The Development of High-Resolution Imaging in Radio Astronomy

Kellermann, K. I.; Moran, J. M.

doi:10.1146/annurev.astro.39.1.457

Cited by 57 publications

(45 citation statements)

References 272 publications

(207 reference statements)

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“…Fierce competition developed between Caltech's plan to construct eight movable antennas, each 39.6-m in diameter, and a more elaborate (and more expensive) proposal from the NRAO to build the 27-element VLA. Repeated reviews by the NSF encouraged the further development of the Owens Valley Array (see Kellermann & Moran 1999), but only one of the 39.6-m dishes was ever built (see Figure 16). Instead, the NSF funded the construction of the NRAO VLA.…”

Section: The Owens Valley Radio Observatory (Ovro)mentioning

confidence: 99%

Gordon James Stanley and the Early Development of Radio Astronomy in Australia and the United States

Kellermann

Orchiston

Slee

2005

Publ. Astron. Soc. Aust

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Abstract:Following the end of the Second World War, the CSIRO Radiophysics Laboratory applied the expertise and surplus radar equipment acquired during the war to problems of astronomy. Gordon Stanley was among the first group of scientists and engineers to work in the exciting new field of radio astronomy. Like many of his contemporaries, he had a strong background in radio and electronics but none in astronomy. At the Radiophysics Laboratory, and later at Caltech, Stanley developed innovative new radio telescopes and sophisticated instrumentation which resulted in important new discoveries that changed, in a fundamental way, our understanding of the Universe. He was one of those who played a key role in the early development of radio astronomy both in Australia and the United States.

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Section: The Owens Valley Radio Observatory (Ovro)mentioning

confidence: 99%

Gordon James Stanley and the Early Development of Radio Astronomy in Australia and the United States

Kellermann

Orchiston

Slee

2005

Publ. Astron. Soc. Aust

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“…Those observations, even for very large baseline interferometry (VLBI), take place at much larger scales (e.g. Kellermann & Moran 2001). Models of the jet morphology on larger scales are based on (general relativistic) magnetohydrodynamic (MHD) methods, but those models can only produce synthetic spectra (Gracia et al 2009;Porth et al 2011).…”

Section: Introductionmentioning

confidence: 99%

A Numerical Model of Parsec-Scale SSC Morphologies and Their Radio Emission

Richter

Spanier

2016

ApJ

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In current models for jets of AGNs and their emission a shortcoming in the description and understanding of the connection between the largest and smallest scales exists. In this work we present a spatially resolved SSC model extended to parsec scales, which opens the possibility of probing the connections between the radio and high energy properties. We simulate an environment that leads to Fermi-I acceleration of leptonic particles and includes the full time dependence of this process. Omitting the restriction of a finite downstream region, we find that the spectral energy distribution (SED) produced by the accelerated particles strongly depends on their radial confinement behind the shock. The requirement, for both the restriction of high energy emission to a small region around the shock and the production of a flat radio spectrum, is an initial linear increase of the radius immediately behind the shock, which then slows down with increasing distance from the shock. A good representation of the data for the Blazar Mkn501 is achieved by a parameterized log-function. The prediction for the shape of the radio blob is given by the flux distribution with respect to shock distance.

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“…For a more extensive overview the reader is referred to [7], [8] or [9]. A good historic perspective can be found in [10], whereas [11] provides a very recent perspective.…”

Section: Introductionmentioning

confidence: 99%

Parametric High Resolution Techniques for Radio Astronomical Imaging

Ben-David

Leshem

2008

IEEE J. Sel. Top. Signal Process.

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The increased sensitivity of future radio telescopes will result in requirements for higher dynamic range within the image as well as better resolution and immunity to interference. In this paper we propose a new matrix formulation of the imaging equation in the cases of non co-planar arrays and polarimetric measurements. Then we improve our parametric imaging techniques in terms of resolution and estimation accuracy. This is done by enhancing both the MVDR parametric imaging, introducing alternative dirty images and by introducing better power estimates based on least squares, with positive semi-definite constraints. We also discuss the use of robust Capon beamforming and semi-definite programming for solving the self-calibration problem. Additionally we provide statistical analysis of the bias of the MVDR beamformer for the case of moving array, which serves as a first step in analyzing iterative approaches such as CLEAN and the techniques proposed in this paper. Finally we demonstrate a full deconvolution process based on the parametric imaging techniques and show its improved resolution and sensitivity compared to the CLEAN method.

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The Development of High-Resolution Imaging in Radio Astronomy

Cited by 57 publications

References 272 publications

Gordon James Stanley and the Early Development of Radio Astronomy in Australia and the United States

Gordon James Stanley and the Early Development of Radio Astronomy in Australia and the United States

A Numerical Model of Parsec-Scale SSC Morphologies and Their Radio Emission

Parametric High Resolution Techniques for Radio Astronomical Imaging

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