微波電路期中報告 論文研討 : John C. Webber 、 Marian W. Pospieszalski, “Microwave Instrumentation for Radio Astronomy”,IEEE TRANSACTIONS ON MICROWAVE THEORY AND

TECHNIQUES, VOL. 50, NO. 3, MARCH 2002

報告人 : 碩研電子一甲 MA030217 陳力源

Southern Taiwan UniversitySouthern Taiwan University Department of Electronic Engineering

摘要 Radio astronomy is a branch of science that

allows observation of natural radio signals from cosmic sources.

Microwave techniques are employed in large radio telescope systems.

Index Terms—Amplifiers, radio astronomy, radio receivers, superconductor–insulator–superconductor mixers.

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IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES, VOL. 50, NO. 3, MARCH 2002

Radiometers

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(a) Resistor at temperature T. (b) Antenna in an absorbing box attemperature T. (c) Antenna observing sky at temperature T (after [2]).

Simplified block diagram of a total power receiver.

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IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES, VOL. 50, NO. 3, MARCH 2002

from antenna theory that Upon substitution of (3) into (2), (1) is obtained, i.n., the available noise power at the ideal antenna terminals of Fig 2.

---(3)

---(2)

---(1)

Geometry of a simple two-element interferometer

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Geometry of a simple two-element interferometer

A.General Remarks

The quest for ultra-low-noise reception is especially important for radio astronomy

as the receiver noise is usually a significant part of the system noise

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IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES, VOL. 50, NO. 3, MARCH 2002

LOW-NOISE DEVICES

B.HFET Amplifiers the technology of InP devices has matured and allowed practical use.

Hybrid “chip and wire” amplifiers have been demonstrated up to frequencies of 118 GHz

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LOW-NOISE DEVICES

IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES, VOL. 50, NO. 3, MARCH 2002

Comparison of noise temperature of NRAO cryogenic receivers using InP HFET amplifiers cooled to approximately 20 K and SIS mixer receivers cooled to 4 K.

IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES, VOL. 50, NO. 3, MARCH 2002

Fig. 4.

C. SIS Mixers

An SIS mixer employs a superconducting tunnel junction as the nonlinear mixing element.

A high-quality SIS mixer can have a noise temperature ( 5 K at 100 GHz)

Modern SIS mixers normally use Nb junctions, which give good results when cooled to 4.0-K physical temperature

Junction sizes are typically a few square micrometers, and critical current densities are typically a few thousand A/cm .

an IF bandwidth of 1 GHz, with the exception of an approximately 3-GHz

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IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES, VOL. 50, NO. 3, MARCH 2002

Example of noise performance of a fixed-tuned SIS mixer (discrete points) and the entire receiver (solid line) for 200–290 GHz

a balanced SIS mixer has the same advantages as a balanced conventional mixer: reduction of the required LO power and canceling of the LO sideband noise downconverted into the IF

band.

A balanced SIS mixer using niobium MMIC technology has been demonstrated at 200–300 GHz

A.HFET Receiver A critical area in very low-noise receiver

design is a low-loss coupling between an ambient temperature feed horn and a cryogenic amplifier.

The VLBA front-ends use a gapped circular waveguide transition from the feed to a cooled polarizer located within the vacuum Dewar.

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IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES, VOL. 50, NO. 3, MARCH 2002

EXAMPLES OF RADIO ASTRONOMY RECEIVERS

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IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES, VOL. 50, NO. 3, MARCH 2002

B. SIS Receiver SIS mixer receivers are typically employed

above frequencies of about 100 GHz.

The radiation into the mixer are the same as for HFET receivers,made even more difficult by smaller dimensions and tolerances as the frequency is increased.

Double-sideband receiver noise temperatures of approximately 20 K have been reported near 100 GHz for Nb SIS mixer receivers

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Simplified block diagram of a MAP satellite pseudocorrelation radiometer

C. MAP Radiometer

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IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES, VOL. 50, NO. 3, MARCH 2002

100-meter Robert C. Byrd GBTInner portion of the VLA in its most compact configuration

本文內容對我自己幫助也很大 ， Microwave Instrumentation for Radio Astronomy， 運作方法需要電子學知識 , 電磁波傳遞與接收 , 需要使用微波工程內容 ,,所以是一個十足有趣的領域。

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結論

參考文獻

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