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Coded aperture mask for gamma camera (for SPECT)

Coded Apertures or Coded-Aperture Masks are grids, gratings, or other patterns of materials opaque to various wavelengths of electromagnetic radiation. The wavelengths are usually high-energy radiation such as X-rays and gamma rays. By blocking radiation in a known pattern, a coded "shadow" is cast upon a plane. The properties of the original radiation sources can then be mathematically reconstructed from this shadow. Coded apertures are used in X- and gamma ray imaging systems, because these high-energy rays cannot be focused with lenses or mirrors that work for visible light.

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RationaleEdit

 
Simplified principle of operation of a HURA hexagonal coded aperture mask used in the SPI instrument of the INTEGRAL space telescope

Imaging is usually made at optical wavelengths by lenses and mirrors. However, for X-rays and γ-rays, lenses and mirrors do not exist, or else are impractical. Image modulation by apertures is therefore often used instead. The pinhole camera is the most basic form of such a modulation imager, but its disadvantage is low throughput, as its small aperture allows through little radiation. Only a tiny fraction of the light passes through the pinhole, which causes a low signal-to-noise ratio. To solve this problem, the mask can contain many holes, in one of several particular patterns, for example. Multiple masks, at varying distances from a detector, add flexibility to this tool. Specifically the modulation collimator, invented by Minoru Oda, was used to identify the first cosmic X-ray source and thereby to launch the new field of X-ray astronomy in 1965. Many other applications in other fields, such as tomography, have since appeared.

In a coded aperture more complicated than a pinhole camera, images from multiple apertures will overlap at the detector array. It is thus necessary to use a computational algorithm (which depends on the precise configuration of the aperture arrays) to reconstruct the original image. In this way a sharp image can be achieved without a lens. The image is formed from the whole array of sensors and is therefore tolerant to faults in individual sensors; on the other hand it accepts more background radiation than a focusing-optics imager (e.g., a refracting or reflecting telescope), and therefore is normally not favored at wavelengths where these techniques can be applied.

The coded aperture imaging technique is one of the earliest forms of computational photography and has a strong affinity to astronomical interferometry. Aperture-coding was first introduced by Ables[1] and Dicke[2] and later popularized by other publications.[3]

Well known types of masksEdit

 
A rectangular MURA mask of size 101

Different mask patterns exhibit different image resolutions, sensitivities and background-noise rejection, and computational simplicities and ambiguities, aside from their relative ease of construction.

Coded-Aperture Space TelescopesEdit

See alsoEdit

ReferencesEdit

  1. ^ J. G. Ables (1968). "Fourier transform photography: a new method for X-ray astronomy". Publications of the Astronomical Society of Australia. Cambridge University Press. 1 (4): 172–173.
  2. ^ R. H. Dicke (1968). "Scatter-hole cameras for x-rays and gamma rays". The Astrophysical Journal. 153: L101.
  3. ^ Edward E. Fenimore and Thomas M. Cannon (1978). "Coded aperture imaging with uniformly redundant arrays". Applied Optics. Optical Society of America. 17 (3): 337–347.
  4. ^ Jean in 't Zand and Heiko Groeneveld. "coded aperture instruments designed for astronomical observations".
  5. ^ Anat Levin, Rob Fergus, Fredo Durand and William Freeman (2007). "Image and depth from a conventional camera with a coded aperture". ACM transactions on graphics (TOG). ACM. 26 (3): 70.
  6. ^ A next generation Ultra-Fast Flash Observatory (UFFO-100) for IR/optical observations of the rise phase of gamma-ray bursts

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