Browsing by Author "Hamilton, J. -Ch."

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    QUBIC I: Overview and science program
    (2022) Hamilton, J. -Ch.; Mousset, L.; Battistelli, E. S.; de Bernardis, P.; Bigot-Sazy, M. -A.; Chanial, P.; Charlassier, R.; D'Alessandro, G.; De Petris, M.; Lerena, M. M. Gamboa; Grandsire, L.; Landau, S.; Mandelli, S.; Marnieros, S.; Masi, S.; Mennella, A.; O'Sullivan, C.; Piat, M.; Ricciardi, G.; Scoccola, C. G.; Stolpovskiy, M.; Tartari, A.; Torchinsky, S. A.; Voisin, F.; Zannoni, M.; Ade, P.; Alberro, J. G.; Almela, A.; Amico, G.; Arnaldi, L. H.; Auguste, D.; Aumont, J.; Azzoni, S.; Banfi, S.; Bau, A.; Belier, B.; Bennett, D.; Berge, L.; Bernard, J. -Ph.; Bersanelli, M.; Bonaparte, J.; Bonis, J.; Bunn, E.; Burke, D.; Buzi, D.; Cavaliere, F.; Chapron, C.; Cerutti, A. C. Cobos; Columbro, F.; Coppolecchia, A.; De Gasperis, G.; De Leo, M.; Dheilly, S.; Duca, C.; Dumoulin, L.; Etchegoyen, A.; Fasciszewski, A.; Ferreyro, L. P.; Fracchia, D.; Franceschet, C.; Ganga, K. M.; Garcia, B.; Redondo, M. E. Garcia; Gaspard, M.; Gayer, D.; Gervasi, M.; Giard, M.; Gilles, V.; Giraud-Heraud, Y.; Berisso, M. Gomez; Gonzalez, M.; Gradziel, M.; Hampel, M. R.; Harari, D.; Henrot-Versille, S.; Incardona, F.; Jules, E.; Kaplan, J.; Kristukat, C.; Lamagna, L.; Loucatos, S.; Louis, T.; Maffei, B.; Marty, W.; Mattei, A.; May, A.; McCulloch, M.; Mele, L.; Melo, D.; Montier, L.; Mundo, L. M.; Murphy, J. A.; Murphy, J. D.; Nati, F.; Olivieri, E.; Oriol, C.; Paiella, A.; Pajot, F.; Passerini, A.; Pastoriza, H.; Pelosi, A.; Perbost, C.; Perciballi, M.; Pezzotta, F.; Piacentini, F.; Piccirillo, L.; Pisano, G.; Platino, M.; Polenta, G.; Prele, D.; Puddu, R.; Rambaud, D.; Rasztocky, E.; Ringegni, P.; Romero, G. E.; Salum, J. M.; Schillaci, A.; Scully, S.; Spinelli, S.; Stankowiak, G.; Supanitsky, A. D.; Thermeau, J. -P.; Timbie, P.; Tomasi, M.; Tucker, C.; Tucker, G.; Vigano, D.; Vittorio, N.; Wicek, F.; Wright, M.; Zullo, A.
    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 Mi-crowave Background (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 system-atic effects and polluted by various astrophysical foregrounds which can only be controlled through multichroic observations. QUBIC is designed to address these observational issues with a novel approach that combines 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 results in the ability to produce maps of the CMB polarization in multiple sub-bands within the two physical bands of the instrument (150 and 220 GHz). These features make QUBIC complementary to 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 not only the measurement of primordial B-modes, but also the measurement of Galactic foregrounds. We give forecasts for typical observations and measurements: with three years of integration on the sky and assuming perfect foreground removal as well as 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-mo des) Sigma(r) = 0.015.
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    QUBIC II: Spectral polarimetry with bolometric interferometry
    (2022) Mousset, L.; Lerena, M. M. Gamboa; Battistelli, E. S.; de Bernardis, P.; Chanial, P.; D'Alessandro, G.; Dashyan, G.; De Petris, M.; Grandsire, L.; Hamilton, J. -Ch.; Incardona, F.; Landau, S.; Marnieros, S.; Masi, S.; Mennella, A.; O'Sullivan, C.; Piat, M.; Ricciardi, G.; Scoccola, C. G.; Stolpovskiy, M.; Tartari, A.; Thermeau, J. -P.; Torchinsky, S. A.; Voisin, F.; Zannoni, M.; Ade, P.; Alberro, J. G.; Almela, A.; Amico, G.; Arnaldi, L. H.; Auguste, D.; Aumont, J.; Azzoni, S.; Banfi, S.; Bau, A.; Belier, B.; Bennett, D.; Berge, L.; Bernard, J. -Ph.; Bersanelli, M.; Bigot-Sazy, M. -A.; Bonaparte, J.; Bonis, J.; Bunn, E.; Burke, D.; Buzi, D.; Cavaliere, F.; Chapron, C.; Charlassier, R.; Cerutti, A. C. Cobos; Columbro, F.; Coppolecchia, A.; De Gasperis, G.; De Leo, M.; Dheilly, S.; Duca, C.; Dumoulin, L.; Etchegoyen, A.; Fasciszewski, A.; Ferreyro, L. P.; Fracchia, D.; Franceschet, C.; Ganga, K. M.; Garcia, B.; Redondo, M. E. Garcia; Gaspard, M.; Gayer, D.; Gervasi, M.; Giard, M.; Gilles, V.; Giraud-Heraud, Y.; Berisso, M. Gomez; Gonzalez, M.; Gradziel, M.; Hampel, M. R.; Harari, D.; Henrot-Versille, S.; Jules, E.; Kaplan, J.; Kristukat, C.; Lamagna, L.; Loucatos, S.; Louis, T.; Maffei, B.; Mandelli, S.; Marty, W.; Mattei, A.; May, A.; McCulloch, M.; Mele, L.; Melo, D.; Montier, L.; Mundo, L. M.; Murphy, J. A.; Murphy, J. D.; Nati, F.; Olivieri, E.; Oriol, C.; Paiella, A.; Pajot, F.; Passerini, A.; Pastoriza, H.; Pelosi, A.; Perbost, C.; Perciballi, M.; Pezzotta, F.; Piacentini, F.; Piccirillo, L.; Pisano, G.; Platino, M.; Polenta, G.; Prele, D.; Puddu, R.; Rambaud, D.; Rasztocky, E.; Ringegni, P.; Romero, G. E.; Salum, J. M.; Schilaci, A.; Scully, S.; Spinelli, S.; Stankowiak, G.; Supanitsky, A. D.; Timbie, P.; Tomasi, M.; Tucker, C.; Tucker, G.; Vigano, D.; Vittorio, N.; Wicek, F.; Wright, M.; Zullo, A.
    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 mi-crowave 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-mo de polarization of the sky at millimeter wavelengths. We consider the specific cases of point source reconstruc-tion 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.