UniverselPixels #BeyondTheVisible #ChileanSkyChampion #SynopticSnapshot

At RAYOPS, we are pushing the boundaries of laser beam propagation simulation with our cutting-edge tool, RAY-Py. Our simulator produces high fidelity, high-resolution turbulence phase screens, offering unprecedented accuracy in wave optic simulations. Turbulence, caused by random perturbations in atmospheric density (temperature), is a major challenge for laser propagation. For those interested in observing the phenomenon, look at a distant object along a hot pavement, you will see it shimmering. Not to be confused by mirage though! Traditional wave optic simulations use low-resolution mesh grids and fewer than 10 uncorrelated phase screens over long distances, failing to accurately model the inner (cm-range) and outer (few meters) scales. RAY-Py leverages GPU calculations to enhance matrix resolution and enables beam propagation through thousands of correlated phase screens along the path. This allows for a proper representation of both inner and outer scales not only transverse to the propagation axis, but also along the path. 📹 Watch for yourself in our latest video: Correlated turbulence phase screens along a 30 m beam propagation path. Each phase screen is spaced by 1 cm, with a mesh resolution of 4096 pixels per side. This configuration aptly samples an inner scale of 2 cm and an outer scale of 3 m. RAY-Py can multiply those over kilometers without saturating the memory! Stay tuned for more updates and innovations from RAYOPS! #LaserTechnology #WaveOptics #DirectedEnergy #OpticalCommunication #LIDAR #PowerBeaming #Simulation #RAYOPS #RAYPy #Innovation #Atmosphere

RAY-Py enables high-fidelity laser propagation simulations through turbulence. Ask RAYOPS for advice if you are concerned about the impact of turbulence on your system.

✨ Excited to share our latest research on NIR beam steering! ✨ "Reprogrammable Metasurface Design for NIR Beam Steering and Active Filtering" In this work, we propose an innovative electrically tunable Au–VO₂ metasurface integrated with a photonic crystal on a SiC substrate. This design achieves: ✅ High optical and thermal efficiencies (~40% reflectance at 1.55 µm as well effective heat transfer from the source to the SiC heat sink) ✅ Broadband beam steering in the NIR range (1.4–1.7 µm) ✅ Active control of light transmittance, reflectance, and absorptance (0.75–3 µm) With its advanced heat management and binary programmability, this metasurface is a promising solution for LiDAR and active filtering applications. My warmest thanks to all the coauthors, particularly Prof. Louise Bradley, as well as to Research Ireland, and the AMBER Centre & CRANN for their support on this project. 📄 Read more here: https://lnkd.in/d4Hq47ag #Metasurface #Photonics #OpticalEngineering #LiDAR #Research

"For objects ~3 meters in size we observe from Figure 7 that object detection performance degrades from F1=0.92 for objects 20 pixels in size to F1=0.27 for objects 1 pixel in size, with a mean error of 0.09. Interestingly, the F1 score only degrades by only 5% as objects shrink from 20 to 5 pixels in size (0.15m to 0.60m #GSD). 𝐀𝐭 𝐥𝐞𝐚𝐬𝐭 𝐟𝐨𝐫 𝐜𝐚𝐫𝐬 𝐯𝐢𝐞𝐰𝐞𝐝 𝐟𝐫𝐨𝐦 𝐨𝐯𝐞𝐫𝐡𝐞𝐚𝐝, 𝐨𝐧𝐞 𝐜𝐚𝐧 𝐜𝐨𝐧𝐜𝐥𝐮𝐝𝐞 𝐭𝐡𝐚𝐭 𝐨𝐛𝐣𝐞𝐜𝐭 𝐬𝐢𝐳𝐞𝐬 𝐨𝐟 𝟓 𝐩𝐢𝐱𝐞𝐥𝐬 𝐨𝐫 𝐠𝐫𝐞𝐚𝐭𝐞𝐫 𝐲𝐢𝐞𝐥𝐝 𝐨𝐛𝐣𝐞𝐜𝐭 𝐝𝐞𝐭𝐞𝐜𝐭𝐢𝐨𝐧 𝐬𝐜𝐨𝐫𝐞𝐬 𝐨𝐟 𝐅𝟏 > 𝟎.𝟖𝟓." https://lnkd.in/dmqYnh5V

Unlock the secrets of optical density and its crucial role in advanced optical applications. Our White Paper from Edmund Optics explores OD fundamentals, its impact on light transmission, and the necessity for high OD in cutting-edge fields like microscopy and lidar. Essential for optical engineers and researchers.

Unlock the secrets of optical density and its crucial role in advanced optical applications. Our White Paper from Edmund Optics explores OD fundamentals, its impact on light transmission, and the necessity for high OD in cutting-edge fields like microscopy and lidar. Essential for optical engineers and researchers.