QUBIC: Using NbSi TESs with a Bolometric Interferometer to Characterize the Polarization of the CMB

Piat, M.; Bélier, B.; Bergé, L.; Bleurvacq, N.; Chapron, C.; Dheilly, S.; Dumoulin, L.; González, M.; Grandsire, L.; Hamilton, J. C.; Henrot-Versillé, S.; Hoang, Duc Thuong; Marnieros, S.; Marty, W.; Montier, L.; Olivieri, E.; Oriol, C.; Perbost, C.; Prêle, D.; Rambaud, D.; Salatino, Maria; Stankowiak, G.; Thermeau, J.-P.; Torchinsky, S.; Voisin, F.; Ade, Peter A. R.; Alberro, J.G.; Almela, A.; Amico, G.; Arnaldi, L. H.; Auguste, Didier; Aumont, J.; Azzoni, S.; Banfi, Stefano; Battaglia, P.; Battistelli, E. S.; Baù, A.; Bennett, D.; Bernard, J.-P.; Bersanelli, M.; Bigot-Sazy, M.-A.; Bonaparte, J.; Bonis, J.; Bottani, A.; Bunn, Emory F.; Burke, David; Buzi, D.; Buzzelli, A.; Cavaliere, F.; Chanial, P.; Charlassier, R.; Columbro, F.; Coppi, Gabriele; Coppolecchia, A.; D’Alessandro, G.; Bernardis, P. de; Gasperis, G. de; Leo, M. De; Petris, M. De; Donato, A.; Etchegoyen, A.; Fasciszewski, A.; Ferreyro, L.P.; Fracchia, D.; Franceschet, C.; Lerena, M.M. Gamboa; Ganga, K.; García, Beatriz; Redondo, M.E. García; Gaspard, M.; Gault, A.; Gayer, D.; Gervasi, M.; Giard, M.; Gilles, V.; Giraud‐Héraud, Y.; Berisso, M. Gómez; Grądziel, M.; Harari, D.; Haynes, V.; Incardona, F.; Jules, E.; Kaplan, J.; Korotkov, Andrei; Kristukat, C.; Lamagna, L.; Loucatos, S.; Louis, Thibaut; Luterstein, R.; Maffei, B.; Masi, S.; Mattei, A.; May, A.; McCulloch, M.; Medina, M. C.; Mele, L.; Melhuish, S. J.; Mennella, A.; Mousset, L.; Mundo, L.M.; Murphy, J. Anthony; Murphy, J.D.; Nati, F.; O'Sullivan, Créidhe M.; Paiella, A.; Pajot, F.; Passerini, A.; Pastoriza, H.; Pelosi, A.; Perciballi, M.; Pezzotta, F.; Piacentini, F.; Piccirillo, L.; Pisano, G.; Platino, M.; Polenta, G.; Puddu, Roberto; Ringegni, P.; Romero, Gustavo E.; Salum, J.M.; Schillaci, A.; Scóccola, Claudia G.; Scully, Stephen; Spinelli, S.; Stolpovskiy, M.; Suárez, F.; Tartari, A.; Timbie, Peter; Tomasi, M.; Tucker, C.; Tucker, Gregory S.; Vanneste, S.; Viganò, Daniele; Vittorio, N.; Watson, Bob; Wicek, F.; Zannoni, M.; Zullo, A.

doi:10.1007/s10909-020-02445-y

Cited by 5 publications

(5 citation statements)

References 16 publications

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“…• replacing the current mirrors by larger mirrors that are already manufactured and characterized (see O'Sullivan et al [39]); • upgrading the single 248 TES array by eight of these (four at 150 GHz and four at 220 GHz) achieving two focal planes of 992 TES each. Note that detailed quasi-optical simulations have shown that the 150 GHz optimization of the back-short of the TES is also nearly optimal at 220 GHz allowing us to use identical detector designs for both frequencies [53,54]. A new readout electronics will avoid the TD noise aliasing through the addition of Nyquist inductors [35].…”

Section: The Qubic Full Instrumentmentioning

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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Section: The Qubic Full Instrumentmentioning

confidence: 99%

QUBIC I: Overview and science program

Hamilton

Mousset

Battistelli

et al. 2022

J. Cosmol. Astropart. Phys.

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“…Each focal plane is composed of four 256-pixel TES arrays assembled together to obtain 1024-pixel detector cooled at about 320 mK by a 3 He fridge. For each quarter focal plane, two blocks of 128 SQUIDs (superconducting quantum interference devices) are used at 1 K in a 128:1 time domain multiplexing (TDM) scheme [1,2]. Each block is controlled and amplified by an ASIC (application specific integrated circuit) cooled to 40 K while a warm FPGA (field programmable gate array) board ensure the control and acquisition of the signal to the acquisition computer.…”

Section: Qubic Detection Chainmentioning

confidence: 99%

“…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 [2,7]. 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. 2022

J. Cosmol. Astropart. Phys.

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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 laboratory in Paris (APC). The detection chain is currently made of 256 NbSi transition edge sensors (TES) cooled to 320 mK. The readout system is a 128:1 time domain multiplexing scheme based on 128 SQUIDs cooled at 1 K that are controlled and amplified by a SiGe application specific integrated circuit at 40 K. We report the performance of this readout chain and the characterization of the TES. 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/√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. It demonstrated a thermal decoupling compatible with a phonon noise of about 5 × 10-17 W/√Hz at 410 mK critical temperature. While still limited by microphonics from the pulse tubes and noise aliasing from readout system, the instrument noise equivalent power is about 2 × 10-16 W/√Hz, enough for the demonstration of bolometric interferometry.

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“…While adding hardware complexity and the need to perform a dedicated assessment of its related systematics, this subsystem ensures excellent control of instrumental polarization issues [6]. This solution is shared by many current and next generation B-mode experiments, including QUBIC [7] and LiteBIRD [8].…”

Section: The Swipe Instrumentmentioning

confidence: 99%

A Testbed for Modeling Validation and Characterization of Quasi-optical Elements in Microwave Receivers

et al. 2022

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We describe the setup for the broadband millimeter/submillimeter characterization of the quasi-optical elements and the dielectric materials commonly used in microwave receivers operated in microwave astronomy. The setup is made of a large aperture (100 mm) Fourier transform spectrometer coupled to a transition edge superconducting detector. The system has been assembled and characterized in different configurations and operation modes for the acquisition of interferograms from various kinds of samples. After the initial test runs, the configuration is now being updated to ensure a broader range of measurements, including reflectance and scattering. We plan to first use this testbed for the characterization of the dielectric materials used in the LSPE/SWIPE experiment, devoted to the study the polarization of the Cosmic Microwave Background.

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QUBIC: Using NbSi TESs with a Bolometric Interferometer to Characterize the Polarization of the CMB

Cited by 5 publications

References 16 publications

QUBIC I: Overview and science program

QUBIC I: Overview and science program

QUBIC IV: Performance of TES bolometers and readout electronics

A Testbed for Modeling Validation and Characterization of Quasi-optical Elements in Microwave Receivers

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