5.3. Very Long Baseline Interferometer Systems

Moran, J. M.

doi:10.1016/s0076-695x(08)60709-7

Cited by 16 publications

(6 citation statements)

References 10 publications

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“…Hence, the density of lag multiplications has a triangular shape as a function of lag over the range˙Nt s , as shown in Fig. 8.23 (see also Moran 1976). Hence, the spectral response, the Fourier transform of this triangular function, is sinc 2 .Nt s / D sinc 2 .n/, where D n=Nt s and n is the spectral channel number.…”

Section: Comparison Of Xf and Fx Correlatorsmentioning

confidence: 91%

Digital Signal Processing

Thompson¹,

Moran²,

Swenson³

2017

Astronomy and Astrophysics Library

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Section: Comparison Of Xf and Fx Correlatorsmentioning

confidence: 91%

Digital Signal Processing

Thompson¹,

Moran²,

Swenson³

2017

Astronomy and Astrophysics Library

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“…Since the radio interferometry method has been analyzed in detail in other places [e.g., Cohen, 1973;Moran, 1974;Thomas, 1972a, b;Williams, 1970], it will be described only briefly in this paper. Single-channel interferometry will be reviewed first, followed by an outline of its extension to two-channel bandwidth synthesis.…”

Section: Radio Interferometry Techniquementioning

confidence: 99%

A demonstration of an independent-station radio interferometry system with 4-cm precision on a 16-km base line

Thomas¹,

Fanselow²,

Macdoran³

et al. 1976

J. Geophys. Res.

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A series of interferometry experiments has been conducted between two antennas at the Goldstone Deep Space Communications Complex near Barstow, California. The primary objective of these experiments was to construct and demonstrate on a short base line independent‐station instrumentation capable of making three‐dimensional base line measurements with accuracies of a few centimeters. To meet this objective, phase stable instrumentation was constructed to precisely measure time delay by means of two‐channel bandwidth synthesis. Delay measurements produced by this instrumentation led to three‐dimensional earth‐fixed base line measurements with a precision (reproducibility) of 2–5 cm for the components of a 16‐km base line. When this interferometry base line vector was compared with a base line vector obtained by a conventional survey, the two measurements differed by 2–15 cm in the various components. Probable causes of this vector discrepancy are discussed, with particular emphasis on the difficulties encountered in the comparison of a purely geometric interferometry base line vector with a geoid‐referenced survey base line.

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“…A typical experiment using European telescopes at an observing frequency of 5 GHz achieves a resolution of around 5 milli-arcseconds, equivalent to the size of a small house on the moon as seen from the Earth, and a factor of 10 better than that achieved by the Hubble Space Telescope. Traditionally the data were recorded on magnetic tape [1], with the tapes shipped to a central processing site when the observations were over. Tapes have now been replaced in most VLBI systems by inexpensive exchangeable computer disks.…”

Section: Introductionmentioning

confidence: 99%

“…The European VLBI Network (EVN) is the organization that administers VLBI operations primarily within Europe, but it also includes telescopes in the Caribbean, Asia and South Africa. The EVN members operate 18 individual antennas, including some of the largest and most sensitive radio telescopes in the world [3], see figure (1). (Fig 1 near here) The recorded data are eventually shipped to a central processor, where the tapes or disks are played back together, and the signals cross-correlated.…”

Section: Introductionmentioning

confidence: 99%

The Role of ESLEA in the development of eVLBI

Spencer

Hughes-Jones

Strong

et al. 2010

Future Generation Computer Systems

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The Internet has been used for data transfer in radio astronomy ever since its inception; however it is only recently that network bandwidth capability means that the Internet becomes competitive with traditional forms of data storage. Very Long Baseline Interferometry (VLBI) uses widely separated telescopes between which high bandwidth direct connections have not been feasible until recently. The academic networks now allow us to connect at high data rates (~1Gbps) in "eVLBI". The ESLEA project (Exploitation of Switched Lightpaths for E-science Applications) has played a major role in the development of eVLBI. We outline this development in this paper.

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5.3. Very Long Baseline Interferometer Systems

Cited by 16 publications

References 10 publications

Digital Signal Processing

Digital Signal Processing

A demonstration of an independent-station radio interferometry system with 4-cm precision on a 16-km base line

The Role of ESLEA in the development of eVLBI

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