Polarimetric receiver in the forty gigahertz band: new instrument for the Q-U-I joint Tenerife experiment

Villa, Enrique; Cano, Juan Luis; Aja, B.; Terán, J. V.; Fuente, Luisa de la; Mediavilla, A.; Artal, E.

doi:10.1007/s10686-018-9579-0

Cited by 3 publications

(2 citation statements)

References 16 publications

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“…The TGI and FGI receivers 4,5 are polarimeters to obtain three (of four) Stokes parameters (I, Q, U). The Cosmic Microwave Background (CMB) has a very weak linear polarization.…”

Section: Receiver Schemesmentioning

confidence: 99%

Broadband polarimeter receivers at 30 and 40 GHz for cosmic microwave background measurement

Artal

Aja

Fuente

et al. 2020

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X

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Broadband radiometers at 30 and 40 GHz for QUIJOTE radio astronomy experiment are very sensitive receivers to perform scientific sky observations of the Cosmic Microwave Background (CMB). The aim of this experiment is the linear polarization percentage measurement of the received signals. Radiometers have cryogenically cooled Front-End Modules followed by room temperature amplification, correlation and detection modules. Their relative bandwidth is around 30%. There are 30 receivers (pixels) at 30 GHz and 29 receivers at 40 GHz. The radiometer scheme is based on two balanced branches, microwave correlation and direct detection. The manufactured receivers measure Stokes polarization parameters I, Q, and U simultaneously. This paper describes the principle of operation of polarimeter receivers, and present details of manufactured subsystems, integration and test results. Receivers integrate different technologies: waveguides, microstrip, Monolithic Microwave Integrated Circuits (MMIC) and active and passive devices. The receivers are currently under installation in El Teide Observatory, Tenerife (Canary Islands, Spain).

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“…The TGI and FGI receivers 4,5 are polarimeters to obtain three (of four) Stokes parameters (I, Q, U). The Cosmic Microwave Background (CMB) has a very weak linear polarization.…”

Section: Receiver Schemesmentioning

confidence: 99%

Broadband polarimeter receivers at 30 and 40 GHz for cosmic microwave background measurement

Artal

Aja

Fuente

et al. 2020

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X

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View full text Add to dashboard Cite

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“…The polarization of the CMB signal can be measured using special radiometer configurations, acting as polarimetric receivers to finally obtain the Stokes parameters of the received CMB signal. 3,[9][10][11] On the other hand, radio interferometry is a particularly valuable technique for the study of the CMB anisotropy, due to its inherently high stability and robustness against many systematic errors. [12][13][14] Since the angular resolution is fixed by the size of the instrument in wavelengths, the system temperature and the instrument bandwidth determine the brightness sensitivity.…”

Section: Introductionmentioning

confidence: 99%

10- to 19.5-GHz microwave receiver of an electro-optical interferometer for radio astronomy

Aja

Fuente

Artal

et al. 2019

J. Astron. Telesc. Instrum. Syst.

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This document describes the analysis, design, and prototype test results of the microwave section of a 10-to 19.5-GHz interferometer, aimed at obtaining polarization data of cosmic microwave background (CMB) radiation from the sky. First, receiver analysis is thoroughly assessed to study the contribution of each subsystem when obtaining the Stokes parameters of an input signal. Then, the receiver design is detailed starting from the front-end module, which works at cryogenic temperature, composed of a set of passive components: feedhorn, orthomode transducer, and polarizer, together with active components, such as very low-noise amplifiers. The back-end module (BEM) is directly connected, working at room temperature for further amplification, phase switching, and correlation of the signals. Moreover, the whole frequency band is split into two sub-bands (10 to 14 GHz and 16 to 20 GHz) using a high selective diplexer in the BEM in order to reject radiofrequency interferences. Phase switches allow phase difference steps of 5.625 deg, which modulate the correlated outputs to reduce systematic effects in the postdetection signal processing. Finally, measurements of all the subsystems comprising the microwave section of the receiver as well as the characterization of the complete microwave receiver are presented. The obtained results demonstrate successful performance of the microwave receiver that, together with an electro-optical correlator and a near-infrared camera, comprises the interferometer. Moreover, synthesized images corresponding to combinations of the Stokes parameters can be obtained with the whole system.

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An Ultra-Compact Full-Band Waveguide Quadrature Hybrid Coupler

Cano

Ceccato

Fernández

et al. 2022

IEEE Microw. Wireless Compon. Lett.

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This work proposes an easily scalable quadrature hybrid coupler (QHC) topology with two symmetric stepped apertures that originate a square coaxial-like mid-section. This new configuration enables an ultra-compact design, three times shorter than equivalent structures, having 40% of fractional bandwidth with 25 dB of matching/isolation and 1 dB of axial ratio (AR). The impedance transformers can be easily redesigned to meet other requirements related to electrical performance or even other desired coupling values. For verification purposes, a prototype at Ku-band was manufactured and measured showing good agreement with simulation results.

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Polarimetric receiver in the forty gigahertz band: new instrument for the Q-U-I joint Tenerife experiment

Cited by 3 publications

References 16 publications

Broadband polarimeter receivers at 30 and 40 GHz for cosmic microwave background measurement

Broadband polarimeter receivers at 30 and 40 GHz for cosmic microwave background measurement

10- to 19.5-GHz microwave receiver of an electro-optical interferometer for radio astronomy

An Ultra-Compact Full-Band Waveguide Quadrature Hybrid Coupler

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