STATUS OF QUBIC THE QU BOLOMETRIC INTERFEROMETER FOR COSMOLOGY

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STATUS OF QUBIC, THE Q&U BOLOMETRIC

INTERFEROMETER FOR COSMOLOGY

L. Mousset1, P. Ade2, A. Almela3, G. Amico4, L.H. Arnaldi5, J. Aumont1, S. Banﬁ6,7,

E.S. Battistelli4,8, B. B´elier9, L. Berg´e10, J.-Ph. Bernard1, P. de Bernardis4,8,

M. Bersanelli11,12, J. Bonaparte13, J.D. Bonilla3, E. Bunn14, D. Buzi4, D. Camilieri15,

F. Cavaliere11,12, P. Chanial15, C. Chapron15, S. Colombo11,12, F. Columbro4,8,

A. Coppolecchia4,8, B. Costanza16,17, G. D’Alessandro4,8, G. De Gasperis18,19,

M. De Leo4,20, M. De Petris4,8, N. Del Castillo3, S. Dheilly15, A. Etchegoyen3, M. Fam´a5,

L.P. Ferreyro3, C. Franceschet11,12, M.M. Gamboa Lerena3, K.M. Ganga15, B. Garc´ıa3,

M.E. Garc´ıa Redondo3, D. Gayer21, J.M. Geria3, M. Gervasi6,7, M. Giard1, V. Gilles4,

M. G´omez Berisso5, M. Gonz´alez15, M. Gradziel21, L. Grandsire15, J.-Ch. Hamilton15,

M.R. Hampel3, G. Isopi4,8, J. Kaplan15, C. Kristukat22, L. Lamagna4,8, F. Lazarte3,

S. Loucatos15,23, A. Mancilla3, D. Mandelli11,12, E. Manzan11,12, S. Marnieros10,

W. Marty1, S. Masi4,8, A. May24, J. Maya3, M. McCulloch24, L. Mele4,8, D. Melo3,

A. Mennella11,12, N. Mir´on-Granese16,17, L. Montier1, N. M¨uller3, J.D. Murphy21,

F. Nati6,7, C. O’Sullivan21, A. Paiella4,8, F. Pajot1, S.Paradiso11,12, A. Passerini6,7,

A. Pelosi8, M. Perciballi8, F. Pezzotta11,12, F. Piacentini4,8, M. Piat15, L. Piccirillo24,

G. Pisano4,8, M. Platino3, G. Polenta25, D. Prˆele15, D. Rambaud1, E. Rasztocky26,

M. R´egnier15, C. Reyes3, F. Rodr´ıguez3, C.A. Rodr´ıguez3, G.E. Romero26, J.M. Salum3,

A. Schillaci27, C.G. Sc´occola16,17, G. Stankowiak15, A.D. Supanitsky3, A. Tartari28,

J.-P. Thermeau15, P. Timbie29, S.A. Torchinsky15,30, G. Tucker31, C. Tucker2,

L. Vacher1, F. Voisin15, M. Wright24, M. Zannoni6,7, and A. Zullo8

1Institut de Recherche en Astrophysique et Plan´etologie (CNRS-INSU), 9 Av. du

Colonel Roche, 31400 Toulouse, France

2Cardiﬀ University, Cardiﬀ CF10 3AT, United Kingdom

3Instituto de Tecnolog´ıas en Detecci´on y Astropart´ıculas (CNEA, CONICET, UNSAM),

Av. Gral Paz 1499 - San Mart´ın, Argentina

4Universit`a di Roma — La Sapienza, Piazzale Aldo Moro, 5, 00185 Roma, Italy

5Centro At´omico Bariloche and Instituto Balseiro (CNEA), Av. Exequiel Bustillo 9500,

San Carlos de Bariloche, Argentina

6Universit`a di Milano — Bicocca, Piazza dell’Ateneo Nuovo, 1, 20126 Milano, Italy

7INFN Milano-Bicocca, Ediﬁcio U2, Piazza della Scienza, 3 - I-20126 Milano, Italy

8INFN sezione di Roma, Piazzale Aldo Moro, 2, 00185 Roma, Italy

9Centre de Nanosciences et de Nanotechnologies, 15 Rue Georges Cl´emenceau, 91405

Orsay Cedex, France

10Laboratoire de Physique des 2 Inﬁnis Ir`ene Joliot-Curie CNRS-IN2P3, Universit´e

Paris-Saclay, Bˆat. 100, 15 rue Georges Cl´emenceau, 91405 Orsay cedex, France

11Universita degli studi di Milano, Via Celoria 16, 20122 Milano, Italy

12INFN sezione di Milano, Via Celoria 16, 20122 Milano, Italy

13Centro At´omico Constituyentes (CNEA), Av. Gral. Paz 1499, B1650 Villa Maip´u,

Argentina

14University of Richmond, Richmond, 410 Westhampton Way, Richmond, VA 23173,

United States

15Astroparticule et Cosmologie, Universit´e de Paris, CNRS, 10 Rue Alice Domon et

arXiv:2210.03161v1 [astro-ph.IM] 6 Oct 2022

L´eonie Duquet, 75013 Paris, France

16Facultad de Ciencias Astron´omicas y Geof´ısicas, Universidad Nacional de La Plata,

Paseo del Bosque S/N, B1900FWA La Plata, Argentina

17Consejo Nacional de Investigaciones Cient´ıﬁcas y T´ecnicas (CONICET), Godoy Cruz

2290, 1425, Ciudad Aut´onoma de Buenos Aires, Argentina

18Dipartimento di ﬁsica, Universit`a di Roma — Tor Vergata, Viale della Ricerca

Scientiﬁca, 1, 00133 Roma, Italy

19INFN sezione di Roma2, Via della Ricerca Scientiﬁca, 1, 00133 Roma, Italy

20University of Surrey, Stag Hill, University Campus, Guildford GU2 7XH, United

Kingdom

21Department of Experimental Physics, National University of Ireland, Maynooth, Co.

Kildare, Ireland

22Escuela de Ciencia y Tecnolog´ıa (UNSAM) and Centro At´omico Constituyentes

(CNEA), Tornav´ıas Mart´ın de Irigoyen No.3100, B1650 Villa Lynch, Argentina

23IRFU, CEA, Universit´e Paris-Saclay, Bˆat 141, F-91191 Gif-sur-Yvette, France

24University of Manchester, Oxford Rd, Manchester M13 9PL, United Kingdom

25Italian Space Agency, Via del Politecnico snc 00133, Roma, Italy

26Instituto Argentino de Radioastronom´ıa (CONICET, CIC), Camino Gral. Belgrano

Km 40, Berazategui, Argentina

27Department of Physics, California Institute of Technology, Pasadena, CA 91125, USA

28INFN — Pisa Section, Largo Bruno Pontecorvo, 3/Ediﬁcio C, 56127 Pisa, Italy

29Department of Physics, University of Wisconsin Madison, 1150 University Ave,

Madison WI 53703, USA

30Observatoire de Paris, Universit´e Paris Science et Lettres, 61 Av. de l’Observatoire,

F-75014 Paris, France

31Brown University, Providence, RI 02912, USA

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 Back-

ground (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 mul-

tichroic observations. QUBIC is designed to address these observational issues with a novel

approach that combines the advantages of interferometry in terms of control of instrumen-

tal systematics with those of bolometric detectors in terms of wide-band, background-limited

sensitivity.

1 Introduction

The quest for B-mode polarization of the Cosmic Microwave Background (CMB) is among

the major challenges of observational cosmology. Cosmic inﬂation predicts primordial scalar

perturbations of the metric (density ﬂuctuations), but also tensor perturbations, equivalent to

primordial gravitational waves. These tensor modes should be imprinted in the CMB polar-

ization ﬂuctuations with a very speciﬁc signature: odd-parity patterns (curl term), known as

B-modes 6. The amplitude of the tensor modes, relative to the scalar modes, is parametrized

by the so called tensor-to-scalar ratio r. The expected signal is weak, requiring high sensitivity

detectors. In addition, astrophysical foregrounds produce non-primordial B-mode polarization,

such as thermal emission from dust grains in the Galaxy.

The Q&U Bolometric Interferometer for Cosmology (QUBIC) was designed to address the

B-mode detection challenge 1. Characterization and calibration of a Technical Demonstrator

(TD) started in 2018, at Astroparticle Physics & Cosmology (APC) laboratory 3. In May 2021,

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STATUSOFQUBIC,THEQ&UBOLOMETRICINTERFEROMETERFORCOSMOLOGYL.Mousset1,P.Ade2,A.Almela3,G.Amico4,L.H.Arnaldi5,J.Aumont1,S.Ban6,7,E.S.Battistelli4,8,B.Belier9,L.Berge10,J.-Ph.Bernard1,P.deBernardis4,8,M.Bersanelli11,12,J.Bonaparte13,J.D.Bonilla3,E.Bunn14,D.Buzi4,D.Camilieri15,F.Cavaliere11,12,P.Chania...

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