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QUBIC II: Spectral polarimetry with bolometric interferometry

2022; Institute of Physics; Volume: 2022; Issue: 04 Linguagem: Inglês

10.1088/1475-7516/2022/04/035

1475-7516

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, Federico Incardona, Susana J. Landau, S. Marnieros, S. Masi, A. Mennella, C. O’Sullivan, M. Piat, Giulia Ricciardi, Claudia G. Scóccola, Mikhail Stolpovskiy, A. Tartari, J.-P. Thermeau, S. Torchinsky, F. Voisin, M. Zannoni, P. A. R. Ade, J.G. Alberro, A. Almela, G. Amico, Horacio Arnaldi, D. Auguste, J. Aumont, S. Azzoni, Stefano Banfi, A. Baù, B. Bélier, D. Bennett, L. Bergé, J.-P. Bernard, M. Bersanelli, M.-A. Bigot-Sazy, J. Bonaparte, J. Bonis, Emory F. Bunn, David Burke, D. Buzi, F. Cavaliere, C. Chapron, R. Charlassier, Agustín 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. Ganga, B. Garćıa, M.E. García Redondo, M. Gaspard, D. Gayer, M. Gervasi, M. Giard, V. Gilles, Y. Giraud–Héraud, M. Gómez Berisso, Manuel González, M. Gradziel, Matías Rolf Hampel, D. Harari, S. Henrot–Versillé, E. Jules, J. Kaplan, C. Kristukat, L. Lamagna, S. Loucatos, Thibaut Louis, B. Maffei, S. Mandelli, 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, Gustavo E. Romero, J. M. Salum, A. Schillaci, S. Scully, S. Spinelli, G. Stankowiak, A. D. Supanitsky, P. Timbie, M. Tomasi, C. Tucker, Gregory S. Tucker, Daniele Viganò, N. Vittorio, F. Wicek, M. Wright, Angelo Zullo,

Galaxies: Formation, Evolution, Phenomena

Bolometric interferometry is a novel technique that has the ability to perform spectral 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 in post-processing of the data. 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 spectral imaging, especially the correlations between sub-bands, using end-to-end simulations together with a fast noise simulator. We conclude showing that spectral imaging performance are nearly optimal up to five sub-bands in the case of QUBIC.