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26 April 2024

» arxiv » 2010.15119

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QUBIC II: Spectro-Polarimetry with Bolometric Interferometry
L. Mousset ; M.M. Gamboa Lerena ; E.S. Battistelli ; P. de Bernardis ; P. Chanial ; G. D'Alessandro ; G. Dashyan ; M. De Petris ; L. Grandsire ; J.-Ch. Hamilton ; F. Incardona ; S. Landau ; S. Marnieros ; S. Masi ; A. Mennella ; C. O'Sullivan ; M. Piat ; G. Ricciardi ; C.G. Scóccola ; M. Stolpovskiy ; A. Tartari ; J.-P. Thermeau ; 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 ; M.-A. Bigot-Sazy ; J. Bonaparte ; J. Bonis ; E. Bunn ; D. Burke ; D. Buzi ; F. Cavaliere ; C. Chapron ; R. Charlassier ; 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 ; 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 ; E. Rasztocky ; P. Ringegni ; G.E. Romero ; J.M. Salum ; A. Schillaci ; S. Scully ; S. Spinelli ; G. Stankowiak ; A.D. Supanitsky ; P. Timbie ; M. Tomasi ; G. Tucker ; C. Tucker ; D. Viganò ; N. Vittorio ; F. Wicek ; M. Wright ; A. Zullo ;
Date:	28 Oct 2020
Abstract:	Bolometric Interferometry is a novel technique that has the ability to perform spectro-imaging. A Bolometric Interferometer observes the sky in a wide frequency band and can reconstruct sky maps in several sub-bands within the physical band. This provides a powerful spectral method to discriminate between the Cosmic Microwave Background (CMB) and astrophysical foregrounds. In this paper, the methodology is illustrated with examples based on the Q & U Bolometric Interferometer for Cosmology (QUBIC) which is a ground-based instrument designed to measure the B-mode polarization of the sky at millimeter wavelengths. We consider the specific cases of point source reconstruction and Galactic dust mapping and we characterize the Point Spread Function as a function of frequency. We study the noise properties of spectro-imaging, especially the correlations between sub-bands, using end-to-end simulations together with a fast noise simulator. We conclude showing that spectro-imaging performance are nearly optimal up to five sub-bands in the case of QUBIC.
Source:	arXiv, 2010.15119
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