Minimum error image reconstruction for coded mask telescopes

Rideout, R. M.; Skinner, G. K.

doi:10.1051/aas:1996310

Cited by 6 publications

(4 citation statements)

References 11 publications

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“…Although for sufficiently long observations or combinations of observations, these systematic errors will inevitably become important, many methods are available to reduce them [33][34][35][36][37][38][39][40][41][42][43]. Typically these involves fitting and subtracting bright sources or otherwise taking them into account, and carefully modeling background non-uniformities.…”

Section: Introductionmentioning

confidence: 99%

“…The ghost images and other imaging artifacts that arise from partial coding, from non-uniform background, or from other effects present in real instruments can be alleviated provided one has a good understanding of the instrument and adequate computing resources. Although for sufficiently long observations or combinations of observations, these systematic errors will inevitably become important, many methods are available to reduce them [33][34][35][36][37][38][39][40][41][42][43]. Typically these involves fitting and subtracting bright sources or otherwise taking them into account, and carefully modeling background non-uniformities.…”

Section: Introductionmentioning

confidence: 99%

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Sensitivity of coded mask telescopes

Skinner

2008

Appl. Opt.

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Simple formulae are often used to estimate the sensitivity of coded mask X-ray or gamma-ray telescopes, but these are strictly only applicable if a number of basic assumptions are met. Complications arise, for example, if a grid structure is used to support the mask elements, if the detector spatial resolution is not good enough to completely resolve all the detail in the shadow of the mask or if any of a number of other simplifying conditions are not fulfilled. We derive more general expressions for the Poisson-noise-limited sensitivity of astronomical telescopes using the coded mask technique, noting explicitly in what circumstances they are applicable. The emphasis is on using nomenclature and techniques that result in simple and revealing results. Where no convenient expression is available a procedure is given which allows the calculation of the sensitivity. We consider certain aspects of the optimization of the design of a coded mask telescope and show that when the detector spatial resolution and the mask to detector separation are fixed, the best source location accuracy is obtained when the mask elements are equal in size to the detector pixels.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Sensitivity of coded mask telescopes

Skinner

2008

Appl. Opt.

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“…In order to obtain S from D, several approaches and algorithms have been discussed in the literature (see Skinner (2003) for a review) and used in specific instruments with specific detector systems and mask patterns (Hammersley et al 1992;Skinner et al 1987a;Krivonos et al 2010;Chou et al 2005;Hong 2002;Rideout and Skinner 1996). A widely used reconstruction method, described in this paper, is the correlation of the recorded data with a suitable decoding function that in general mimics the mask pattern.…”

Section: Image Formationmentioning

confidence: 99%

Coded Aperture Imaging in High-energy Astrophysics

Braga¹

2019

PASP

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Hard X-ray and low-energy gamma-ray coded-aperture imaging instruments have been highly successful as high-energy surveyors and transientsource discoverers and trackers over the past decades. Albeit having relatively low sensitivity as compared to focussing instruments, coded-aperture telescopes still represent a very good choice for simultaneous, high cadence spectral measurements of individual point sources in large source fields. Here I present a review of the fundamentals of coded-aperture imaging instruments in high-energy astrophysics. Emphasis is on fundamental aspects of the technique, coded-mask instrument characteristics, and properties of the reconstructed images.After the first CAI space experiments were developed and flown, comprehensive reviews of astronomical spatial multiplexing imaging techniques, including CAI, were published (Caroli et al. 1987;Skinner 1995). In the Web, an excellent description of CAI is available at in 't Zand (1992) and references therein. The focus of this article is to bring the field up to date and review some aspects of the technique that were not specifically covered before, such as some special features of coded-mask instruments and some statistical properties of the reconstructed images. I also comment on important results obtained by more recent coded-mask space instruments.

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“…Hence, the reconstruction (6) is a constrained Wiener filtering which extends the work of Rideout & Skinner (1996) to the Poissonian statistic. This choice is attractive, since it usually produces faster algorithmic forms.…”

Section: Choosing a Penalty Functional φmentioning

confidence: 99%

Imaging techniques for gamma-ray diffuse emission: application to INTEGRAL/SPI

Allain

Roques²

2006

A&A

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Diffuse imaging in the gamma-ray energy range is a challenging problem, since faint radiation is usually mixed with strong instrumental background components. This situation results in data sets that are not very informative, so they lead to non robust image reconstruction. In this paper, we used a Bayesian approach to produce sky-maps with high resolution features. This method is then compared with the standard Richardson-Lucy algorithm on the basis of mock data sets that were generated from the SPI/INTEGRAL in-flight model.

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Minimum error image reconstruction for coded mask telescopes

Cited by 6 publications

References 11 publications

Sensitivity of coded mask telescopes

Sensitivity of coded mask telescopes

Coded Aperture Imaging in High-energy Astrophysics

Imaging techniques for gamma-ray diffuse emission: application to INTEGRAL/SPI

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