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QUBIC I: Overview and ScienceProgram | | J.-Ch. Hamilton
; L. Mousset
; E.S. Battistelli
; M.-A. Bigot-Sazy
; P. Chanial
; R. Charlassier
; G. D'Alessandro
; P. de Bernardis
; M. De Petris
; M.M. Gamboa Lerena
; L. Grandsire
; S. Lau
; S. Marnieros
; S. Masi
; A. Mennella
; C. O'Sullivan
; M. Piat
; G. Riccardi
; C. Scóccola
; M. Stolpovskiy
; A. Tartari
; S.A. Torchinsky
; F. Voisin
; M. Zannoni
; P. Ade
; J.G. Alberro
; A. Almela
; G. Amico
; L.H. Arnaldi
; D. Auguste
; J. Aumont
; S. Azzoni
; S. Banfi
; B. Bélier
; A. Baù
; D. Bennett
; L. Bergé
; J.-Ph. Bernard
; M. Bersanelli
; J. Bonaparte
; J. Bonis
; E. Bunn
; D. Burke
; D. Buzi
; F. Cavaliere
; C. Chapron
; A.C. Cobos Cerutti
; F. Columbro
; A. Coppolecchia
; G. De Gasperis
; M. De Leo
; S. Dheilly
; C. Duca
; L. Dumoulin
; A. Etchegoyen
; A. Fasciszewski
; L.P. Ferreyro
; D. Fracchia
; C. Franceschet
; K.M. Ganga
; B. García
; M.E. García Redondo
; M. Gaspard
; D. Gayer
; M. Gervasi
; M. Giard
; V. Gilles
; Y. Giraud-Heraud
; M. Gómez Berisso
; M. González
; M. Gradziel
; M.R. Hampel
; D. Harari
; S. Henrot-Versillé
; F. Incardona
; E. Jules
; J. Kaplan
; C. Kristukat
; L. Lamagna
; S. Loucatos
; T. Louis
; B. Maffei
; W. Marty
; A. Mattei
; A. May
; M. McCulloch
; L. Mele
; D. Melo
; L. Montier
; L.M. Mundo
; J.A. Murphy
; J.D. Murphy
; F. Nati
; E. Olivieri
; C. Oriol
; A. Paiella
; F. Pajot
; A. Passerini
; H. Pastoriza
; A. Pelosi
; C. Perbost
; M. Perciballi
; F. Pezzotta
; F. Piacentini
; L. Piccirillo
; G. Pisano
; M. Platino
; G. Polenta
; D. Prêle
; R. Puddu
; D. Rambaud
; P. Ringegni
; G.E. Romero
; E. Rasztocky
; J.M. Salum
; A. Schillaci
; S. Scully
; S. Spinelli
; G. Stankowiak
; A.D. Supanitsky
; J.-P. Thermeau
; P. Timbie
; M. Tomasi
; C. Tucker
; G. Tucker
; D. Viganò
; N. Vittorio
; F. Wicek
; M. Wright
; A. Zullo
; | | Date: |
4 Nov 2020 | | Abstract: | QUBIC is a novel kind of polarimeter optimized for the measurement of the
B-mode polarization of the Cosmic Microwave Background, 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
allows producing maps of the CMB polarization in multiple sub-bands 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 the measurement of primordial B-modes
and Galactic foregrounds. We give forecasts for typical observations and
measurements: with three years of integration, assuming perfect foreground
removal and 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)
$sigma(r)=0.015$. 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 $sigma(r)=0.021$. | | Source: | arXiv, 2011.02213 | | Services: | Forum | Review | PDF | Favorites | |
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