Thermal architecture for the QUBIC cryogenic receiver

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

doi:10.1117/12.2312085

Cited by 5 publications

(6 citation statements)

References 15 publications

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“…near San Antonio de los Cobres, in the Salta province. A full description of the QUBIC instrument is given in these proceedings [3] and in [4,5,6,7,8,9]. A schematic of QUBIC is shown in Fig.…”

Section: The Qubic Instrumentmentioning

confidence: 99%

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

et al. 2020

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QUBIC (Q & U Bolometric Interferometer for Cosmology) is an international ground-based experiment dedicated in the measurement of the polarized fluctuations of the Cosmic Microwave Background (CMB). It is based on bolometric interferometry, an original detection technique which combine the immunity to systematic effects of an interferometer with the sensitivity of low temperature incoherent detectors. QUBIC will be deployed in Argentina, at the Alto Chorrillos mountain site near San Antonio de los Cobres, in the Salta province.The QUBIC detection chain consists in 2048 NbSi Transition Edge Sensors (TESs) cooled to 350mK.The voltage-biased TESs are read out with Time Domain Multiplexing based on Superconducting QUantum Interference Devices (SQUIDs) at 1 K and a novel SiGe Application-Specific Integrated Circuit (ASIC) at 60 K allowing to reach an unprecedented multiplexing (MUX) factor equal to 128.The QUBIC experiment is currently being characterized in the lab with a reduced number of detectors before upgrading to the full instrument. I will present the last results of this characterization phase with a focus on the detectors and readout system.

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Section: The Qubic Instrumentmentioning

confidence: 99%

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

et al. 2020

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“…Sub-K cooling can be obtained by means of simple sealed L 4 He and L 3 He evaporation refrigerators (EVRs, see e.g. [16][17][18]), if an operating temperature ∼300 mK is sufficient. The detectors of QUBIC operate in two bands, centered at 150 and 220 GHz, around the maximum brightness of the CMB.…”

Section: Jcap04(2022)038 1 Introductionmentioning

confidence: 99%

QUBIC V: Cryogenic system design and performance

Masi¹,

Battistelli²,

Bernardis³

et al. 2022

J. Cosmol. Astropart. Phys.

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Current experiments aimed at measuring the polarization of the Cosmic Microwave Background (CMB) use cryogenic detector arrays with cold optical systems to boost their mapping speed. For this reason, large volume cryogenic systems with large optical windows, working continuously for years, are needed. The cryogenic system of the QUBIC (Q & U Bolometric Interferometer for Cosmology) experiment solves a combination of simultaneous requirements: very large optical throughput (∼40 cm2sr), large volume (∼1 m3) and large mass (∼165 kg) of the cryogenic instrument. Here we describe its design, fabrication, experimental optimization and validation in the Technological Demonstrator configuration. The QUBIC cryogenic system is based on a large volume cryostat that uses two pulse-tube refrigerators to cool the instrument to ∼3 K. The instrument includes the cryogenic polarization modulator, the corrugated feedhorn array, and the lower temperature stages: a 4He evaporator cooling the interferometer beam combiner to ∼1 K and a 3He evaporator cooling the focal-plane detector arrays to ∼0.3 K. The cryogenic system has been tested and validated for more than 6 months of continuous operation. The detector arrays have reached a stable operating temperature of 0.33 K, while the polarization modulator has operated at a ∼10 K base temperature. The system has been tilted to cover the boresight elevation range 20°-90° without significant temperature variations. The instrument is now ready for deployment to the high Argentinean Andes.

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“…Each focal plane is populated by 1,024 Transition-Edge Sensors (TESes) cooled down to 350 mK by a custom 3 He-4 He adsorption fridge. 11 For a general overview of the experiment and bolometric interferometry see Battistelli et al 12 and references therein. For the instrument design and its thermal architecture see the QUBIC Technical Report 13 and May et al, 11 respectively.…”

Section: Introductionmentioning

confidence: 99%

“…11 For a general overview of the experiment and bolometric interferometry see Battistelli et al 12 and references therein. For the instrument design and its thermal architecture see the QUBIC Technical Report 13 and May et al, 11 respectively. Updates on the current status of the experiment can be found in Mennella et al 14 and in O'Sullivan et al 15 Simulations of the optical combiner and the back to back horns array are described in O'Sullivan et al 16 In this paper we focus on the experimental characterization of a QUBIC detector array which consists of 256 TESes.…”

Section: Introductionmentioning

confidence: 99%

Performance of NbSi transition-edge sensors readout with a 128 MUX factor for the QUBIC experiment

Bélier

Chapron

Hoang³

et al. 2018

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

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QUBIC (the Q&U Bolometric Interferometer for Cosmology) is a ground-based experiment which seeks to improve the current constraints on the amplitude of primordial gravitational waves. It exploits the unique technique, among Cosmic Microwave Background experiments, of bolometric interferometry, combining together the sensitivity of bolometric detectors with the control of systematic effects typical of interferometers. QUBIC will perform sky observations in polarization, in two frequency bands centered at 150 and 220 GHz, with two kilopixel focal plane arrays of NbSi Transition-Edge Sensors (TES) cooled down to 350 mK. A subset of the QUBIC instrument, the so called QUBIC Technological Demonstrator (TD), with a reduced number of detectors with respect to the full instrument, will be deployed and commissioned before the end of 2018. The voltage-biased TES are read out with Time Domain Multiplexing and an unprecedented multiplexing (MUX) factor equal to 128. This MUX factor is reached with two-stage multiplexing: a traditional one exploiting Superconducting QUantum Interference Devices (SQUIDs) at 1 K and a novel SiGe Application-Specific Integrated Circuit (ASIC) at 60 K. The former provides a MUX factor of 32, while the latter provides a further 4. Each TES array is composed of 256 detectors and read out with four modules of 32 SQUIDs and two ASICs. A custom software synchronizes and manages the readout and detector operation, while the TES are sampled at 780 Hz (100kHz/128 MUX rate). In this work we present the experimental characterization of the QUBIC TES arrays and their multiplexing readout chain, including time constant, critical temperature, and noise properties.

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Thermal architecture for the QUBIC cryogenic receiver

Cited by 5 publications

References 15 publications

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

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

QUBIC V: Cryogenic system design and performance

Performance of NbSi transition-edge sensors readout with a 128 MUX factor for the QUBIC experiment

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