QUBIC II: Spectro-Polarimetry with Bolometric Interferometry. (arXiv:2010.15119v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mousset_L/0/1/0/all/0/1">L. Mousset</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lerena_M/0/1/0/all/0/1">M.M. Gamboa Lerena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battistelli_E/0/1/0/all/0/1">E.S. Battistelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardis_P/0/1/0/all/0/1">P. de Bernardis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chanial_P/0/1/0/all/0/1">P. Chanial</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAlessandro_G/0/1/0/all/0/1">G. D'Alessandro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dashyan_G/0/1/0/all/0/1">G. Dashyan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petris_M/0/1/0/all/0/1">M. De Petris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grandsire_L/0/1/0/all/0/1">L. Grandsire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hamilton_J/0/1/0/all/0/1">J.-Ch. Hamilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Incardona_F/0/1/0/all/0/1">F. Incardona</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Landau_S/0/1/0/all/0/1">S. Landau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marnieros_S/0/1/0/all/0/1">S. Marnieros</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masi_S/0/1/0/all/0/1">S. Masi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mennella_A/0/1/0/all/0/1">A. Mennella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+OSullivan_C/0/1/0/all/0/1">C. O'Sullivan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piat_M/0/1/0/all/0/1">M. Piat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricciardi_G/0/1/0/all/0/1">G. Ricciardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scoccola_C/0/1/0/all/0/1">C.G. Scóccola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stolpovskiy_M/0/1/0/all/0/1">M. Stolpovskiy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tartari_A/0/1/0/all/0/1">A. Tartari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thermeau_J/0/1/0/all/0/1">J.-P. Thermeau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Torchinsky_S/0/1/0/all/0/1">S.A. Torchinsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Voisin_F/0/1/0/all/0/1">F. Voisin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zannoni_M/0/1/0/all/0/1">M. Zannoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ade_P/0/1/0/all/0/1">P. Ade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alberro_J/0/1/0/all/0/1">J.G. Alberro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Almela_A/0/1/0/all/0/1">A. Almela</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amico_G/0/1/0/all/0/1">G. Amico</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaldi_L/0/1/0/all/0/1">L.H. Arnaldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Auguste_D/0/1/0/all/0/1">D. Auguste</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aumont_J/0/1/0/all/0/1">J. Aumont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Azzoni_S/0/1/0/all/0/1">S. Azzoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banfi_S/0/1/0/all/0/1">S. Banfi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belier_B/0/1/0/all/0/1">B. Bélier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bau_A/0/1/0/all/0/1">A. Baù</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bennett_D/0/1/0/all/0/1">D. Bennett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berge_L/0/1/0/all/0/1">L. Bergé</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernard_J/0/1/0/all/0/1">J.-Ph. Bernard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bersanelli_M/0/1/0/all/0/1">M. Bersanelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bigot_Sazy_M/0/1/0/all/0/1">M.-A. Bigot-Sazy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonaparte_J/0/1/0/all/0/1">J. Bonaparte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonis_J/0/1/0/all/0/1">J. Bonis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bunn_E/0/1/0/all/0/1">E. Bunn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_D/0/1/0/all/0/1">D. Burke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buzi_D/0/1/0/all/0/1">D. Buzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cavaliere_F/0/1/0/all/0/1">F. Cavaliere</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chapron_C/0/1/0/all/0/1">C. Chapron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Charlassier_R/0/1/0/all/0/1">R. Charlassier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cerutti_A/0/1/0/all/0/1">A.C. Cobos Cerutti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Columbro_F/0/1/0/all/0/1">F. Columbro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coppolecchia_A/0/1/0/all/0/1">A. Coppolecchia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gasperis_G/0/1/0/all/0/1">G. De Gasperis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leo_M/0/1/0/all/0/1">M. De Leo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dheilly_S/0/1/0/all/0/1">S. Dheilly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duca_C/0/1/0/all/0/1">C. Duca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dumoulin_L/0/1/0/all/0/1">L. Dumoulin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Etchegoyen_A/0/1/0/all/0/1">A. Etchegoyen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fasciszewski_A/0/1/0/all/0/1">A. Fasciszewski</a>, et al. (72 additional authors not shown)
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.
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.
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