QUBIC Technical Design Report

Aumont, J.; Bélier, B.; Lowitz, A.; Cammilleri, D.; Tartari, A.; Ghribi, A.; Coppolecchia, A.; Vittorio, N.; Grądziel, M.; Puddu, Roberto; Giard, M.; Bordier, G.; Tristram, M.; Gasperis, G. de; Brossard, J.; Pajot, F.; Grandsire, L.; Dumoulin, L.; Bernard, J.-P.; O'Sullivan, Créidhe M.; Salatino, Maria; Chanial, P.; D’Alessandro, G.; Franceschet, C.; Mennella, A.; Zullo, A.; Giraud‐Héraud, Y.; Pelosi, A.; Rigaut, O.; Battaglia, P.; Kaplan, J.; Pisano, G.; Korotkov, Andrei; Torto, F. Del; Buzi, D.; Bergé, L.; Chapron, C.; Viganò, Daniele; Paiella, A.; Gayer, D.; Henrot-Versillé, S.; Holtzer, N.; Coppi, Gabriele; Tucker, Gregory S.; Bunn, Emory F.; Harari, D.; Montier, L.; Prêle, D.; Bennett, D.; Murphy, A.; Lande, J.; Marnieros, S.; Passerini, A.; Voisin, F.; Zannoni, M.; Battistelli, E. S.; Banfi, Stefano; Hamilton, Jean-Christophe; Medina, M. C.; Bleurvacq, N.; Bersanelli, M.; Loucatos, S.; Buzzelli, A.; Scully, Stephen; Decourcelle, T.; Martino, J. Rodrı́guez; García, Beatriz; Rambaud, D.; Timbie, Peter; D’Agostino, Rocco; Cavaliere, F.; Petris, M. De; Baù, A.; Lamagna, L.; Romero, Gustavo E.; Melhuish, S. J.; May, A.; Perdereau, O.; Gervasi, M.; Stolpovskiy, M.; Schillaci, A.; Gault, A.; Piccirillo, L.; Suárez, F.; Couchot, F.; Haynes, V.; Etchegoyen, A.; Maffei, B.; Néel, Delphine; Luković, Vladimir V.; Bernardis, P. de; McCulloch, M.; Perbost, C.; Bigot-Sazy,; Piat, M.; Watson, Bob; Masi, S.; Ng, M. W.

doi:10.48550/arxiv.1609.04372

Cited by 9 publications

(12 citation statements)

References 8 publications

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“…For this detection chain each FPGA manages 128 detectors, with a total of 16 FPGAs for the full 2048 pixel focal planes. A dedicated software named QUBIC Studio was developed at the Institute for Research in Astrophysics and Planetology (IRAP) for the data acquisition [6]. QUBIC Studio interfaces with the generic Electrical Ground Support Equipment (EGSE) tool, called "Dispatcher", which was also developed at IRAP.…”

Section: Warm Electronics and Acquisition Softwarementioning

confidence: 99%

QUBIC IV: Performance of TES Bolometers and Readout Electronics

Piat,

Stankowiak,

Battistelli

et al. 2021

Preprint

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A prototype version of the Q & U Bolometric Interferometer for Cosmology (QUBIC) underwent a campaign of testing in the laboratory at Astroparticle Physics and Cosmology in Paris. The detection chain is currently made of 256 NbSi Transition Edge Sensors cooled to 320 mK. The readout system is a 128:1 Time Domain Multiplexing scheme based on 128 SQUIDs cooled at 1K that are controlled and amplified by an SiGe Application Specific Integrated Circuit at 40 K. We report the performance of this readout chain and the characterization of the TESs. The readout system has been functionally tested and characterized in the lab and in QUBIC. The Low Noise Amplifier demonstrated a white noise level of 0.3 nV/sqrt(Hz). Characterizations of the QUBIC detectors and readout electronics includes the measurement of I-V curves, time constant and the Noise Equivalent Power. The QUBIC TES bolometer array has approximately 80% detectors within operational parameters. While still limited by micro-phonics from the pulse tubes and noise aliasing from readout system, the Noise Equivalent Power is about 2 × 10 −16 W/ √ Hz, enough for the demonstration of bolometric interferometry. 18 4.8 Noise characterizations 21 4.8.1 Noise in normal and superconducting states 23 4.8.2 Noise in the transition 23 5 Conclusion 29

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Section: Warm Electronics and Acquisition Softwarementioning

confidence: 99%

QUBIC IV: Performance of TES Bolometers and Readout Electronics

Piat,

Stankowiak,

Battistelli

et al. 2021

Preprint

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“…The instrument design, based on this architecture, has been finalised. 2 At the time of writing, all of the subsystems have been validated 3 and have been shipped to the Laboratoire Astroparticule et Cosmologie (APC) for integration and testing before deployment to the Alto Chorrillos site later this year. Figure 2 below shows a section-view of the full receiver cryostat model.…”

Section: Instrument Architecturementioning

confidence: 99%

“…QUBIC, the QU Bolometric Interferometer for Cosmology, [1][2][3] is a novel forthcoming instrument to measure the Bmode polarization anisotropy of the Cosmic Microwave Background at intermediate angular scales (30 < < 200). The detection of primordial B-mode polarization would constitute direct evidence for inflation.…”

Section: Introductionmentioning

confidence: 99%

“…4,5 Measurement of the signal will be extremely challenging, owing primarily to the size of the expected signal, instrumental systematics that could possibly induce polarization leakage from the relatively large E signal into B, and the brightness of foregrounds (principally polarized galactic dust emission). 2 QUBIC has been designed to address this challenge with a novel approach, namely bolometric interferometry, which combines the background-limited sensitivity of transition edge sensors (TES) with the control of systematics allowed by the observation of interference fringe patterns.…”

Section: Introductionmentioning

confidence: 99%

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Thermal architecture for the QUBIC cryogenic receiver

May¹,

Chapron²,

Coppi³

et al. 2018

Preprint

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QUBIC, the QU Bolometric Interferometer for Cosmology, is a novel forthcoming instrument to measure the B-mode polarization anisotropy of the Cosmic Microwave Background. The detection of the B-mode signal will be extremely challenging; QUBIC has been designed to address this with a novel approach, namely bolometric interferometry. The receiver cryostat is exceptionally large and cools complex optical and detector stages to 40 K, 4 K, 1 K and 350 mK using two pulse tube coolers, a novel 4 He sorption cooler and a double-stage 3 He/ 4 He sorption cooler. We discuss the thermal and mechanical design of the cryostat, modelling and thermal analysis, and laboratory cryogenic testing.

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“…These are the Millimeter-wave Bolometric Interferometry [MBI, 17,18], the Einstein Polarization Interferometer for Cosmology [EPIC,19], the Background RAdiation INterferometer [BRAIN,20], and CMBPol [21]. Members of all these collaborations joined together to develop the Q & U Bolometric Interferometer for Cosmology [QUBIC, [22][23][24][25][26].…”

Section: Introductionmentioning

confidence: 99%

QUBIC I: Overview and ScienceProgram

Hamilton,

Mousset,

Battistelli

et al. 2020

Preprint

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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 its unique capability to combine 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 subbands within the two physical bands of the instrument (150 and 220 GHz). This unique capability distinguishes QUBIC from 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 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. Assuming the 220 GHz is used to subtract foreground contamination together with data from other surveys such as Planck 353 GHz channel, our sensitivity to primordial tensors is given by that of the 150 GHz channel alone and is σ(r) = 0.021.

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QUBIC Technical Design Report

Cited by 9 publications

References 8 publications

QUBIC IV: Performance of TES Bolometers and Readout Electronics

QUBIC IV: Performance of TES Bolometers and Readout Electronics

Thermal architecture for the QUBIC cryogenic receiver

QUBIC I: Overview and ScienceProgram

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