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1. QUBIC - The Q&U Bolometric Interferometer for Cosmology - A novel way to look at the polarized Cosmic Microwave Background

Author

Mennella, A., Ade, P. A. R., Aumont, J., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bélier, B., Bennett, D., Bergé, L., Bernard, J. Ph., Bersanelli, M., Bigot-Sazy, M. A., Bleurvacq, N., Bordier, G., Brossard, J., Bunn, E. F., Burke, D. P., Buzi, D., Buzzelli, A., Cammilleri, D., Cavaliere, F., Chanial, P., Chapron, C., Columbro, F., Coppi, G., Coppolecchia, A., Couchot, F., D'Agostino, R., D'Alessandro, G., de Bernardis, P., De Gasperis, G., De Leo, M., De Petris, M., Decourcelle, T., Del Torto, F., Dumoulin, L., Etchegoyen, A., Franceschet, C., Garcia, B., Gault, A., Gayer, D., Gervasi, M., Ghribi, A., Giard, M., Giraud-Héraud, Y., Gradziel, M., Grandsire, L., Hamilton, J. Ch., Harari, D., Haynes, V., Henrot-Versillé, S., Holtzer, N., Incardona, F., Kaplan, J., Korotkov, A., Krachmalnicoff, N., Lamagna, L., Lande, J., Loucatos, S., Lowitz, A., Lukovic, V., Maffei, B., Marnieros, S., Martino, J., Masi, S., May, A., McCulloch, M., Medina, M. C., Mele, L., Melhuish, S., Montier, L., Murphy, A., Néel, D., Ng, M. W., O'Sullivan, C., Paiella, A., Pajot, F., Passerini, A., Pelosi, A., Perbost, C., Perdereau, O., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Préle, D., Puddu, R., Rambaud, D., Rigaut, O., Romero, G. E., Salatino, M., Schillaci, A., Scully, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Torchinsky, S., Tristram, M., Tucker, C., Tucker, G., Viganò, D., Vittorio, N., Voisin, F., Watson, B., Zannoni, M., and Zullo, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

In this paper we describe QUBIC, an experiment that takes up the challenge posed by the detection of primordial gravitational waves with a novel approach, that combines the sensitivity of state-of-the art bolometric detectors with the systematic effects control typical of interferometers. The so-called "self-calibration" is a technique deeply rooted in the interferometric nature of the instrument and allows us to clean the measured data from instrumental effects. The first module of QUBIC is a dual band instrument (150 GHz and 220 GHz) that will be deployed in Argentina during the Fall 2018., Comment: Presented at the EPS Conference on High Energy Physics, Venice (Italy), 5-12 July 2017 Accepted for publication in conference proceedings

Published
2018

2. QUBIC Technical Design Report

Author

Aumont, J., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bélier, B., Bennett, D., Bergé, L., Bernard, J. Ph., Bersanelli, M., Bigot-Sazy, M. A., Bleurvacq, N., Bordier, G., Brossard, J., Bunn, E. F., Buzi, D., Buzzelli, A., Cammilleri, D., Cavaliere, F., Chanial, P., Chapron, C., Coppi, G., Coppolecchia, A., Couchot, F., D'Agostino, R., D'Alessandro, G., de Bernardis, P., De Gasperis, G., De Petris, M., Decourcelle, T., Del Torto, F., Dumoulin, L., Etchegoyen, A., Franceschet, C., Garcia, B., Gault, A., Gayer, D., Gervasi, M., Ghribi, A., Giard, M., Giraud-Héraud, Y., Gradziel, M., Grandsire, L., Hamilton, J. Ch., Harari, D., Haynes, V., Henrot-Versillé, S., Holtzer, N., Kaplan, J., Korotkov, A., Lamagna, L., Lande, J., Loucatos, S., Lowitz, A., Lukovic, V., Maffei, B., Marnieros, S., Martino, J., Masi, S., May, A., McCulloch, M., Medina, M. C., Melhuish, S., Mennella, A., Montier, L., Murphy, A., Néel, D., Ng, M. W., O'Sullivan, C., Paiella, A., Pajot, F., Passerini, A., Pelosi, A., Perbost, C., Perdereau, O., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Prêle, D., Puddu, R., Rambaud, D., Rigaut, O., Romero, G. E., Salatino, M., Schillaci, A., Scully, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Tristram, M., Tucker, G., Viganò, D., Vittori, N., Voisin, F., Watson, B., Zannoni, M., and Zullo, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

QUBIC is an instrument aiming at measuring the B mode polarisation anisotropies at medium scales angular scales (30-200 multipoles). The search for the primordial CMB B-mode polarization signal is challenging, because of many difficulties: smallness of the expected signal, instrumental systematics that could possibly induce polarization leakage from the large E signal into B, brighter than anticipated polarized foregrounds (dust) reducing to zero the initial hope of finding sky regions clean enough to have a direct primordial B-modes observation. The QUBIC instrument is designed to address all aspects of this challenge with a novel kind of instrument, a Bolometric Interferometer, combining the background-limited sensitivity of Transition-Edge-Sensors and the control of systematics allowed by the observation of interference fringe patterns, while operating at two frequencies to disentangle polarized foregrounds from primordial B mode polarization. Its characteristics are described in details in this Technological Design Report., Comment: 139 pages ; high resolution version can be found on the qubic website (http://qubic.in2p3.fr/QUBIC/Home.html) minor changes : update author list & affiliations ; correct title

Published
2016

3. QUBIC: The QU Bolometric Interferometer for Cosmology

Author

The QUBIC collaboration, Battistelli, E., Baù, A., Bennett, D., Bergé, L., Bernard, J. -Ph., de Bernardis, P., Bounab, A., Bréelle, É., Bunn, E. F., Calvo, M., Charlassier, R., Collin, S., Cruciani, A., Curran, G., Dumoulin, L., Gault, A., Gervasi, M., Ghribi, A., Giard, M., Giordano, C., Giraud-Héraud, Y., Gradziel, M., Guglielmi, L., Hamilton, J. -Ch., Haynes, V., Kaplan, J., Korotkov, A., Landé, J., Maffei, B., Maiello, M., Malu, S., Marnieros, S., Masi, S., Murphy, A., Nati, F., O'Sullivan, C., Pajot, F., Passerini, A., Peterzen, S., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Polenta, G., Prêle, D., Romano, D., Rosset, C., Salatino, M., Schillacci, A., Sironi, G., Sordini, R., Spinelli, S., Tartari, A., Timbie, P., Tucker, G., Vibert, L., Voisin, F., Watson, R. A., and Zannoni, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

One of the major challenges of modern cosmology is the detection of B-mode polarization anisotropies in the CMB. These originate from tensor fluctuations of the metric produced during the inflationary phase. Their detection would therefore constitute a major step towards understanding the primordial Universe. The expected level of these anisotropies is however so small that it requires a new generation of instruments with high sensitivity and extremely good control of systematic effects. We propose the QUBIC instrument based on the novel concept of bolometric interferometry, bringing together the sensitivity advantages of bolometric detectors with the systematics effects advantages of interferometry. Methods: The instrument will directly observe the sky through an array of entry horns whose signals will be combined together using an optical combiner. The whole set-up is located inside a cryostat. Polarization modulation will be achieved using a rotating half-wave plate and interference fringes will be imaged on two focal planes (separated by a polarizing grid) tiled with bolometers. We show that QUBIC can be considered as a synthetic imager, exactly similar to a usual imager but with a synthesized beam formed by the array of entry horns. Scanning the sky provides an additional modulation of the signal and improve the sky coverage shape. The usual techniques of map-making and power spectrum estimation can then be applied. We show that the sensitivity of such an instrument is comparable with that of an imager with the same number of horns. We anticipate a low level of beam-related systematics thanks to the fact that the synthesized beam is determined by the location of the primary horns. Other systematics should be under good control thanks to an autocalibration technique, specific to our concept, that will permit the accurate determination of most of the systematics parameters., Comment: 12 pages, 10 figures, submitted to Astronomy and Astrophysics

Published
2010
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4. Bandwidth in bolometric interferometry

Author

Charlassier, R., Bunn, E. F., Hamilton, J. -Ch., Kaplan, J., and Malu, S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Bolometric Interferometry is a technology currently under development that will be first dedicated to the detection of B-mode polarization fluctuations in the Cosmic Microwave Background. A bolometric interferometer will have to take advantage of the wide spectral detection band of its bolometers in order to be competitive with imaging experiments. A crucial concern is that interferometers are presumed to be importantly affected by a spoiling effect known as bandwidth smearing. In this paper, we investigate how the bandwidth modifies the work principle of a bolometric interferometer and how it affects its sensitivity to the CMB angular power spectra. We obtain analytical expressions for the broadband visibilities measured by broadband heterodyne and bolometric interferometers. We investigate how the visibilities must be reconstructed in a broadband bolometric interferometer and show that this critically depends on hardware properties of the modulation phase shifters. Using an angular power spectrum estimator accounting for the bandwidth, we finally calculate the sensitivity of a broadband bolometric interferometer. A numerical simulation has been performed and confirms the analytical results. We conclude (i) that broadband bolometric interferometers allow broadband visibilities to be reconstructed whatever the kind of phase shifters used and (ii) that for dedicated B-mode bolometric interferometers, the sensitivity loss due to bandwidth smearing is quite acceptable, even for wideband instruments (a factor 2 loss for a typical 20% bandwidth experiment)., Comment: 13 pages, 14 figures, submitted to A&A

Published
2009
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5. Frequentist Estimation of Cosmological Parameters from the MAXIMA-1 Cosmic Microwave Background Anisotropy Data

Author

Abroe, M. E., Balbi, A., Borrill, J., Bunn, E. F., Ferreira, P. G., Hanany, S., Jaffe, A. H., Lee, A. T., Olive, K. A., Rabii, B., Richards, P. L., Smoot, G. F., Stompor, R., Winant, C. D., and Wu, J. H. P.

Subjects
Astrophysics
Abstract

We use a frequentist statistical approach to set confidence intervals on the values of cosmological parameters using the MAXIMA-1 and COBE measurements of the angular power spectrum of the cosmic microwave background. We define a $\Delta \chi^{2}$ statistic, simulate the measurements of MAXIMA-1 and COBE, determine the probability distribution of the statistic, and use it and the data to set confidence intervals on several cosmological parameters. We compare the frequentist confidence intervals to Bayesian credible regions. The frequentist and Bayesian approaches give best estimates for the parameters that agree within 15%, and confidence interval-widths that agree within 30%. The results also suggest that a frequentist analysis gives slightly broader confidence intervals than a Bayesian analysis. The frequentist analysis gives values of \Omega=0.89{+0.26\atop -0.19}, \Omega_{\rm B}h^2=0.026{+0.020\atop -0.011} and n=1.02{+0.31\atop -0.10}, and the Bayesian analysis gives values of \Omega=0.98{+0.14\atop -0.19}, \Omega_{\rm B}h^2=0.0.029{+0.015\atop-0.010}, and $n=1.18{+0.10\atop -0.23}$, all at the 95% confidence level., Comment: 10 pages, 9 Postscript figures, changes made to reflect published version

Published
2001
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6. The COBE Normalization for Standard CDM

Author

Bunn, E. F., Scott, D., and White, M.

Subjects
Astrophysics
Abstract

The COBE detection of CMB anisotropies provides the best way of fixing the amplitude of fluctuations on the largest scales. This normalization is usually given for an n=1 spectrum, including only the anisotropy caused by the Sachs- Wolfe effect. This is certainly not a good approximation for a model containing any reasonable amount of baryonic matter. In fact, even tilted S-W spectra are not a good fit to models like CDM. Here we normalize standard CDM (sCDM) to the 2-year COBE data, and quote the best amplitude in terms of the conventionally used measures of power. We also give normalizations for some specific variants of this standard model, and we indicate how the normalization depends on the assumed values of n, Omega_B and H_0. For sCDM we find =19.9\pm1.5uK, corresponding to sigma_8=1.34\pm0.10, with the normalization at large scales being B=(8.16\pm1.04)\times10^5 (Mpc/h)^4, and other numbers given in the Table. The measured rms temperature fluctuation smoothed on 10deg is a little low relative to this normalization. This is mainly due to the low quadrupole in the data: when the quadrupole is removed, the measured value of sigma(10) is quite consistent with the best-fitting . The use of should be preferred over sigma(10), when its value can be determined for a particular theory, since it makes full use of the data., Comment: 4 pages compressed uuencoded postscript. We have corrected an error in our analysis

Published
1994
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7. QUBIC: A Fizeau Interferometer Targeting Primordial B-Modes

Author

Tartari, A., Aumont, J., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bélier, B., Bennett, D., Bergé, L., Bernard, J. Ph., Bersanelli, M., Bigot-Sazy, M. A., Bleurvacq, N., Bordier, G., Brossard, J., Bunn, E. F., Buzi, D., Cammilleri, D., Cavaliere, F., Chanial, P., Chapron, C., Coppolecchia, A., D’Alessandro, G., De Bernardis, P., Decourcelle, T., Del Torto, F., De Petris, M., Dumoulin, L., Franceschet, C., Gault, A., Gayer, D., Gervasi, M., Ghribi, A., Giard, M., Giraud-Héraud, Y., Gradziel, M., Grandsire, L., Hamilton, J. Ch., Haynes, V., Holtzer, N., Kaplan, J., Korotkov, A., Lande, J., Lowitz, A., Maffei, B., Marnieros, S., Martino, J., Masi, S., McCulloch, M., Melhuish, S., Mennella, A., Montier, L., Murphy, A., Néel, D., Ng, M. W., O’Sullivan, C., Pajot, F., Passerini, A., Perbost, C., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Prêle, D., Rambaud, D., Rigaut, O., Salatino, M., Schillaci, A., Scully, S., Stolpovskiy, M. M., Timbie, P., Tucker, G., Viganò, D., Voisin, F., Watson, B., and Zannoni, M.

Published
2016
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8. QUBIC: the Q&U Bolometric Interferometer for Cosmology

Author

Piat, M., Battistelli, E., Baù, A., Bennett, D., Bergé, L., Bernard, J.-P., de Bernardis, P., Bigot-Sazy, M.-A., Bordier, G., Bounab, A., Bréelle, E., Bunn, E. F., Calvo, M., Charlassier, R., Collin, S., Cruciani, A., Curran, G., Dumoulin, L., Gault, A., Gervasi, M., Ghribi, A., Giard, M., Giordano, C., Giraud-Héraud, Y., Gradziel, M., Guglielmi, L., Hamilton, J.-C., Haynes, V., Kaplan, J., Korotkov, A., Landé, J., Maffei, B., Maiello, M., Malu, S., Marnieros, S., Martino, J., Masi, S., Montier, L., Murphy, A., Nati, F., O’Sullivan, C., Pajot, F., Parisel, C., Passerini, A., Peterzen, S., Piacentini, F., Piccirillo, L., Pisano, G., Polenta, G., Prêle, D., Romano, D., Rosset, C., Salatino, M., Schillaci, A., Sironi, G., Sordini, R., Spinelli, S., Tartari, A., Timbie, P., Tucker, G., Vibert, L., Voisin, F., Watson, R. A., and Zannoni, M.

Published
2012
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9. Optical modelling and analysis of the Q and U bolometric interferometer for cosmology

Author

Sadwick L.P.,Yang T., Burke, D, Gayer, D, Kalinauskaite, E, O'Sullivan, C, Murphy, J, Scully, S, De Petris, M, De Leo, M, Mennella, A, Torchinsky, S, Zannoni, M, Amico, G, Auguste, D, Aumont, J, Banfi, S, Barbaran, G, Battaglia, P, Battistelli, E, Bau, A, Belier, B, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bleurvac, N, Bonaparte, J, Bonis, J, Bordier, G, Breelle, E, Bunn, E, Buzi, D, Buzzelli, A, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Columbro, F, Coppi, G, Coppolecchia, A, Couchot, F, D'Alessandro, G, D'Agostino, R, De Bernardis, P, De Gasperis, G, Di Donato, A, Drilien, A, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Franceschet, C, Gamboa-Lerena, M, Garcia, B, Garrido, X, Gaspard, M, Gault, A, Gervasi, M, Giard, M, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Grandsire, L, Guerrard, E, Hamilton, J, Harari, D, Haynes, V, Henrot-Versille, S, Hoang, D, Holtzer, N, Incardona, F, Jules, E, Kaplan, J, Korotkov, A, Kristukat, C, Lamagna, L, Lande, J, Loucatos, S, Louis, T, Lowitz, A, Lukovic, V, Luterstein, R, Maffei, B, Marnieros, S, Masi, S, Mattei, A, May, A, Mcculloch, M, Medina, M, Mele, L, Melhuish, S, Mundo, L, Montier, L, Neel, D, Olivieri, E, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perdereau, O, Pezzotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Polenta, G, Prele, D, Puddu, R, Rambaud, D, Rigaut, O, Ringegni, P, Romero, G, Salatino, M, Schillaci, A, Scoccola, C, Spinelli, S, Stolpovskiy, M, Suarez, F, Tartari, A, Thermeau, J, Timbie, P, Tristram, M, Truongcanh, V, Tucker, G, Tucker, C, Vigano, D, Vittorio, N, Voisin, F, Watson, B, Wicek, F, Zullo, A, Burke D., Gayer D., Kalinauskaite E., O'Sullivan C., Murphy J. D., Scully S. P., De Petris M., De Leo M., Mennella A., Torchinsky S. A., Zannoni M., Amico G., Auguste D., Aumont J., Banfi S., Barbaran G., Battaglia P., Battistelli E., Bau A., Belier B., Bennett D. G., Berge L., Bernard J. -P., Bersanelli M., Bigot-Sazy M. -A., Bleurvac N., Bonaparte J., Bonis J., Bordier G., Breelle E., Bunn E. F., Buzi D., Buzzelli A., Cavaliere F., Chanial P., Chapron C., Charlassier R., Columbro F., Coppi G., Coppolecchia A., Couchot F., D'Alessandro G., D'Agostino R., De Bernardis P., De Gasperis G., Di Donato A., Drilien A. -A., Dumoulin L., Etchegoyen A., Fasciszewski A., Franceschet C., Gamboa-Lerena M., Garcia B., Garrido X., Gaspard M., Gault A., Gervasi M., Giard M., Giraud-Heraud Y., Gomez Berisso M., Gonzalez M., Gradziel M. L., Grandsire L., Guerrard E., Hamilton J. -C., Harari D., Haynes V., Henrot-Versille S., Hoang D. T., Holtzer N., Incardona F., Jules E., Kaplan J., Korotkov A. L., Kristukat C., Lamagna L., Lande J., Loucatos S., Louis T., Lowitz A., Lukovic V., Luterstein R., Maffei B., Marnieros S., Masi S., Mattei A., May A. J., McCulloch M. A., Medina M. C., Mele L., Melhuish S. J., Mundo L., Montier L., Murphy J. A., Neel D., Olivieri E., Paiella A., Pajot F., Passerini A., Pastoriza H., Pelosi A., Perbost C., Perdereau O., Pezzotta F., Piacentini F., Piat M. R., Piccirillo L., Pisano G., Polenta G., Prele D., Puddu R., Rambaud D., Rigaut O., Ringegni P., Romero G. E., Salatino M., Schillaci A., Scoccola C. G., Spinelli S. M., Stolpovskiy M., Suarez F., Tartari A., Thermeau J. -P., Timbie P. T., Tristram M., Truongcanh V., Tucker G. S., Tucker C. E., Vigano D., Vittorio N., Voisin F., Watson B., Wicek F., Zullo A., Sadwick L.P.,Yang T., Burke, D, Gayer, D, Kalinauskaite, E, O'Sullivan, C, Murphy, J, Scully, S, De Petris, M, De Leo, M, Mennella, A, Torchinsky, S, Zannoni, M, Amico, G, Auguste, D, Aumont, J, Banfi, S, Barbaran, G, Battaglia, P, Battistelli, E, Bau, A, Belier, B, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bleurvac, N, Bonaparte, J, Bonis, J, Bordier, G, Breelle, E, Bunn, E, Buzi, D, Buzzelli, A, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Columbro, F, Coppi, G, Coppolecchia, A, Couchot, F, D'Alessandro, G, D'Agostino, R, De Bernardis, P, De Gasperis, G, Di Donato, A, Drilien, A, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Franceschet, C, Gamboa-Lerena, M, Garcia, B, Garrido, X, Gaspard, M, Gault, A, Gervasi, M, Giard, M, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Grandsire, L, Guerrard, E, Hamilton, J, Harari, D, Haynes, V, Henrot-Versille, S, Hoang, D, Holtzer, N, Incardona, F, Jules, E, Kaplan, J, Korotkov, A, Kristukat, C, Lamagna, L, Lande, J, Loucatos, S, Louis, T, Lowitz, A, Lukovic, V, Luterstein, R, Maffei, B, Marnieros, S, Masi, S, Mattei, A, May, A, Mcculloch, M, Medina, M, Mele, L, Melhuish, S, Mundo, L, Montier, L, Neel, D, Olivieri, E, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perdereau, O, Pezzotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Polenta, G, Prele, D, Puddu, R, Rambaud, D, Rigaut, O, Ringegni, P, Romero, G, Salatino, M, Schillaci, A, Scoccola, C, Spinelli, S, Stolpovskiy, M, Suarez, F, Tartari, A, Thermeau, J, Timbie, P, Tristram, M, Truongcanh, V, Tucker, G, Tucker, C, Vigano, D, Vittorio, N, Voisin, F, Watson, B, Wicek, F, Zullo, A, Burke D., Gayer D., Kalinauskaite E., O'Sullivan C., Murphy J. D., Scully S. P., De Petris M., De Leo M., Mennella A., Torchinsky S. A., Zannoni M., Amico G., Auguste D., Aumont J., Banfi S., Barbaran G., Battaglia P., Battistelli E., Bau A., Belier B., Bennett D. G., Berge L., Bernard J. -P., Bersanelli M., Bigot-Sazy M. -A., Bleurvac N., Bonaparte J., Bonis J., Bordier G., Breelle E., Bunn E. F., Buzi D., Buzzelli A., Cavaliere F., Chanial P., Chapron C., Charlassier R., Columbro F., Coppi G., Coppolecchia A., Couchot F., D'Alessandro G., D'Agostino R., De Bernardis P., De Gasperis G., Di Donato A., Drilien A. -A., Dumoulin L., Etchegoyen A., Fasciszewski A., Franceschet C., Gamboa-Lerena M., Garcia B., Garrido X., Gaspard M., Gault A., Gervasi M., Giard M., Giraud-Heraud Y., Gomez Berisso M., Gonzalez M., Gradziel M. L., Grandsire L., Guerrard E., Hamilton J. -C., Harari D., Haynes V., Henrot-Versille S., Hoang D. T., Holtzer N., Incardona F., Jules E., Kaplan J., Korotkov A. L., Kristukat C., Lamagna L., Lande J., Loucatos S., Louis T., Lowitz A., Lukovic V., Luterstein R., Maffei B., Marnieros S., Masi S., Mattei A., May A. J., McCulloch M. A., Medina M. C., Mele L., Melhuish S. J., Mundo L., Montier L., Murphy J. A., Neel D., Olivieri E., Paiella A., Pajot F., Passerini A., Pastoriza H., Pelosi A., Perbost C., Perdereau O., Pezzotta F., Piacentini F., Piat M. R., Piccirillo L., Pisano G., Polenta G., Prele D., Puddu R., Rambaud D., Rigaut O., Ringegni P., Romero G. E., Salatino M., Schillaci A., Scoccola C. G., Spinelli S. M., Stolpovskiy M., Suarez F., Tartari A., Thermeau J. -P., Timbie P. T., Tristram M., Truongcanh V., Tucker G. S., Tucker C. E., Vigano D., Vittorio N., Voisin F., Watson B., Wicek F., and Zullo A.

Abstract

Remnant radiation from the early universe, known as the Cosmic Microwave Background (CMB), has been redshifted and cooled, and today has a blackbody spectrum peaking at millimetre wavelengths. The QUBIC (Q&U Bolometric Interferometer for Cosmology) instrument is designed to map the very faint polaristion structure in the CMB. QUBIC is based on the novel concept of bolometric interferometry in conjunction with synthetic imaging. It will have a large array of input feedhorns, which creates a large number of interferometric baselines. The beam from each feedhorn is passed through an optical combiner, with an off-axis compensated Gregorian design, to allow the generation of the synthetic image. The optical-combiner will operate in two frequency bands (150 and 220 GHz with 25% and 18.2 % bandwidth respectively) while cryogenically cooled TES bolometers provide the sensitivity required at the image plane. The QUBIC Technical Demonstrator (TD), a proof of technology instrument that contains 64 input feed-horns, is currently being built and will be installed in the Alto Chorrillos region of Argentina. The plan is then for the full QUBIC instrument (400 feed-horns) to be deployed in Argentina and obtain cosmologically significant results. In this paper we will examine the output of the manufactered feed-horns in comparison to the nominal design. We will show the results of optical modelling that has been performed in anticipation of alignment and calibration of the TD in Paris, in particular testing the validity of real laboratory environments. We show the output of large calibrator sources (50 ° full width haf max Gaussian beams) and the importance of accurate mirror definitions when modelling large beams. Finally we describe the tolerance on errors of the position and orientation of mirrors in the optical combiner.

Published
2018

10. Optical design and modelling of the QUBIC instrument, a next-generation quasi-optical bolometric interferometer for cosmology

Author

Scully, S., additional, Burke, D., additional, O'Sullivan, C., additional, Gayer, D., additional, Gradziel, M., additional, Murphy, J. A., additional, De Petris, M., additional, Buzi, D., additional, Zannoni, M., additional, Mennella, A, additional, Gervasi, M., additional, Tartari, A., additional, Maffei, B., additional, Aumont, J., additional, Banfi, S., additional, Battaglia, P., additional, Battistelli, E. S., additional, Baù, A., additional, Bélier, B., additional, Bennet, D., additional, Bergé, L., additional, Bernard, J.-Ph., additional, Bersanelli, M., additional, Bigot-Sazy, M.-A., additional, Bleurvacq, N., additional, Bordier, G., additional, Brossard, J., additional, Bunn, E. F., additional, Cammileri, D., additional, Cavaliere, F., additional, Chanial, P., additional, Chapron, C., additional, Coppolecchia, A., additional, Couchot, F., additional, D'Alessandro, G., additional, De Bernardis, P., additional, Decourcelle, T., additional, Del Torto, F., additional, Dumoulin, L., additional, Franceschet, C., additional, Gault, A., additional, Ghribi, A., additional, Giard, M., additional, Giraud-Héraud, Y., additional, Grandsire, L., additional, Hamilton, J. C., additional, Haynes, V., additional, Henrot-Versillé, S., additional, Holtzer, N., additional, Kaplan, J., additional, Korotkov, A., additional, Lande, J., additional, Lowitz, A., additional, Marnieros, S., additional, Martino, J., additional, Masi, S., additional, McCulloch, Mark, additional, Melhuish, Simon, additional, Montier, L., additional, Néel, D., additional, Ng, M. W., additional, Pajot, F., additional, Passerini, A., additional, Perbost, C., additional, Perdereau, O., additional, Piacentini, F., additional, Piat, M., additional, Piccirillo, L., additional, Pisano, G., additional, Prêle, D., additional, Puddu, R., additional, Rambaud, D., additional, Rigaut, O., additional, Salatino, M., additional, Schillaci, A., additional, Stolpovskiy, M., additional, Timbie, P., additional, Tristram, M., additional, Tucker, G., additional, Viganò, D., additional, Voisin, F., additional, and Watson, B., additional

Published
2016
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11. QUBIC: A Fizeau Interferometer Targeting Primordial B-Modes

Author

Tartari, A., primary, Aumont, J., additional, Banfi, S., additional, Battaglia, P., additional, Battistelli, E. S., additional, Baù, A., additional, Bélier, B., additional, Bennett, D., additional, Bergé, L., additional, Bernard, J. Ph., additional, Bersanelli, M., additional, Bigot-Sazy, M. A., additional, Bleurvacq, N., additional, Bordier, G., additional, Brossard, J., additional, Bunn, E. F., additional, Buzi, D., additional, Cammilleri, D., additional, Cavaliere, F., additional, Chanial, P., additional, Chapron, C., additional, Coppolecchia, A., additional, D’Alessandro, G., additional, De Bernardis, P., additional, Decourcelle, T., additional, Del Torto, F., additional, De Petris, M., additional, Dumoulin, L., additional, Franceschet, C., additional, Gault, A., additional, Gayer, D., additional, Gervasi, M., additional, Ghribi, A., additional, Giard, M., additional, Giraud-Héraud, Y., additional, Gradziel, M., additional, Grandsire, L., additional, Hamilton, J. Ch., additional, Haynes, V., additional, Holtzer, N., additional, Kaplan, J., additional, Korotkov, A., additional, Lande, J., additional, Lowitz, A., additional, Maffei, B., additional, Marnieros, S., additional, Martino, J., additional, Masi, S., additional, McCulloch, M., additional, Melhuish, S., additional, Mennella, A., additional, Montier, L., additional, Murphy, A., additional, Néel, D., additional, Ng, M. W., additional, O’Sullivan, C., additional, Pajot, F., additional, Passerini, A., additional, Perbost, C., additional, Piacentini, F., additional, Piat, M., additional, Piccirillo, L., additional, Pisano, G., additional, Prêle, D., additional, Rambaud, D., additional, Rigaut, O., additional, Salatino, M., additional, Schillaci, A., additional, Scully, S., additional, Stolpovskiy, M. M., additional, Timbie, P., additional, Tucker, G., additional, Viganò, D., additional, Voisin, F., additional, Watson, B., additional, and Zannoni, M., additional

Published
2015
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12. Optical modelling and analysis of the Q and U bolometric interferometer for cosmology

Author

Sadwick, Laurence P., Yang, Tianxin, Burke, D., Gayer, D., Kalinauskaite, E., O'Sullivan, C., Murphy, J. D., Scully, S. P., De Petris, M., De Leo, M., Mennella, A., Torchinsky, S. A., Zannoni, M., Amico, G., Auguste, D., Aumont, J., Banfi, S., Barbarán, G., Battaglia, P., Battistelli, E., Baù, A., Bélier, B., Bennett, D. G., Bergé, L., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bleurvac, N., Bonaparte, J., Bonis, J., Bordier, G., Bréelle, E., Bunn, E. F., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Chapron, C., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., Couchot, F., D’Alessandro, G., D'Agostino, R., de Bernardis, P., De Gasperis, G., Di Donato, A., Drilien, A.-A., Dumoulin, Louis, Etchegoyen, A., Fasciszewski, A., Franceschet, C., Gamboa-Lerena, M., García, B., Garrido, X., Gaspard, M., Gault, A., Gervasi, M., Giard, M., Giraud-Héraud, Y., Gómez Berisso, M., González, M., Gradziel, M. L., Grandsire, L., Guerrard, E., Hamilton, J.-Ch., Harari, D., Haynes, V., Henrot-Versillé, S., Hoang, D. T., Holtzer, N., Incardona, F., Jules, E., Kaplan, J., Korotkov, A. L., Kristukat, C., Lamagna, L., Lande, J., Loucatos, S., Louis, T., Lowitz, A., Lukovic, V., Luterstein, R., Maffei, Bruno, Marnieros, S., Masi, S., Mattei, A., May, A. J., McCulloch, M. A., Medina, M. C., Mele, L., Melhuish, S. J., Mundo, L., Montier, L., Murphy, J. A., Néel, D., Olivieri, E., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perbost, C., Perdereau, O., Pezzotta, F., Piacentini, F., Piat, M. R., Piccirillo, L., Pisano, G., Polenta, G., Prêle, D., Puddu, R., Rambaud, D., Rigaut, O., Ringegni, P., Romero, G. E., Salatino, M., Schillaci, A., Scóccola, C. G., Spinelli, S. M., Stolpovskiy, M., Suarez, F., Tartari, A., Thermeau, J.-P., Timbie, P. T., Tristram, M., Truongcanh, V., Tucker, G. S., Tucker, C. E., Viganò, D., Vittorio, N., Voisin, F., Watson, B., Wicek, F., and Zullo, A.

Published
2018
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14. Frequentist estimation of cosmological parameters from the MAXIMA-1 cosmic microwave background anisotropy data

Author

Abroe, M. E., primary, Balbi, A., additional, Borrill, J., additional, Bunn, E. F., additional, Hanany, S., additional, Ferreira, P. G., additional, Jaffe, A. H., additional, Lee, A. T., additional, Olive, K. A., additional, Rabii, B., additional, Richards, P. L., additional, Smoot, G. F., additional, Stompor, R., additional, Winant, C. D., additional, and Wu, J. H. P., additional

Published
2002
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15. Optical design and modelling of the QUBIC instrument, a next-generation quasi-optical bolometric interferometer for cosmology

Author

Holland, Wayne S., Zmuidzinas, Jonas, Scully, S., Burke, D., O'Sullivan, C., Gayer, D., Gradziel, M., Murphy, J. A., De Petris, M., Buzi, D., Zannoni, M., Mennella, A, Gervasi, M., Tartari, A., Maffei, B., Aumont, J., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bélier, B., Bennet, D., Bergé, L., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bleurvacq, N., Bordier, G., Brossard, J., Bunn, E. F., Cammileri, D., Cavaliere, F., Chanial, P., Chapron, C., Coppolecchia, A., Couchot, F., D'Alessandro, G., De Bernardis, P., Decourcelle, T., Del Torto, F., Dumoulin, L., Franceschet, C., Gault, A., Ghribi, A., Giard, M., Giraud-Héraud, Y., Grandsire, L., Hamilton, J. C., Haynes, V., Henrot-Versillé, S., Holtzer, N., Kaplan, J., Korotkov, A., Lande, J., Lowitz, A., Marnieros, S., Martino, J., Masi, S., McCulloch, Mark, Melhuish, Simon, Montier, L., Néel, D., Ng, M. W., Pajot, F., Passerini, A., Perbost, C., Perdereau, O., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Prêle, D., Puddu, R., Rambaud, D., Rigaut, O., Salatino, M., Schillaci, A., Stolpovskiy, M., Timbie, P., Tristram, M., Tucker, G., Viganò, D., Voisin, F., and Watson, B.

Published
2016
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17. Frequentist estimation of cosmological parameters from theMAXIMA-1 cosmic microwave background anisotropy data.

Author

Abroe, M. E., Balbi, A., Borrill, J., Bunn, E. F., Hanany, S., Ferreira, P. G., Jaffe, A. H., Lee, A. T., Olive, K. A., Rabii, B., Richards, P. L., Smoot, G. F., Stompor, R., Winant, C. D., and Wu, J. H. P.

Subjects
COSMIC background radiation, ASTROPHYSICAL radiation
Abstract

We use a frequentist statistical approach to set confidence intervals on the values of cosmological parameters using the MAXIMA-1 and COBE measurements of the angular power spectrum of the cosmic microwave background. We define a Δχ² statistic, simulate the measurements of MAXIMA-1 and COBE, determine the probability distribution of the statistic, and use it and the data to set confidence intervals on several cosmological parameters. We compare the frequentist confidence intervals with Bayesian credible regions. The frequentist and Bayesian approaches give best estimates for the parameters that agree within 15 per cent, and confidence interval widths that agree to within 30 per cent. The results also suggest that a frequentist analysis gives slightly broader confidence intervals than a Bayesian analysis. The frequentist analysis gives values of Ω = 089[sup +0.26, sub -0.19], Ω[sub B]h² = 0.026[sup + 0.020,sub 0.011] and n = 1.02[sup +0.31, sub -0.10], and the Bayesian analysis gives values of Ω = 0.98[sup +0.14, sub -0.19], Ω[sub B]h² = 0.029[sup +0.015, sub -0.010] and n = 1.18[sup +0.10, sub -0.23], all at the 95 per cent confidence level. [ABSTRACT FROM AUTHOR]

Published
2002
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18. Optical design and modelling of the QUBIC instrument, a next-generation quasi-optical bolometric interferometer for cosmology

Author

Holland, Wayne S., Zmuidzinas, Jonas, Burke, D., Scully, S., O'Sullivan, C., Gayer, D., Gradziel, M., Murphy, J. A., De Petris, M., Buzi, D., Zannoni, M., Mennella, A, Gervasi, M., Tartari, A., Maffei, B., Aumont, J., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bélier, B., Bennet, D., Bergé, L., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bleurvacq, N., Bordier, G., Brossard, J., Bunn, E. F., Cammileri, D., Cavaliere, F., Chanial, P., Chapron, C., Coppolecchia, A., Couchot, F., D'Alessandro, G., De Bernardis, P., Decourcelle, T., Del Torto, F., Dumoulin, L., Franceschet, C., Gault, A., Ghribi, A., Giard, M., Giraud-Héraud, Y., Grandsire, L., Hamilton, J. C., Haynes, V., Henrot-Versillé, S., Holtzer, N., Kaplan, J., Korotkov, A., Lande, J., Lowitz, A., Marnieros, S., Martino, J., Masi, S., McCulloch, Mark, Melhuish, Simon, Montier, L., Néel, D., Ng, M. W., Pajot, F., Passerini, A., Perbost, C., Perdereau, O., Piacentini, F., Piat, M., Piccirillo, L., Pisano, Giampaolo, Prêle, D., Puddu, R., Rambaud, D., Rigaut, O., Salatino, M., Schillaci, A., Stolpovskiy, M., Timbie, P., Tristram, M., Tucker, G., Viganò, D., Voisin, F., Watson, B., Holland, Wayne S., Zmuidzinas, Jonas, Burke, D., Scully, S., O'Sullivan, C., Gayer, D., Gradziel, M., Murphy, J. A., De Petris, M., Buzi, D., Zannoni, M., Mennella, A, Gervasi, M., Tartari, A., Maffei, B., Aumont, J., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bélier, B., Bennet, D., Bergé, L., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bleurvacq, N., Bordier, G., Brossard, J., Bunn, E. F., Cammileri, D., Cavaliere, F., Chanial, P., Chapron, C., Coppolecchia, A., Couchot, F., D'Alessandro, G., De Bernardis, P., Decourcelle, T., Del Torto, F., Dumoulin, L., Franceschet, C., Gault, A., Ghribi, A., Giard, M., Giraud-Héraud, Y., Grandsire, L., Hamilton, J. C., Haynes, V., Henrot-Versillé, S., Holtzer, N., Kaplan, J., Korotkov, A., Lande, J., Lowitz, A., Marnieros, S., Martino, J., Masi, S., McCulloch, Mark, Melhuish, Simon, Montier, L., Néel, D., Ng, M. W., Pajot, F., Passerini, A., Perbost, C., Perdereau, O., Piacentini, F., Piat, M., Piccirillo, L., Pisano, Giampaolo, Prêle, D., Puddu, R., Rambaud, D., Rigaut, O., Salatino, M., Schillaci, A., Stolpovskiy, M., Timbie, P., Tristram, M., Tucker, G., Viganò, D., Voisin, F., and Watson, B.

Abstract

Big Bang cosmologies predict that the cosmic microwave background (CMB) contains faint temperature and polarisation anisotropies imprinted in the early universe. ESA's PLANCK satellite has already measured the temperature anisotropies1 in exquisite detail; the next ambitious step is to map the primordial polarisation signatures which are several orders of magnitude lower. Polarisation E-modes have been measured2 but the even-fainter primordial B-modes have so far eluded detection. Their magnitude is unknown but it is clear that a sensitive telescope with exceptional control over systematic errors will be required. QUBIC3 is a ground-based European experiment that aims to exploit the novel concept of bolometric interferometry in order to measure B-mode polarisation anisotropies in the CMB. Beams from an aperture array of corrugated horns will be combined to form a synthesised image of the sky Stokes parameters on two focal planes: one at 150 GHz the other at 220 GHz. In this paper we describe recent optical modelling of the QUBIC beam combiner, concentrating on modelling the instrument point-spread-function and its operation in the 220-GHz band. We show the effects of optical aberrations and truncation as successive components are added to the beam path. In the case of QUBIC, the aberrations introduced by off-axis mirrors are the dominant contributor. As the frequency of operation is increased, the aperture horns allow up to five hybrid modes to propagate and we illustrate how the beam pattern changes across the 25% bandwidth. Finally we describe modifications to the QUBIC optical design to be used in a technical demonstrator, currently being manufactured for testing in 2016.

19. The Millimeter-wave Bolometric Interferometer (MBI)

Author

Gault, Amanda C., Ade, Peter A. R., Bierman, E., Bunn, E. F., Hyland, P. O., Keating, B. G., Korotkov, A. L., Malu, S. S., O'Sullivan, C., Piccirillo, L., Timbie, P. T., Tucker, G. S., Gault, Amanda C., Ade, Peter A. R., Bierman, E., Bunn, E. F., Hyland, P. O., Keating, B. G., Korotkov, A. L., Malu, S. S., O'Sullivan, C., Piccirillo, L., Timbie, P. T., and Tucker, G. S.

Abstract

We report on the design and tests of a prototype of the Millimeter-wave Bolometric Interferometer (MBI). MBI is designed to make sensitive measurements of the polarization of the cosmic microwave background (CMB). It combines the differencing capabilities of an interferometer with the high sensitivity of bolometers at millimeter wavelengths. The prototype, which we call MBI-4, views the sky directly through four corrugated horn antennas. MBI ultimately will have 1000 antennas. These antennas have low sidelobes and nearly symmetric beam patterns, so spurious instrumental polarization from reflective optics is avoided. The MBI-4 optical band is defined by filters with a central frequency of 90 GHz. The set of baselines, determined by placement of the four antennas, results in sensitivity to CMB polarization fluctuations over the multipole range l = 150 - 270. The signals are combined with a Fizeau beam combiner and interference fringes are detected by an array of spiderweb bolometers. In order to separate the visibility signals from the total power detected by each bolometer, the phase of the signal from each antenna is modulated by a ferrite-based waveguide phase shifter. Initial tests and observations have been made at Pine Bluff Observatory (PBO) outside Madison, WI.

20. The Millimeter-wave Bolometric Interferometer (MBI)

Author

Gault, Amanda C., Ade, Peter A. R., Bierman, E., Bunn, E. F., Hyland, P. O., Keating, B. G., Korotkov, A. L., Malu, S. S., O'Sullivan, C., Piccirillo, L., Timbie, P. T., Tucker, G. S., Gault, Amanda C., Ade, Peter A. R., Bierman, E., Bunn, E. F., Hyland, P. O., Keating, B. G., Korotkov, A. L., Malu, S. S., O'Sullivan, C., Piccirillo, L., Timbie, P. T., and Tucker, G. S.

Abstract

We report on the design and tests of a prototype of the Millimeter-wave Bolometric Interferometer (MBI). MBI is designed to make sensitive measurements of the polarization of the cosmic microwave background (CMB). It combines the differencing capabilities of an interferometer with the high sensitivity of bolometers at millimeter wavelengths. The prototype, which we call MBI-4, views the sky directly through four corrugated horn antennas. MBI ultimately will have 1000 antennas. These antennas have low sidelobes and nearly symmetric beam patterns, so spurious instrumental polarization from reflective optics is avoided. The MBI-4 optical band is defined by filters with a central frequency of 90 GHz. The set of baselines, determined by placement of the four antennas, results in sensitivity to CMB polarization fluctuations over the multipole range l = 150 - 270. The signals are combined with a Fizeau beam combiner and interference fringes are detected by an array of spiderweb bolometers. In order to separate the visibility signals from the total power detected by each bolometer, the phase of the signal from each antenna is modulated by a ferrite-based waveguide phase shifter. Initial tests and observations have been made at Pine Bluff Observatory (PBO) outside Madison, WI.

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