QUBIC III: Laboratory Characterization

Torchinsky, S. A.; Hamilton, J. -Ch.; Piat, M.; Battistelli, E. S.; Chapron, C.; D'Alessandro, G.; de Bernardis, P.; De Petris, M.; Lerena, M. M. Gamboa; González, M.; Grandsire, L.; Masi, S.; Marnieros, S.; Mennella, A.; Mousset, L.; Murphy, J. D.; Prêle, D.; Stankowiak, G.; O'Sullivan, C.; Tartari, A.; Thermeau, J. -P.; Voisin, F.; Zannoni, M.; Ade, P.; Alberro, J. G.; Almela, A.; Amico, G.; Arnaldi, L. H.; Auguste, D.; Aumont, J.; Azzoni, S.; Banfi, S.; Bélier, B.; Baù, A.; Bennett, D.; Bergé, L.; Bernard, J. -Ph.; Bersanelli, M.; Bigot-Sazy, M. -A.; Bonaparte, J.; Bonis, J.; Bunn, E.; Burke, D.; Buzi, D.; Cavaliere, F.; Chanial, P.; Charlassier, R.; Cerutti, A. C. Cobos; Columbro, F.; Coppolecchia, A.; De Gasperis, G.; De Leo, M.; Dheilly, S.; Duca, C.; Dumoulin, L.; Etchegoyen, A.; Fasciszewski, A.; Ferreyro, L. P.; Fracchia, D.; Franceschet, C.; Ganga, K. M.; García, B.; Redondo, M. E. García; Gaspard, M.; Gayer, D.; Gervasi, M.; Giard, M.; Gilles, V.; Giraud-Heraud, Y.; Berisso, M. Gómez; Gradziel, M.; Hampel, M. R.; Harari, D.; Henrot-Versillé, S.; Incardona, F.; Jules, E.; Kaplan, J.; Kristukat, C.; Lamagna, L.; Loucatos, S.; Louis, T.; Maffei, B.; Marty, W.; Mattei, A.; May, A.; McCulloch, M.; Mele, L.; Melo, D.; Montier, L.; Mundo, L. M.; Murphy, J. A.; Nati, F.; Olivieri, E.; Oriol, C.; Paiella, A.; Pajot, F.; Passerini, A.; Pastoriza, H.; Pelosi, A.; Perbost, C.; Perciballi, M.; Pezzotta, F.; Piacentini, F.; Piccirillo, L.; Pisano, G.; Platino, M.; Polenta, G.; Puddu, R.; Rambaud, D.; Ringegni, P.; Romero, G. E.; Rasztocky, E.; Salum, J. M.; Schillaci, A.; Scóccola, C.; Scully, S.; Spinelli, S.; Stolpovskiy, M.; Supanitsky, A. D.; Timbie, P.; Tomasi, M.; Tucker, G.; Tucker, C.; Viganò, D.; Vittorio, N.; Wicek, F.; Wright, M.; Zullo, A.

doi:10.48550/arxiv.2008.10056

Cited by 7 publications

(26 citation statements)

References 7 publications

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“…2.7 it is straightforward to see that the FWHM of the large peaks is roughly given by FWHM = λ (P −1)∆h while their separation is θ = λ ∆h as illustrated in figure 2. The real synthesized beam of the QUBIC Technological Demonstrator has been measured in the lab using a monochromatic calibration source and is presented in [22]. For the Technological Demonstrator, the horn array is an 8 × 8 square array.…”

Section: The Monochromatic Synthesized Beammentioning

confidence: 99%

“…We compare a simulated sky to the reconstructed one using the QUBIC data analysis pipeline. Tests with a real point source were carried out in the lab and results are presented in [22].…”

mentioning

confidence: 99%

“…Detailed information about QUBIC can be found in the companion papers: Scientific overview and expected performance of QUBIC [23], Characterization of the Technological Demonstrator (TD) [22], Transition-Edge Sensors and readout characterization [24], Cryogenic system performance [25], Half Wave Plate rotator design and performance [26], Feedhorn-switches system of the TD [27], and Optical design and performance [28].…”

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confidence: 99%

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QUBIC II: Spectro-Polarimetry with Bolometric Interferometry

Mousset,

Lerena,

Battistelli

et al. 2020

Preprint

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Bolometric Interferometry is a novel technique that has the ability to perform spectroimaging. A Bolometric Interferometer observes the sky in a wide frequency band and can reconstruct sky maps in several sub-bands within the physical band. This provides a powerful spectral method to discriminate between the Cosmic Microwave Background (CMB) and astrophysical foregrounds. In this paper, the methodology is illustrated with examples based on the Q & U Bolometric Interferometer for Cosmology (QUBIC) which is a ground-based instrument designed to measure the B-mode polarization of the sky at millimeter wavelengths. We consider the specific cases of point source reconstruction and Galactic dust mapping and we characterize the Point Spread Function as a function of frequency. We study the noise properties of spectro-imaging, especially the correlations between sub-bands, using end-toend simulations together with a fast noise simulator. We conclude showing that spectroimaging performance are nearly optimal up to five sub-bands in the case of QUBIC.

show abstract

Section: The Monochromatic Synthesized Beammentioning

confidence: 99%

“…We compare a simulated sky to the reconstructed one using the QUBIC data analysis pipeline. Tests with a real point source were carried out in the lab and results are presented in [22].…”

mentioning

confidence: 99%

mentioning

confidence: 99%

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QUBIC II: Spectro-Polarimetry with Bolometric Interferometry

Mousset,

Lerena,

Battistelli

et al. 2020

Preprint

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“…We also positively tested both in lab and inside the QUBIC cryostat the switch array at a temperature 5K close to the nominal one (1K). We developed a readout system able to monitor the actual switch positions with a very good repeatability and reliability, as witnessed by the fringe pattern detection ( [11]). Since the micro-miniaturized coils of the TD are no more available, we found an alternative for the FI which forced us to redesign the whole mechanism around a bi-stable shutter which has been already tested at 5K with very positive results.…”

Section: Discussionmentioning

confidence: 99%

QUBIC VII: The feedhorn-switch system of the technological demonstrator

Cavaliere,

Mennella,

Zannoni

et al. 2020

Preprint

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We present the design, manufacturing and performance of the horn-switch system developed for the technological demonstrator of QUBIC (the Q&U Bolometric Interferometer for Cosmology). This system is constituted of 64 back-to-back dual-band (150 GHz and 220 GHz) corrugated feed-horns interspersed with mechanical switches used to select desired baselines during the instrument self-calibration. We manufactured the horns in aluminum platelets milled by photo-chemical etching and mechanically tightened with screws. The switches are based on steel blades that open and close the wave-guide between the backto-back horns and are operated by miniaturized electromagnets. We also show the current development status of the feedhorn-switch system for the QUBIC full instrument, based on an array of 400 horn-switch assemblies.

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“…The scientific overview and expected performance of the instrument are addressed here. The other papers in the special issue address the following topics: the ability of bolometric interferometry to do spectral imaging [33], the calibration and performance in the laboratory of the TD [34], the performance of the detector array and readout electronics [35], the cryogenic system performance [36], the Half Wave Plate rotator system [37], the back-to-back feedhorn-switch system [38], and the optical design and performance [39].…”

Section: Introductionmentioning

confidence: 99%

QUBIC I: Overview and science program

Hamilton

Mousset

Battistelli

et al. 2022

J. Cosmol. Astropart. Phys.

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The Q & U Bolometric Interferometer for Cosmology (QUBIC) is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Background (CMB), which is one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical foregrounds which can only be controlled through multichroic observations. QUBIC is designed to address these observational issues with a novel approach that combines the advantages of interferometry in terms of control of instrumental systematic effects with those of bolometric detectors in terms of wide-band, background-limited sensitivity. The QUBIC synthesized beam has a frequency-dependent shape that results in the ability to produce maps of the CMB polarization in multiple sub-bands within the two physical bands of the instrument (150 and 220 GHz). These features make QUBIC complementary to other instruments and makes it particularly well suited to characterize and remove Galactic foreground contamination. In this article, first of a series of eight, we give an overview of the QUBIC instrument design, the main results of the calibration campaign, and present the scientific program of QUBIC including not only the measurement of primordial B-modes, but also the measurement of Galactic foregrounds. We give forecasts for typical observations and measurements: with three years of integration on the sky and assuming perfect foreground removal as well as stable atmospheric conditions from our site in Argentina, our simulations show that we can achieve a statistical sensitivity to the effective tensor-to-scalar ratio (including primordial and foreground B-modes) σ(r)=0.015.

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QUBIC III: Laboratory Characterization

Cited by 7 publications

References 7 publications

QUBIC II: Spectro-Polarimetry with Bolometric Interferometry

QUBIC II: Spectro-Polarimetry with Bolometric Interferometry

QUBIC VII: The feedhorn-switch system of the technological demonstrator

QUBIC I: Overview and science program

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