QUBIC VIII: Optical design and performance

O'Sullivan, C.; De Petris, M.; Amico, G.; Battistelli, E. S.; Burke, D.; Buzi, D.; Chapron, C.; Conversi, L.; D'Alessandro, G.; de Bernardis, P.; De Leo, M.; Gayer, D.; Grandsire, L.; Hamilton, J. -Ch.; Marnieros, S.; Masi, S.; Mattei, A.; Mennella, A.; Mousset, L.; Murphy, J. D.; Pelosi, A.; Perciballi, M.; Piat, M.; Scully, S.; Tartari, A.; Torchinsky, S. A.; Voisin, F.; Zannoni, M.; Zullo, A.; Ade, P.; Alberro, J. G.; Almela, A.; Arnaldi, L. H.; Auguste, D.; Aumont, J.; Azzoni, S.; Banfi, S.; Bélier, B.; Bau, A.; Bennett, D.; Berge, L.; Bernard, J. -Ph.; Bersanelli, M.; Bigot-Sazy, M. -A.; Bonaparte, J.; Bonis, J.; Bunn, E.; Cavaliere, F.; Chanial, P.; Charlassier, R.; Cerutti, A. C. Cobos; Columbro, F.; Coppolecchia, A.; De Gasperis, G.; Dheilly, S.; Duca, C.; Dumoulin, L.; Etchegoyen, A.; Fasciszewski, A.; Ferreyro, L. P.; Fracchia, D.; Franceschet, C.; Lerena, M. M. Gamboa; Ganga, K. M.; García, B.; Redondo, M. E. García; Gaspard, M.; Gervasi, M.; Giard, M.; Gilles, V.; Giraud-Heraud, Y.; GomezBerisso, M.; 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.; May, A.; McCulloch, M.; Mele, L.; Melo, D.; Montier, L.; Mundo, L. M.; Murphy, J. A.; Nati, F.; Olivieri, E.; Oriol, C.; Paiella, A.; Pajot, F.; Passerini, A.; Pastoriza, H.; Perbost, C.; Pezzotta, F.; Piacentini, F.; Piccirillo, L.; Pisano, G.; Platino, M.; Polenta, G.; Prele, D.; Puddu, R.; Rambaud, D.; Ringegni, P.; Romero, G. E.; Rasztocky, E.; Salum, J. M.; Schillaci, A.; Scoccola, C.; Spinelli, S.; Stankowiak, G.; Stolpovskiy, M.; Supanitsky, A. D.; Thermeau, J. -P.; Timbie, P.; Tomasi, M.; Tucker, G.; Tucker, C.; Vigano, D.; Vittorio, N.; Wicek, F.; Wright, M.

doi:10.48550/arxiv.2008.10119

Cited by 9 publications

(36 citation statements)

References 10 publications

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“…The left panel of figure 1 shows the array of back-to-back feedhorns of the Full Instrument (FI). The back-to-back feedhorn array makes 400 pupils arranged on a rectangular grid within a circle (see [27,28] for more details). The beam looking at the sky is called the primary beam, and secondary beam is the one looking toward the focal plane.…”

Section: Bolometric Interferometry As Synthesized Imagingmentioning

confidence: 99%

“…Detailed information about QUBIC can be found in the companion papers: Scientific overview and expected performance of QUBIC [23], Characterization of the Technological Demonstrator (TD) [22], Transition-Edge Sensors and readout characterization [24], Cryogenic system performance [25], Half Wave Plate rotator design and performance [26], Feedhorn-switches system of the TD [27], and Optical design and performance [28].…”

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confidence: 99%

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QUBIC II: Spectro-Polarimetry with Bolometric Interferometry

Mousset,

Lerena,

Battistelli

et al. 2020

Preprint

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Bolometric Interferometry is a novel technique that has the ability to perform spectroimaging. 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-toend simulations together with a fast noise simulator. We conclude showing that spectroimaging performance are nearly optimal up to five sub-bands in the case of QUBIC.

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Section: Bolometric Interferometry As Synthesized Imagingmentioning

confidence: 99%

mentioning

confidence: 99%

QUBIC II: Spectro-Polarimetry with Bolometric Interferometry

Mousset,

Lerena,

Battistelli

et al. 2020

Preprint

Self Cite

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“…The Q and U Bolometric Interferometer (QUBIC) is designed with particular attention to the limitation and control of systematics [2]. See also in this series of papers [3] for the optics design, [4] for the cryogenics design, and [5] for the readout electronics. QUBIC uses the technique of interferometry which leads to the possibility of doing "self-calibration" in order to have exquisite control of instrument systematics [6].…”

Section: Introductionmentioning

confidence: 99%

QUBIC III: Laboratory Characterization

Torchinsky,

Hamilton,

Piat

et al. 2020

Preprint

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A prototype version of the Q & U Bolometric Interferometer for Cosmology (QUBIC) underwent a campaign of testing in the laboratory at Astroparticle Physics and Cosmology in Paris. We report the results of this Technological Demonstrator which successfully shows the feasibility of the principle of Bolometric Interferometry. Characterization of QUBIC includes the measurement of the synthesized beam, the measurement of interference fringes, and the measurement of polarization performance. A modulated and frequency tunable millimetre-wave source in the telescope far-field is used to simulate a point source. The QUBIC pointing is scanned across the point source to produce beam maps. Polarization modulation is measured using a rotating Half Wave Plate. The measured beam matches well to the theoretical simulations and gives QUBIC the ability to do spectro imaging. The polarization performance is excellent with less than 0.5% cross-polarization rejection. QUBIC is ready for deployment on the high altitude site at Alto Chorillo, Argentina to begin scientific operations.

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“…The inner side of the forebaffle can be either perfectly reflective or absorbing. We also have the option of a 5-mm thick layer of dielectric meant to mimic ECCOSORB HR-10, 15 with a relative electric permittivity ε r = 3.54 and loss tangent δ = 0.057.…”

Section: Baffling the Telescopementioning

confidence: 99%

“…To mitigate possible diffraction effects at the outer rim of the forebaffle, 15 a curved flare can be added, whose radius is nλ, with λ corresponding to the wavelength of our source. The ground screen is, at its base, a cylinder 7 m in radius.…”

Section: Baffling the Telescopementioning

confidence: 99%

Modeling sidelobe response for ground-based mm-wavelength telescopes with the geometrical theory of diffraction

Adler,

Gudmundsson

2020

Preprint

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Accurate optical modeling is important for the design and characterisation of current and next-generation experiments studying the Cosmic Microwave Background (CMB). Geometrical Optics (GO) cannot model diffractive effects. In this work, we discuss two methods that incorporate diffraction, Physical Optics (PO) and the Geometrical Theory of Diffraction (GTD). We simulate the optical response of a ground-based two-lens refractor design shielded by a ground screen with time-reversed simulations. In particular, we use GTD to determine the interplay between the design of the refractor's forebaffle and the sidelobes caused by interaction with the ground screen.

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QUBIC VIII: Optical design and performance

Cited by 9 publications

References 10 publications

QUBIC II: Spectro-Polarimetry with Bolometric Interferometry

QUBIC II: Spectro-Polarimetry with Bolometric Interferometry

QUBIC III: Laboratory Characterization

Modeling sidelobe response for ground-based mm-wavelength telescopes with the geometrical theory of diffraction

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