van Cittert-Zernike Theorem

Slides:



Advertisements
Similar presentations
Interferometry Jack Replinger Observational Cosmology Lab Professor Peter Timbie University of Wisconsin-Madison Interferometry uses an array of small.
Advertisements

A Crash Course in Radio Astronomy and Interferometry: 2
Principles of Interferometry I
Fourier Transform – Chapter 13. Image space Cameras (regardless of wave lengths) create images in the spatial domain Pixels represent features (intensity,
Dr. Daniel F.V. James MS B283, PO Box 1663, Los Alamos NM Invited Correlation-induced spectral (and other) changes Daniel F. V. James, Los Alamos.
NASSP Masters 5003F - Computational Astronomy Lecture 13 Further with interferometry – Resolution and the field of view; Binning in frequency and.
Overview from last week Optical systems act as linear shift-invariant (LSI) filters (we have not yet seen why) Analysis tool for LSI filters: Fourier transform.
Radio `source’ Goals of telescope: maximize collection of energy (sensitivity or gain) isolate source emission from other sources… (directional gain… dynamic.
Sampling Pixel is an area!! – Square, Rectangular, or Circular? How do we approximate the area? – Why bother? Color of one pixel Image Plane Areas represented.
PHY 1371Dr. Jie Zou1 Chapter 37 Interference of Light Waves.
Optics in Astronomy - Interferometry - Oskar von der Lühe Kiepenheuer-Institut für Sonnenphysik Freiburg, Germany.
2010 CASS Imaging Workshop Narrabri, NSW. Fundamentals of Radio Interferometry Rick Perley, NRAO/Socorro.
1 Synthesis Imaging Workshop Error recognition R. D. Ekers Narrabri, 14 May 2003.
3: Interference, Diffraction and Polarization
Chapter 37 Wave Optics. Wave optics is a study concerned with phenomena that cannot be adequately explained by geometric (ray) optics.  Sometimes called.
1 W14D1: EM Waves, Dipole Radiation, Polarization and Interference Today’s Reading Course Notes: Sections 13.8, 13.10,
Interferometry Basics
14 Sep 1998R D Ekers - Synth Image Workshop: INTRODUCTION 1 Synthesis Imaging Workshop Introduction R. D. Ekers 14 Sep 1998.
Separable functions University of Illinois at Chicago ECE 427, Dr. D. Erricolo University of Illinois at Chicago ECE 427, Dr. D. Erricolo A function of.
The Wave Nature of Light. Waves So far we have learned about mechanical waves in slinkies, strings, and air. Sound waves are mechanical waves. Mechanical.
Wireless and Mobile Computing Transmission Fundamentals Lecture 2.
Interferometry Discuss Group & Python Tutorial Adam Leroy & Scott Schnee (NRAO) February 28, 2014.
Tutorial on Computational Optical Imaging University of Minnesota September David J. Brady Duke University
Fourier relations in Optics Near fieldFar field FrequencyPulse duration FrequencyCoherence length Beam waist Beam divergence Focal plane of lensThe other.
1 ATNF Synthesis Workshop 2001 Basic Interferometry - II David McConnell.
1 Waves 10 Lecture 10 Wave propagation. D Aims: ëFraunhofer diffraction (waves in the “far field”). > Young’s double slits > Three slits > N slits and.
Lecture Nine: Interference of Light Waves: I
NASSP Masters 5003F - Computational Astronomy Lecture 12: The beautiful theory of interferometry. First, some movies to illustrate the problem.
NASSP Masters 5003F - Computational Astronomy Lecture 14 Reprise: dirty beam, dirty image. Sensitivity Wide-band imaging Weighting –Uniform vs Natural.
Figure 28-1 Constructive and Destructive Interference
Tutorial on Computational Optical Imaging University of Minnesota September David J. Brady Duke University
NASSP Masters 5003F - Computational Astronomy Lecture 12 Complex numbers – an alternate view The Fourier transform Convolution, correlation, filtering.
© 2012 Pearson Education, Inc. { Chapter 35 Interference.
NASSP Masters 5003F - Computational Astronomy Lecture 16 Further with interferometry – Digital correlation Earth-rotation synthesis and non-planar.
Lecture 14. Radio Interferometry Talk at Nagoya University IMS Oct /43.
Lens to interferometer Suppose the small boxes are very small, then the phase shift Introduced by the lens is constant across the box and the same on both.
1 ATNF Synthesis Workshop 2003 Basics of Interferometry David McConnell.
Introduction: Vectors and Integrals. Vectors Vectors are characterized by two parameters: length (magnitude) direction These vectors are the same Sum.
Relevance of a Generic and efficient "E-field Parallel Imaging Correlator”(EPIC) for future radio telescopes Nithyanandan Thyagarajan (ASU, Tempe) Adam.
Chapters 36 & 37 Interference and Diffraction. Combination of Waves In general, when we combine two waves to form a composite wave, the composite wave.
Mathematical groundwork I: Fourier theory
Details: Gridding, Weight Functions, the W-term
Course Details Fundamentals of Radio Interferometry NASSP 2016
Chapter 11 Fourier optics
Young Fourier III & Ψ.
Chapter 25 Wave Optics.
Correlators ( Backend System )
Wave Optics Chapter 27.
You should have been reading Chapter 35 (interference)
A Brief Introduction To Interferometry
Limitations of Single Dish Astronomy
Positional Astronomy Chapter 3 Fundamentals of Radio Interferometry
CLEAN: Iterative Deconvolution
Radio Interferometry Jeff Kenney.
3. SR interferometer.
Telescopes and Images.
Wide-field imaging Max Voronkov (filling up for Tim Cornwell)
Young’s double slit experiment & Spatial coherence of light
Coherence 1 1.
Two sources S1 and S2 oscillating in phase emit sinusoidal waves.
Young’s double slit experiment & Spatial coherence of light
Observational Astronomy
Two-beam interference:
Goals of telescope: Radio `source’
Diffraction.
WAVES John Parkinson St. Brendan’s Sixth Form College John Parkinson
Coherence (chapter 8) Coherence theory is the study of correlation that exist between different parts of a light field Two type of coherences: Temporal.
Fundamentals of Radio Interferometry
PHYS 408 Applied Optics (Lecture 19)
Chapter 11 Fourier optics
Presentation transcript:

van Cittert-Zernike Theorem Fundamentals of Radio Interferometry, Section 4.5 Griffin Foster SKA SA/Rhodes University NASSP 2016

What is the Fourier transform of the sky? NASSP 2016

Important Points: The van Cittert-Zernike Theorem is at the heart of aperture synthesis. Fourier transforms are essential to synthesis imaging. NASSP 2016

van Cittert-Zernike Theorem Simply stated: there exists a relationship between the mutual spatial coherence function and the sky intensity distribution. This relationship can be approximated as: The mutual spatial coherence function (visibilities) and the sky intensity distribution (image of the sky) are Fourier pairs NASSP 2016

Mutual Spatial Coherence Function Given a signal, in our case the electric field (E), the mutual spatial coherence function for two point in space (r1, r2) is the time-averaged correlation of the signal measured at each point. The mutual spatial coherence function is a correlation between two points in space, in our case, two radio antennas. NASSP 2016

Thus, the Visibility function is in the uvw-space. Mutual Spatial Coherence Function In aperture synthesis we call the mutual spatial coherence function the Visibility function. Instead of the absolute position of each point we instead use the spatial difference Thus, the Visibility function is in the uvw-space. NASSP 2016

Sky Intensity Distribution The sky intensity distribution is a fancy name for what the sky looks like at a given frequency ν. For the van Cittert-Zernike theorem we use the direction-cosine reference frame. NASSP 2016

NASSP 2016

Hand-wavy Derivation Image of the Sky NASSP 2016

Hand-wavy Derivation 1. Given a source far away, such as an astronomical object, the electric field from that source can be considered a plane wave (i.e. the source is in the far-field). NASSP 2016

Hand-wavy Derivation 2. We measure the electric field at two spatially separated points r1, r2. NASSP 2016

Hand-wavy Derivation 3. For any two point in space in which we measure the electric field there is a phase difference between the measured signals which results in a constructive or destructive interference depending on the relative position of the two measurement points and the observing frequency. NASSP 2016

Hand-wavy Derivation Geometric Delay: Phase: 4. For any relative spatial difference there is this phase difference is constant. NASSP 2016

Hand-wavy Derivation Geometric Delay: Fringe Pattern Phase: 5. This fringe pattern results in a sinusoidal wave in the 2-D mutual spatial coherence space. NASSP 2016

Hand-wavy Derivation Visibility Function Image of the Sky 6. The Fourier transform of a sinusoidal function is a delta function at a particular position, i.e. the source of the electric field in the sky. NASSP 2016

See Interferometry and Synthesis in Radio Astronomy (TMS) Chapter 14 Real Derivation See Interferometry and Synthesis in Radio Astronomy (TMS) Chapter 14 NASSP 2016

The more complete van Cittert-Zernike Theorem Our 2-D Fourier relation between the visibility function and the sky is an approximate form of the van Cittert-Zernike theorem: A more complete version of van Cittert-Zernike is: Unfortunately, this is not a 2-D Fourier relation. NASSP 2016

Approximations to reduce to a 2D Fourier transform Small Angle/Narrow Field of View Approximation: From positional astronomy, the sky instensity is distributed on the celestial (unit) sphere such that for any position (l,m,n): If we are only interested in a small area on the sky then the extant of (l,m) is small: Then the van Cittert-Zernike theorem can be approximated as: NASSP 2016

Approximations to reduce to a 2D Fourier transform Delay term/w-term Approximation: If our visibility sampling is approximately on a plane, or again we are only interested in a narrow field of view then the so-called w-term can be seen as a constant delay term, with a simple correction w=0. NASSP 2016

What is the Fourier transform of the sky? NASSP 2016

NASSP 2016