Pattern measurements of reflector antennas in the compact range and validation with computer code simulation

Lee, T.-H.; Rudduck, R.; Lambert, Kevin M.

doi:10.1109/8.55587

Cited by 13 publications

(3 citation statements)

References 9 publications

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“…This code, called the Antenna Workbench (Kouyoumjian & Pathak 1974;Lee et al 1979;Lee & Ruddick 1985;Lee et al 1990), can be used to analyze single or multiple reflectors. It is capable of calculating both near-field and far-field radiation patterns.…”

Section: Appendix A: Calculation Of the Gbt Antenna Patternmentioning

confidence: 99%

“…The main beam and the sidelobes of the GBT at 1.40 GHz were calculated using a reflector antenna code developed at the Ohio State University. This code, called the Antenna Workbench (Kouyoumjian & Pathak 1974;Lee et al 1979;Lee & Ruddick 1985;Lee et al 1990), can be used to analyze single or multiple reflectors. It is capable of calculating both near-field and far-field radiation patterns.…”

Section: Appendix A: Calculation Of the Gbt Antenna Patternmentioning

confidence: 99%

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Accurate galactic 21-cm H I measurements with the NRAO Green Bank Telescope

Boothroyd

Blagrave

Lockman

et al. 2011

A&A

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Aims. We devise a data reduction and calibration system for producing highly-accurate 21-cm H i spectra from the Green Bank Telescope (GBT) of the NRAO. Methods. A theoretical analysis of the all-sky response of the GBT at 21 cm is made, augmented by extensive maps of the far sidelobes. Observations of radio sources and the Moon are made to check the resulting aperture and main beam efficiencies. Results. The all-sky model made for the response of the GBT at 21 cm is used to correct for "stray" 21-cm radiation reaching the receiver through the sidelobes rather than the main beam. This reduces systematic errors in 21-cm measurements by about an order of magnitude, allowing accurate 21-cm H i spectra to be made at about 9 angular resolution with the GBT. At this resolution the procedures discussed here allow for measurement of total integrated Galactic H i line emission, W, with errors of 3 K km s −1 , equivalent to errors in optically thin N HI of 5 × 10 18 cm −2 .

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Section: Appendix A: Calculation Of the Gbt Antenna Patternmentioning

confidence: 99%

Section: Appendix A: Calculation Of the Gbt Antenna Patternmentioning

confidence: 99%

Accurate galactic 21-cm H I measurements with the NRAO Green Bank Telescope

Boothroyd

Blagrave

Lockman

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…However, the effects on sidelobe level of varying strut diameter, wavelength, and illumination efficiency are all reproduced with an accuracy of about 0.5 dB. A discrepancy of about the same magnitude, and in the same sense, between NEC calculations of scatter cone levels and measured values has been found by Lee et al [1990].…”

Section: An Approximatementioning

confidence: 59%

Ground radiation scattered from feed support struts: A significant source of noise in paraboloidal antennas

Landecker¹,

Routledge²,

Smegal³

et al. 1991

Radio Science

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The struts supporting the feed or subreflector of a symmetrical paraboloidal antenna generate sidelobes around cones of wide opening angle by scattering energy from the plane wave leaving the reflector. On the basis of simple assumptions about these “scatter cone” sidelobes, an approximate formula is derived to predict their level relative to the main beam; it is tested against published measurements. The noise added to the antenna when the scatter cone sidelobes receive radiation from the ground is calculated, and this mechanism is seen as a significant contributor to antenna noise. The use of struts of triangular cross section in place of circular ones redirects sidelobe energy away from the back hemisphere of the radiation pattern to the front hemisphere. For most antenna pointings these sidelobes will not strike the ground, and antenna noise temperature is likely to be reduced. Radiometric measurements at 1420 MHz have been made using a 9‐m antenna equipped with struts of various cross sections and sizes. These measurements have been used to isolate the strut contribution to antenna noise, and have verified that this contribution can be reduced by using triangular struts. The strut contribution to antenna noise is calculated as a function of zenith angle of the main beam of the antenna. Triangular struts are superior to circular ones at all main‐beam zenith angles. When three struts are used, the upright Y configuration of the tripod is better than the inverted Y.

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Calculation and verification of antenna temperature for Earth‐based reflector antennas

Lambert¹,

Rudduck²

1992

Radio Science

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This paper describes an application of the classical convolution integral for the calculation of antenna temperature to Earth‐based microwave antennas. The Ohio State University‐Reflector Antenna Code has been implemented to provide the radiation pattern of antennas in the calculation. Use of the code allows the full volumetric pattern of the antenna, including all sidelobes, backlobes, and cross‐polarized response, to be included in the calculation. Additionally, the contribution to the antenna temperature from various regions of the pattern can be calculated separately and analyzed. Examples of the calculations are given along with a description of an experiment which was performed to verify the accuracy of the technique.

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Pattern measurements of reflector antennas in the compact range and validation with computer code simulation

Cited by 13 publications

References 9 publications

Accurate galactic 21-cm H I measurements with the NRAO Green Bank Telescope

Accurate galactic 21-cm H I measurements with the NRAO Green Bank Telescope

Ground radiation scattered from feed support struts: A significant source of noise in paraboloidal antennas

Calculation and verification of antenna temperature for Earth‐based reflector antennas

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