Overcoming the Diffraction-Limited Spatio-Angular Resolution Tradeoff
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Journal of Interdisciplinary Science Topics Determining Distance Or
Journal of Interdisciplinary Science Topics Determining Distance or Object Size from a Photograph Chuqiao Huang The Centre for Interdisciplinary Science, University of Leicester 19/02/2014 Abstract The purpose of this paper is to create an equation relating the distance and width of an object in a photograph to a constant when the conditions under which the photograph was taken are known. These conditions are the sensor size of the camera and the resolution and focal length of the picture. The paper will highlight when such an equation would be an accurate prediction of reality, and will conclude with an example calculation. Introduction may be expressed as a tan (opposite/adjacent) In addition to displaying visual information relationship: such as colour, texture, and shape, a photograph (1.0) may provide size and distance information on (1.1) subjects. The purpose of this paper is to develop such an equation from basic trigonometric principles when given certain parameters about the photo. Picture Angular Resolution With the image dimensions, we can make an Picture Field of View equation for one-dimensional angular resolution. First, we will determine an equation for the Since l2 describes sensor width and not height, we horizontal field of view of a photograph when given will calculate horizontal instead of vertical angular the focal length and width of the sensor. resolution: Consider the top down view of the camera (2.0) system below (figure 1), consisting of an object (left), lens (centre), and sensor (right). Let d be the (2.1) 1 distance of object to the lens, d2 be the focal length, Here, αhPixel is the average horizontal field of l1 be the width of the object, l2 be the width of the view for a single pixel, and nhPixel is the number of sensor, and α be the horizontal field of view of the pixels that make up a row of the picture. -
Sub-Airy Disk Angular Resolution with High Dynamic Range in the Near-Infrared A
EPJ Web of Conferences 16, 03002 (2011) DOI: 10.1051/epjconf/20111603002 C Owned by the authors, published by EDP Sciences, 2011 Sub-Airy disk angular resolution with high dynamic range in the near-infrared A. Richichi European Southern Observatory,Karl-Schwarzschildstr. 2, 85748 Garching, Germany Abstract. Lunar occultations (LO) are a simple and effective high angular resolution method, with minimum requirements in instrumentation and telescope time. They rely on the analysis of the diffraction fringes created by the lunar limb. The diffraction phenomen occurs in space, and as a result LO are highly insensitive to most of the degrading effects that limit the performance of traditional single telescope and long-baseline interferometric techniques used for direct detection of faint, close companions to bright stars. We present very recent results obtained with the technique of lunar occultations in the near-IR, showing the detection of companions with very high dynamic range as close as few milliarcseconds to the primary star. We discuss the potential improvements that could be made, to increase further the current performance. Of course, LO are fixed-time events applicable only to sources which happen to lie on the Moon’s apparent orbit. However, with the continuously increasing numbers of potential exoplanets and brown dwarfs beign discovered, the frequency of such events is not negligible. I will list some of the most favorable potential LO in the near future, to be observed from major observatories. 1. THE METHOD The geometry of a lunar occultation (LO) event is sketched in Figure 1. The lunar limb acts as a straight diffracting edge, moving across the source with an angular speed that is the product of the lunar motion vector VM and the cosine of the contact angle CA. -
The Most Important Equation in Astronomy! 50
The Most Important Equation in Astronomy! 50 There are many equations that astronomers use L to describe the physical world, but none is more R 1.22 important and fundamental to the research that we = conduct than the one to the left! You cannot design a D telescope, or a satellite sensor, without paying attention to the relationship that it describes. In optics, the best focused spot of light that a perfect lens with a circular aperture can make, limited by the diffraction of light. The diffraction pattern has a bright region in the center called the Airy Disk. The diameter of the Airy Disk is related to the wavelength of the illuminating light, L, and the size of the circular aperture (mirror, lens), given by D. When L and D are expressed in the same units (e.g. centimeters, meters), R will be in units of angular measure called radians ( 1 radian = 57.3 degrees). You cannot see details with your eye, with a camera, or with a telescope, that are smaller than the Airy Disk size for your particular optical system. The formula also says that larger telescopes (making D bigger) allow you to see much finer details. For example, compare the top image of the Apollo-15 landing area taken by the Japanese Kaguya Satellite (10 meters/pixel at 100 km orbit elevation: aperture = about 15cm ) with the lower image taken by the LRO satellite (0.5 meters/pixel at a 50km orbit elevation: aperture = ). The Apollo-15 Lunar Module (LM) can be seen by its 'horizontal shadow' near the center of the image. -
Understanding Resolution Diffraction and the Airy Disk, Dawes Limit & Rayleigh Criterion by Ed Zarenski [email protected]
Understanding Resolution Diffraction and The Airy Disk, Dawes Limit & Rayleigh Criterion by Ed Zarenski [email protected] These explanations of terms are based on my understanding and application of published data and measurement criteria with specific notation from the credited sources. Noted paragraphs are not necessarily quoted but may be summarized directly from the source stated. All information if not noted from a specific source is mine. I have attempted to be as clear and accurate as possible in my presentation of all the data and applications put forth here. Although this article utilizes much information from the sources noted, it represents my opinion and my understanding of optical theory. Any errors are mine. Comments and discussion are welcome. Clear Skies, and if not, Cloudy Nights. EdZ November 2003, Introduction: Diffraction and Resolution Common Diffraction Limit Criteria The Airy Disk Understanding Rayleigh and Dawes Limits Seeing a Black Space Between Components Affects of Magnitude and Color Affects of Central Obstruction Affect of Exit Pupil on Resolution Resolving Power Resolving Power in Extended Objects Extended Object Resolution Criteria Diffraction Fringes Interfere with Resolution Magnification is Necessary to See Acuity Determines Magnification Summary / Conclusions Credits 1 Introduction: Diffraction and Resolution All lenses or mirrors cause diffraction of light. Assuming a circular aperture, the image of a point source formed by the lens shows a small disk of light surrounded by a number of alternating dark and bright rings. This is known as the diffraction pattern or the Airy pattern. At the center of this pattern is the Airy disk. As the diameter of the aperture increases, the size of the Airy disk decreases. -
About Resolution
pco.knowledge base ABOUT RESOLUTION The resolution of an image sensor describes the total number of pixel which can be used to detect an image. From the standpoint of the image sensor it is sufficient to count the number and describe it usually as product of the horizontal number of pixel times the vertical number of pixel which give the total number of pixel, for example: 2 Image Sensor & Camera Starting with the image sensor in a camera system, then usually the so called modulation transfer func- Or take as an example tion (MTF) is used to describe the ability of the camera the sCMOS image sensor CIS2521: system to resolve fine structures. It is a variant of the optical transfer function1 (OTF) which mathematically 2560 describes how the system handles the optical infor- mation or the contrast of the scene and transfers it That is the usual information found in technical data onto the image sensor and then into a digital informa- sheets and camera advertisements, but the question tion in the computer. The resolution ability depends on arises on “what is the impact or benefit for a camera one side on the number and size of the pixel. user”? 1 Benefit For A Camera User It can be assumed that an image sensor or a camera system with an image sensor generally is applied to detect images, and therefore the question is about the influence of the resolution on the image quality. First, if the resolution is higher, more information is obtained, and larger data files are a consequence. -
High-Aperture Optical Microscopy Methods for Super-Resolution Deep Imaging and Quantitative Phase Imaging by Jeongmin Kim a Diss
High-Aperture Optical Microscopy Methods for Super-Resolution Deep Imaging and Quantitative Phase Imaging by Jeongmin Kim A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Engineering { Mechanical Engineering and the Designated Emphasis in Nanoscale Science and Engineering in the Graduate Division of the University of California, Berkeley Committee in charge: Professor Xiang Zhang, Chair Professor Liwei Lin Professor Laura Waller Summer 2016 High-Aperture Optical Microscopy Methods for Super-Resolution Deep Imaging and Quantitative Phase Imaging Copyright 2016 by Jeongmin Kim 1 Abstract High-Aperture Optical Microscopy Methods for Super-Resolution Deep Imaging and Quantitative Phase Imaging by Jeongmin Kim Doctor of Philosophy in Engineering { Mechanical Engineering and the Designated Emphasis in Nanoscale Science and Engineering University of California, Berkeley Professor Xiang Zhang, Chair Optical microscopy, thanks to the noninvasive nature of its measurement, takes a crucial role across science and engineering, and is particularly important in biological and medical fields. To meet ever increasing needs on its capability for advanced scientific research, even more diverse microscopic imaging techniques and their upgraded versions have been inten- sively developed over the past two decades. However, advanced microscopy development faces major challenges including super-resolution (beating the diffraction limit), imaging penetration depth, imaging speed, and label-free imaging. This dissertation aims to study high numerical aperture (NA) imaging methods proposed to tackle these imaging challenges. The dissertation first details advanced optical imaging theory needed to analyze the proposed high NA imaging methods. Starting from the classical scalar theory of optical diffraction and (partially coherent) image formation, the rigorous vectorial theory that han- dles the vector nature of light, i.e., polarization, is introduced. -
Computation and Validation of Two-Dimensional PSF Simulation
Computation and validation of two-dimensional PSF simulation based on physical optics K. Tayabaly1,2, D. Spiga1, G. Sironi1, R.Canestrari1, M.Lavagna2, G. Pareschi1 1 INAF/Brera Astronomical Observatory, Via Bianchi 46, 23807 Merate, Italy 2 Politecnico di Milano, Via La Masa 1, 20156 Milano, Italy ABSTRACT The Point Spread Function (PSF) is a key figure of merit for specifying the angular resolution of optical systems and, as the demand for higher and higher angular resolution increases, the problem of surface finishing must be taken seriously even in optical telescopes. From the optical design of the instrument, reliable ray-tracing routines allow computing and display of the PSF based on geometrical optics. However, such an approach does not directly account for the scattering caused by surface microroughness, which is interferential in nature. Although the scattering effect can be separately modeled, its inclusion in the ray-tracing routine requires assumptions that are difficult to verify. In that context, a purely physical optics approach is more appropriate as it remains valid regardless of the shape and size of the defects appearing on the optical surface. Such a computation, when performed in two-dimensional consideration, is memory and time consuming because it requires one to process a surface map with a few micron resolution, and the situation becomes even more complicated in case of optical systems characterized by more than one reflection. Fortunately, the computation is significantly simplified in far-field configuration, since the computation involves only a sequence of Fourier Transforms. In this paper, we provide validation of the PSF simulation with Physical Optics approach through comparison with real PSF measurement data in the case of ASTRI-SST M1 hexagonal segments. -
Modern Astronomical Optics 1
Modern Astronomical Optics 1. Fundamental of Astronomical Imaging Systems OUTLINE: A few key fundamental concepts used in this course: Light detection: Photon noise Diffraction: Diffraction by an aperture, diffraction limit Spatial sampling Earth's atmosphere: every ground-based telescope's first optical element Effects for imaging (transmission, emission, distortion and scattering) and quick overview of impact on optical design of telescopes and instruments Geometrical optics: Pupil and focal plane, Lagrange invariant Astronomical measurements & important characteristics of astronomical imaging systems: Collecting area and throughput (sensitivity) flux units in astronomy Angular resolution Field of View (FOV) Time domain astronomy Spectral resolution Polarimetric measurement Astrometry Light detection: Photon noise Poisson noise Photon detection of a source of constant flux F. Mean # of photon in a unit dt = F dt. Probability to detect a photon in a unit of time is independent of when last photon was detected→ photon arrival times follows Poisson distribution Probability of detecting n photon given expected number of detection x (= F dt): f(n,x) = xne-x/(n!) x = mean value of f = variance of f Signal to noise ration (SNR) and measurement uncertainties SNR is a measure of how good a detection is, and can be converted into probability of detection, degree of confidence Signal = # of photon detected Noise (std deviation) = Poisson noise + additional instrumental noises (+ noise(s) due to unknown nature of object observed) Simplest case (often -
Beat the Rayleigh Limit: OAM Based Super-Resolution Diffraction Tomography
Beat the Rayleigh limit: OAM based super-resolution diffraction tomography Lianlin Li1 and Fang Li2 1Center of Advanced Electromagnetic Imaging, Department of Electronics, Peking University, Beijing 100871, China 2 Institute of Electronics, CAS, Beijing 100190, China This letter is the first to report that a super-resolution imaging beyond the Rayleigh limit can be achieved by using classical diffraction tomography (DT) extended with orbital angular momentum (OAM), termed as OAM based diffraction tomography (OAM-DT). It is well accepted that the orbital angular momentum (OAM) provides additional electromagnetic degrees of freedom. This concept has been widely applied in science and technology. In this letter we revisit the DT problem extended with OAM, demonstrate theoretically and numerically that there is no physical limits on imaging resolution in principle by the OAM-DT. This super-resolution OAM-DT imaging paradigm, has no requirement for evanescent fields, subtle focusing lens, complicated post- processing, etc., thus provides a new approach to realize the wavefield imaging of universal objects with sub-wavelength resolution. In 1879 Lord Rayleigh formulated a criterion that a conventional imaging system cannot achieve a resolution beyond that of the diffraction limit, i.e., the Rayleigh limit. Such a “physical barrier” characters the minimum separation of two adjacent objects that an imaging system can resolve. In the past decade numerous efforts have been made to achieve imaging resolution beyond that of Rayleigh limit. Among various proposals dedicated to surpass this “barrier”, a representative example is the well-known technique of near-field imaging, an essential sub-wavelength imaging technology. Near-field imaging relies on the fact that the evanescent component carries fine details of the electromagnetic field distribution at the immediate vicinity of probed objects [1]. -
Preview of “Olympus Microscopy Resou... in Confocal Microscopy”
12/17/12 Olympus Microscopy Resource Center | Confocal Microscopy - Resolution and Contrast in Confocal … Olympus America | Research | Imaging Software | Confocal | Clinical | FAQ’s Resolution and Contrast in Confocal Microscopy Home Page Interactive Tutorials All optical microscopes, including conventional widefield, confocal, and two-photon instruments are limited in the resolution that they can achieve by a series of fundamental physical factors. In a perfect optical Microscopy Primer system, resolution is restricted by the numerical aperture of optical components and by the wavelength of light, both incident (excitation) and detected (emission). The concept of resolution is inseparable from Physics of Light & Color contrast, and is defined as the minimum separation between two points that results in a certain level of contrast between them. In a typical fluorescence microscope, contrast is determined by the number of Microscopy Basic Concepts photons collected from the specimen, the dynamic range of the signal, optical aberrations of the imaging system, and the number of picture elements (pixels) per unit area in the final image. Special Techniques Fluorescence Microscopy Confocal Microscopy Confocal Applications Digital Imaging Digital Image Galleries Digital Video Galleries Virtual Microscopy The influence of noise on the image of two closely spaced small objects is further interconnected with the related factors mentioned above, and can readily affect the quality of resulting images. While the effects of many instrumental and experimental variables on image contrast, and consequently on resolution, are familiar and rather obvious, the limitation on effective resolution resulting from the division of the image into a finite number of picture elements (pixels) may be unfamiliar to those new to digital microscopy. -
Measuring Angles and Angular Resolution
Angles Angle θ is the ratio of two lengths: R: physical distance between observer and objects [km] Measuring Angles S: physical distance along the arc between 2 objects Lengths are measured in same “units” (e.g., kilometers) and Angular θ is “dimensionless” (no units), and measured in “radians” or “degrees” Resolution R S θ R Trigonometry “Angular Size” and “Resolution” 22 Astronomers usually measure sizes in terms R +Y of angles instead of lengths R because the distances are seldom well known S Y θ θ S R R S = physical length of the arc, measured in m Y = physical length of the vertical side [m] Trigonometric Definitions Angles: units of measure R22+Y 2π (≈ 6.28) radians in a circle R 1 radian = 360˚ ÷ 2π≈57 ˚ S Y ⇒≈206,265 seconds of arc per radian θ Angular degree (˚) is too large to be a useful R S angular measure of astronomical objects θ ≡ R 1º = 60 arc minutes opposite side Y 1 arc minute = 60 arc seconds [arcsec] tan[]θ ≡= adjacent side R 1º = 3600 arcsec -1 -6 opposite sideY 1 1 arcsec ≈ (206,265) ≈ 5 × 10 radians = 5 µradians sin[]θ ≡== hypotenuse RY22+ R 2 1+ Y 2 1 Number of Degrees per Radian Trigonometry in Astronomy Y 2π radians per circle θ S R 360° Usually R >> S (particularly in astronomy), so Y ≈ S 1 radian = ≈ 57.296° 2π SY Y 1 θ ≡≈≈ ≈ ≈ 57° 17'45" RR RY22+ R 2 1+ Y 2 θ ≈≈tan[θθ] sin[ ] Relationship of Trigonometric sin[θ ] ≈ tan[θ ] ≈ θ for θ ≈ 0 Functions for Small Angles 1 sin(πx) Check it! tan(πx) 0.5 18˚ = 18˚ × (2π radians per circle) ÷ (360˚ per πx circle) = 0.1π radians ≈ 0.314 radians 0 Calculated Results -
Super-Resolution Optical Imaging Using Microsphere Nanoscopy
Super-resolution Optical Imaging Using Microsphere Nanoscopy A thesis submitted to The University of Manchester For the degree of Doctor of Philosophy (PhD) in the Faculty of Engineering and Physical Sciences 2013 Seoungjun Lee School of Mechanical, Aerospace and Civil Engineering Super-resolution optical imaging using microsphere nanoscopy Table of Contents Table of Contents ...................................................................................................... 2 List of Figures and Tables ....................................................................................... 7 List of Publications ................................................................................................. 18 Abstract .................................................................................................................... 19 Declaration ............................................................................................................... 21 Copyright Statement ............................................................................................... 22 Acknowledgements ................................................................................................. 23 Dedication ............................................................................................................... 24 1 Introduction ...................................................................................................25 1.1 Research motivation and rationale ........................................................25 1.2