We have proposed a new method of quantum dots (QD) chip scaled package technology and developed the world-first bin-free QD micro-LED display. Experimental result shows that the wavelength derivations of red and green color of QD CSPs are under 0.6nm, which enables us to use over 95% of a blue wafer. Furthermore, the quantum yield of red ones only drops under 5% after 1000 hours to apply commercial products. From the research work, we expect that the QD μ-CSP will become the core technology to dominate future TV, home theatre, and signage markets.

Whiteboards are commonly used as a medium of instant illustration of ideas during several activities including presentations, lectures, meetings, and related others through videoconferencing systems. However, the acquisition of whiteboard contents is inhibited by issues inherent to the camera technologies, the whiteboard glossy surfaces along with other environmental issues such as room lighting or camera positioning. The contents of whiteboards are mostly invisible due to the low luminance contrast and other related color degradation problems. This article presents an account of a work aimed at extracting the whiteboard image and consequently enhancing its perceptual quality and legibility. Two different methods based on color balancing and color warping are introduced to improve the global and local luminance contrast as well as color saturation of the contents. The methods are implemented based on different general models of the videoconferencing environment for avoiding color shifts and unnaturalness of results. Our evaluations, through psycho-visual experiments, reveal the significance of the proposed method's improvements over the state of the art methods in terms of visual quality and visibility. © 2018 Society for Imaging Science and Technology. [DOI: 10.2352/J.Percept.Imaging.2018.1.1.010504]

High Dynamic Range (HDR) and Wide Color Gamut (WCG) displays require adapted color measurements analysis. In this paper, we evaluate the viewing angle dependence of the color gamut and color volume of two HDR/WCG displays, one QLED TV and one OLED TV measured using a Fourier optics viewing angle system. The analysis is made using L*a*b* color space and ICtCp color space recently proposed by Dolby laboratories. The different interests of the ICtCp color space for direct comparison of the displays is discussed.

Transparent displays allow observers to see the objects behind the displays as well as information on the displays. For this reason, transparent displays have received attention as next-generation displays. Visibility of the background objects when they are seen through the on-screen contents is very important for designers of on-screen contents as well as observers of transparent displays. In this paper, factors affecting the visibility of the seethrough objects are examined first. Each of selected factors is formulated. Finally, visibility of the see-through objects is defined as a function of the selected factors. Validity of the proposed model for visibility of the see-through objects is verified by comparing them with results from human visual experiments.

With advances in sensor technology, the availability of multispectral cameras and their use are increasing. Having more information compared to a three-channel camera has its advantages but the data must be handled appropriately. In this work, we are interested in multispectral camera characterization. We measure the camera characterization performance by two methods, by linear mapping and through spectral reconstruction. Linear mapping is used in 3-channel camera characterization and we use the same method for a multispectral camera. We also investigate whether instead of linear mapping, spectral reconstruction from the camera data improves the performance of color reproduction. The recovery of reflectance spectra is an under-determined problem and certain assumptions are required for obtaining a unique solution. Linear methods are generally used for spectral reconstruction from the camera data and are based on training on known spectra. These methods can perform well when the test data consists of a subset of the training spectra, however, their performance is significantly reduced when the test data is different. In this paper, we also investigate the role of training spectra for camera characterization. Five different spectral reflectance datasets are used for training the camera characterization models. Finally we provide a comparison between the linear mapping and spectral reconstruction methods for multispectral camera characterization and also test the camera characterization framework on hyperspectral images of natural scenes.

In order to investigate factors necessary for reproducing actual star images in a planetarium, for this article, the authors conducted a psychophysical experiment using projection stimuli generated by changing three parameters of the stars: color, luminance, and size. A reference projection pattern was designed to be faithful to the actual starry sky perceptually (rather than physically) by an experienced group with abundant astronomical observation experience. A reproduction system was constructed to project ten types of star image patterns to a planetarium dome using different parameters. Then, evaluation experiments with twenty observers were conducted. The results of the experiment indicate that the intensity of the stars was sensitive to the fidelity of the reproduction, and in either case of change (whether the star was bright or dark compared to the reference pattern), the result was a loss of fidelity. In addition, although the fidelity was improved when the size of the projected star was small, for stars that were projected larger than the reference pattern, the result was remarkably negative. As for differences in color, the evaluation results suggested that the tolerance to loss of fidelity was wide. © 2017 Society for Imaging Science and Technology. [DOI: 10.2352/J.ImagingSci.Technol.2017.61.6.060401]

Fast Radio Bursts (FRBs) are extra-galactic transient radio signals of great interest to astronomers. Due to their non-repeating random nature and short time duration (much less than one second), automatic and reliable detection of these events has been a significant challenge, with only 25 published detections since 2007. This research provides a toolset for simulation and distributed detection of FRBs based on well-known image processing techniques. Custom software was developed to simulate FRB events with unprecedented granularity based upon the currently known population of pulses, and represents them as colormapped intensity images. These images are operated on directly by a Generalized Hough transform approach, followed by pattern recognition and machine learning steps, which yields a binary classifier that is successful in detecting Fast Radio Burst pulse profiles. When compared to the computationally expensive traditional process known as de-dispersion, our approach enjoys the advantage of no need for iterative data transformation.

Preparations for the "Great American Eclipse" captivated astronomers and the general public alike. With the preparations came numerous warnings about how the eclipse could be viewed safely. There was a suggestion online that Pop-Tart® wrappers, which are made of Mylar®, can be used to create homemade eclipse glasses. Mylar® is a brand name for biaxially-oriented polyethylene terephthalate; it is a metallized plastic sheeting that reflects almost all light and also functions as an insulating material. This could be appealing to novices who don't know any better and who want to be able to look at the sun without having to buy ISO and CE certified eclipse glasses. This could potentially be dangerous if the Pop-Tart® wrappers don't filter out enough of the sun's rays to fully protect the viewer's eyes. This project ascertained the safety of Pop-Tart® wrapper eclipse glasses by comparing their transmission to the transmission of verified glasses from reputable dealers. Transmission measurements were performed with a monochromator and were plotted to compare the data. Measurement results indicate that a double-layered Pop-Tart® wrapper performs comparably with eclipse glasses in the visible range and filters more radiation in the near UV and near IR regions.

Color correction in standard images is mainly based on controlling the interaction of illuminant and reflectance and often results in a compensation of actual chromatic casts with respect to a chosen reference illuminant. Primary reference illuminants come from our reference star, the sun, whose color characteristics are of G2V star class. Visually, color correction in standard images allows us to obtain scene colors more pleasant and closer to our everyday experience. Quality of color is usually intended to please the vision system of the observer, that looks at the picture using the powerful mechanisms of visual color and contrast adjustment (color constancy), a very different tool with respect to a camera. In astrophotography this basic principle does not apply: the illuminants of the many different stars or emission nebulae are the only information we detect, while the only reflectance involved (not considering Solar System planets) is originated by dust particles producing the so called reflection nebulae. Thus, what is the meaning and the goal of color correction in astrophotography? In this paper, we try to present to the reader some points of discussion about this broad question.