QUIJOTE Experiment: status of telescopes and instrumentation

Pérez-de-Taoro, M. R.; Aguiar-González, M.; Cózar-Castellano, Juan; Génova-Santos, R. T.; Gómez-Reñasco, F.; Hoyland, R. J.; Peláez-Santos, A.; Poidevin, F.; Tramonte, D.; Rebolo, R.; Rubiño-Martín, J. A.; Sánchez-de-la-Rosa, V.; Vega-Moreno, A.; Viera-Curbelo, T.; Vignaga, R.; Casas, F. J.; Martínez-González, E.; Ortiz, D.; Aja, B.; Artal, E.; Cano-de-Diego, J. L.; Fuente, Luisa de la; Mediavilla, A.; Terán, J. V.; Villa, Enrique; Harper, Stuart E.; McCulloch, M.; Melhuish, S. J.; Piccirillo, L.; Lasenby, A.

doi:10.1117/12.2233225

Cited by 6 publications

(3 citation statements)

References 13 publications

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“…As it was mentioned before, the receivers have the same conceptual design of the ones of QUIJOTE experiment [14,15] but with some improvements and optimization in the design. In particular, the operation bandwidth is the same of the QUIJOTE multi-frequency instrument (MFI) [15], but with a receiver design using an electronic polarization modulation similar to thirty- and forty-gigahertz instruments (TGI and FGI) [19]. On the other hand, while MFI has two polarimeters covering the band from 10 to 14 GHz and the other two covering the band from 16 to 20 GHz, the receivers of the proposed demonstrator split the full 10–20 GHz input signal to obtain the Stokes parameters of the two sub-bands in each polarimeter.…”

Section: Polarimeter Descriptionmentioning

confidence: 99%

A Microwave Polarimeter Demonstrator for Astronomy with Near-Infra-Red Up-Conversion for Optical Correlation and Detection

Casas

Ortiz

Aja

et al. 2019

Sensors

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This paper presents a 10 to 20 GHz bandwidth microwave polarimeter demonstrator, based on the implementation of a near-infra-red frequency up-conversion stage that allows both the optical correlation, when operating as a synthesized-image interferometer, and signal detection, when operating as a direct-image instrument. The proposed idea is oriented towards the implementation of ultra-sensitive instruments presenting several dozens or even thousands of microwave receivers operating in the lowest bands of the cosmic microwave background. In this work, an electro-optical back-end module replaces the usual microwave detection stage with Mach–Zehnder modulators for the frequency up-conversion, and an optical stage for the signals correlation and detection at near-infra-red wavelengths (1550 nm). As interferometer, the instrument is able to correlate the signals of large-format instruments, while operating as a direct imaging instrument also presents advantages in terms of the possibility of implementing the optical back end by means of photonic integrated circuits to achieve reductions in cost, weight, size, and power consumption. A linearly polarized input wave, with a variable polar angle, is used as a signal source for laboratory tests. The receiver demonstrator has proved its capabilities of being used as a new microwave-photonic polarimeter for the study of the lowest bands of cosmic microwave background.

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Section: Polarimeter Descriptionmentioning

confidence: 99%

A Microwave Polarimeter Demonstrator for Astronomy with Near-Infra-Red Up-Conversion for Optical Correlation and Detection

Casas

Ortiz

Aja

et al. 2019

Sensors

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“…QT-1 is focused on observations at low frequencies (10)(11)(12)(13)(14)(15)(16)(17)(18)(19)(20), and was operating between 2012 and 2018 with the Multi-Frequency Instrument (MFI, 2; 7).From 2018-2020 the KISS spectrometer was mounted(KISS, 8). QT-2 is dedicated to observations in the 30-40 GHz range, using two instruments, the Thirty-GHz Instrument (TGI) and the Forty-GHz Instrument (FGI) (7). Both TGI and FGI share the same cryostat, which contains space for 29 detectors ("pixels") that can be reconfigured in multiple ways.…”

Section: Introductionmentioning

confidence: 99%

The new multi-frequency instrument (MFI2) for the QUIJOTE facility in Tenerife

Hoyland¹,

Rubiño-Martín²,

Alonso-Arias³

et al. 2022

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

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The QUIJOTE (Q-U-I JOint TEnerife) Experiment combines the operation of two radio-telescopes and three instruments working in the microwave bands 10-20 GHz, 26-36 GHz and 35-47 GHz at the Teide observatory, Tenerife, and has already been presented in previous SPIE meetings (1; 2). The Cosmology group at the IAC have designed a new upgrade to the MFI instrument in the band 10-20 GHz. The aim of the QUIJOTE telescopes is to characterise the polarised emission of the Cosmic Microwave Background (CMB), as well as Further author information: (Send correspondence to R.J.H.

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“…The Thirty and Forty GHz polarimeters for the Q-U-I JOint TEnerife (QUIJOTE) CMB radio astronomy experiment, 1,2 are broadband very sensitive receivers to perform scientific sky observations of the Cosmic Microwave Background (CMB). The aim of the QUIJOTE experiment is the measurement of the linear polarization percentage of the received waves from the sky.…”

Section: Introductionmentioning

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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QUIJOTE Experiment: status of telescopes and instrumentation

Cited by 6 publications

References 13 publications

A Microwave Polarimeter Demonstrator for Astronomy with Near-Infra-Red Up-Conversion for Optical Correlation and Detection

A Microwave Polarimeter Demonstrator for Astronomy with Near-Infra-Red Up-Conversion for Optical Correlation and Detection

The new multi-frequency instrument (MFI2) for the QUIJOTE facility in Tenerife

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

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