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1. 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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2. QUBIC: The QU bolometric interferometer for cosmology

Author

Battistelli, E., Baú, A., Bennett, D., Bergé, L., Bernard, J.-Ph., de Bernardis, P., Bordier, G., Bounab, A., Bréelle, É., Bunn, E.F., Calvo, M., Charlassier, R., Collin, S., Coppolecchia, A., Cruciani, A., Curran, G., de Petris, M., 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., Martino, J., 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., 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
2011
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3. 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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5. The BRAIN CMB polarization experiment

Author

Polenta, G., Ade, P.A.R., Bartlett, J., Bréelle, E., Conversi, L., de Bernardis, P., Dufour, C., Gervasi, M., Giard, M., Giordano, C., Giraud-Heraud, Y., Maffei, B., Masi, S., Nati, F., Orlando, A., Peterzen, S., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Pons, R., Rosset, C., Savini, G., Sironi, G., Tartari, A., Veneziani, M., and Zannoni, M.

Published
2007
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6. BRAIN/MBI: a bolometric interferometer dedicated to the CMB polarization

Author

Tartari, A., Bartlett, J. G., Elia Stefano Battistelli, Baù, A., Bennett, D., Bergé, L., Bernard, J. P., Bounab, A., Bréelle, E., Bunn, E., Charlassier, R., Cruciani, A., Collin, S., Curran, G., Paolo de Bernardis, Dumoulin, L., Gault, A., Gervasi, M., Ghribi, A., Giard, M., Giordano, C., Giraud Héraud, Y., Gradziel, M., Guglielmi, L., Hamilton, J. C., Haynes, V., Iacoangeli, A., Kaplan, J., Korotkov, A., Lande, J., Maffei, B., Maiello, M., Malu, S. S., Marnieros, S., Silvia Masi, Murphy, A., Sullivan, C. O., Pajot, F., Passerini, A., Peterzen, S. S., Francesco Piacentini, Piccirillo, L., Piat, M., Giampaolo Pisano, Polenta, G., Prêle, D., Rosset, C., Schillaci, Alessandro, Sironi, G., Spinelli, S., Tucker, G., Timbie, P., Voisin, F., Watson, B., Zannoni, M., Tartari, A, Bartlett, J, Battistelli, E, Bau', A, Bennett, D, Bergè, L, Bernard, J, Bounab, A, Brèelle, E, Bunn, E, Charlassier, R, Cruciani, A, Collin, S, Curran, G, De Bernardis, P, Dumoulin, L, Gault, A, Gervasi, M, Ghribi, A, Giard, M, Giordano, C, Giraud Hèraud, J, Gradziel, M, Guglielmi, L, Hamilton, J, Haynes, V, Iacoangeli, A, Kaplan, J, Korotkov, A, Lande, J, Maffei, B, Maiello, M, Malu, S, Marnieros, S, Masi, S, Murphy, A, O'Sullivan, C, Pajot, F, Passerini, A, Peterzen, S, Piacentini, F, Piccirillo, L, Piat, M, Pisano, G, Polenta, G, Prêle, D, Rosset, C, Schillaci, A, Sironi, G, Spinelli, S, Tucker, G, Timbie, P, Voisin, F, Watson, B, and Zannoni, M

Subjects
QUBIC, CMB, Polarization, CMB, polarimetry, QUBIC, CMB, polarimetry
Abstract

BRAIN/MBI is a mm-wave ground-based experiment dedicated to the study of the B-modes of CMB polarization. It is based on the bolometric interferometry (BI) technique, and it is the result of the merging of two different projects proposed in the last years: BRAIN (France, Italy, UK) and MBI 4 (US, UK). BI is a technique already validated in a laboratory environment using small scale demonstrators employing as detectors standard 4 K bolometers. In fact, both the MBI and BRAIN teams demonstrated that interference fringes are observed once the signals coming from the two antennas of a single baseline are phase-shifted, combined and then detected. Both optical and wave-guided combination schemes have been tested within the collaboration. From the hardware point of view, the simplest unity of BRAIN/MBI is constituted by a feed horn, an OMT, and two independent phase shifters for each polarization. After phase shifting, the two beams coming out from each unity, feed a beam combiner redirecting the signals towards the detectors. Some of the most critical components, that are OMTs, phase-shifters and possibly detectors, will be made using superconducting technologies and are now under development. Moreover, detailed calculations showed that the sensitivity of a bolometric interferometer, if operated with a proper phase modulation-demodulation scheme, can approach that one of an imager with a comparable number of detectors, while exploiting the systematics cleaness of compact interferometers. On one side, BRAIN/MBI will be an instrument with a sensitivity and a polarization purity suitable for the detection of B-modes. On the other side, it will be a benchmark for new and promisings technologies that may be qualified for the CMB science in perspective of a post-Planck space mission. Since BI is prone to different contaminations from systematics with respect to imagers, a cross-check of the results and a comparison of two conceptually orthogonal strategies will finally be possible

Published
2009

8. OLIMPO

Author

Masi, Silvia, Battistelli, Elia Stefano, Brienza, D., Conversi, L., Cruciani, A., DE BERNARDIS, Paolo, DE PETRIS, Marco, Fiadino, P., Iacoangeli, A., Lamagna, Luca, Nati, L., Nati, Federico, Piacentini, Francesco, Polenta, G., Ade, P. A. R., Hargrave, P., Mauskopf, P., Morozov, D., Savini, G., Tucker, C., Boscaleri, A., Peterzen, S., DI STEFANO, G., Romeo, G., Delbart, A., Magneville, C., Pansart, J. P., Yvon, D., Doumoulin, L., Camus, P., Gromov, V., and Maslov, I.

Subjects
Cosmology: Cosmic Microwave Background – Cosmology: Clusters of Galaxies – Stratospheric Balloons
Published
2008

11. First circumpolar trajectory ultralight to heavy long duration balloon development from svalbard, Norway

Author

Peterzen, S. E., Ibba, R., Olsen, G. J., Dragoy, P., Masi, S., Giovanni ROMEO, Distefano, G., Cardillo, A., and Musso, I.

Subjects
Long duration balloon, Stratospheric balloon, Circumpolar flight
Abstract

During the 2006 Ultra Light LDB campaign in Svalbard, the Italian Space Agency (Agenzia Spaziale Italiana, (ASI)) in a joint effort with Andoya Rocket Range (ARR) launched what became the first complete circumpolar trajectory around the northern polar region by a stratospheric balloon launched from Svalbard. The historic balloon experiment was launched from the Nobile / Amundsen Stratospheric Balloon Center Svalbard (N/A SBC). The flight trajectory starting from Longyearbyen, Svalbard, took the stratospheric balloon on a 17 day excursion in a near perfect circle back over Svalbard and on to Greenland where the flight was successfully terminated for recovery. Not only did this historic flight prove concept of successful LDB programs above 79 degrees N, but also proved the viability of using Ultralite LDB platform to achieve exciting science. These small balloons (9,300 m(3)) Carry Iridium based TM systems, redundant terminate systems, solar charging system and a parachute making die entire system recoverable. The N/A SBC-Svalbard effort offers an excellent opportunity as a student launch program due to the year-round access to Longyearbyen, low comparative cost, and local support. The Ultralite LDB program also make accessible a quick opportunity for testing components in a real time environment for future Rights (large LDB systems) as well as a stratospheric platforms for science research. For the 2007 summer season there will be further testing of TM systems as well as continuing with our successful Ultra Light LDB. Programs for 2007 include staging of equipment in Longyearbyen to support the 2008 OLIMPO and BOOMERanG experiments, setting up integration facilities for experimenters, and performing system tests. Since 2003, ASI and ARR have launched 10 LDB systems with balloon payloads reaching up to a maximum of 39 days at the float altitude from the world's most northern scientific balloon research facility ... the Nobile/Amundsen Stratospheric Balloon Center at Svalbard.

Published
2007

12. The BRAIN project: looking for B-mode from Dome-C

Author

Cressiot, C., Piat, M., Kaplan, J., Bréelle, E., Dufour, C., Rosset, C., Masi, S., Polenta, G., Peterzen, S., AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), D. Barret, F. Casoli, G. Lagache, A. Lecavelier, L. Pagani, BRAIN, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

Texte integral disponible sur http://proc.sf2a.asso.fr/sf2a06.php; International audience; The detection and characterisation of Cosmic Microwave Background B-mode polarization is one of the next challenges in observational cosmology. This primordial polarization mode is only due to tensor perturbations of the metric produced by primordial gravitational waves, which could have been generated during the inflation epoch. With a signal of less than 0.1? K, B-mode measurement requires very sensitive experiments and also an extremely good control of instrumental effects. In this paper we present the BRAIN experiment, a bolometric interferometer devoted to B-mode detection. This new detection architecture allows to directly measure the Fourier modes of the Stokes parameters. High sensitivity is obtained by using low temperature bolometers while systematic effects are reduced by using the interferometric technique.

Published
2006

13. A long duration balloon borne mm and sub-mm telescope for multi-frequency survey of galaxy clusters and CMB

Author

Nati, F., Nati, L., Conversi, L., Silvia Masi, Calvo, M., Paolo de Bernardis, Petris, M. D., Troia, G. D., Lacoangeli, A., Lamagna, Luca, Bettolo, C. M., Alessandro Melchiorri, Melchiorri, F., Francesco Piacentini, Polenta, G., Ade, P., Hargrave, P., Mauskopf, P., Orlando, A., Giampaolo Pisano, Savini, G., Tucker, C., Boscaleri, A., Peterzen, S., Colafrancesco, S., Rephaeli, Y., Romeo, G., Salvaterra, L., Delbart, A., Juin, J. B., Magneville, C., Pansart, J. P., and Yvon, D.

Subjects
Cosmic Microwave Background radiation, balloon borne experiments, millimetre waves, Cosmic Microwave Background radiation, Sunyaev-Zeldovich effect, balloon borne experiments, millimetre waves, Sunyaev-Zeldovich effect
Published
2006

14. Pegaso: an ultra-light long duration stratospheric

Author

Romeo G., Peterzen S., Masi S., Di Stefano G., Di Felice F., Ibba R., Cardillo A., Musso I., Benedetti P., Caprara F., Iarocci A., Mari M., Palangio P., Spinelli G., Spoto D., Urbini G., and Drakoy P.

Subjects
tratospheric balloons, Geomagnetic crustal anomalies
Abstract

Launched from the Mario Zuccelli Station (Baia Terra Nova) in Antarctica during the 2005/06 austral summer, the PEGASO-D payload lifted into the stratospheric anticyclone over the southern polar region. This effort marks the first Long Duration Scientific payload to be launched from this location and is the fourth such payload launched in the polar regions. Performing in the framework of the NOBILE/AMUNDSEN collaborative LDB development between ASI-ARR. The Italian Institute of Geophysics and Volcanology (INGV), with the sponsorship of the Italian Antarctic Program (PNRA) and the Italian Space Agency (ASI),designed and built the Ultra-Light system together with three Universities in Italy. The Pegaso program has been created to investigate the Earth magnetic field and provide a precursor series of small payload launches for the bigger LDB program such as OLIMPO, BOOMERanG and BArSPOrt through this collaboration between ASI and ARR. The Italian scientific community, aware of the big advantages that LDB balloons can offer to their experiments, proposed to extend the LDB program to Southern polar regions, besides performing launches from the newly initiated Nobile/Amundsen Stratospheric Balloon Center in Svalbard, Norway.Three PEGASO (Polar Explorer for Geomagnetics And other Scientific Observations) payloads have been launched from the Svalbard (No) in collaboration with Andoya Rocket Range, ASI and ISTAR (Operations and logistics) during the past two northern summers. These stratospheric (altitude m.35000) small 10kmc balloons have floated in the stratosphere between 14 to 39 days measuring the magnetic field of polar regions, by means of a 3-axys-fluxgate magnetometer, during a three year campaign. The study of the magnetic field and its variations is done through permanent observatories. They provide us with high quality data but their spatial distribution is not quite regular, specially in Antarctica due to logistic difficulties. The coverage is improved through marine and aeromagnetic surveys, and also through satellite missions. There exists nevertheless a gap in the wavelengths of the magnetic field represented by these kind of measurements. Satellite data are too far away from Earth's surface to individuate wavelengths lower than 1000 km, and near-ground sur- veys are not able to represent wavelengths longer than the dimensions of the surveyed area. Moreover, there is a region empty of data around the geographical pole for the satellite measurements. The size of these gaps depends on the orbital parameters, but it can reach up to 10 degrees around the pole. PEGASO allows to bridge this gap in the measurements of the magnetic field. Surveys carried out at 35 km height allow the study of crustal anomalies in the range between, we can say, 60 and 1000 km. Taking into account that pathfinders (smaller non-recoverable balloon systems) are usually sent to explore the atmospheric currents, the use of PEGASO as pathfinder allows us to obtain all these results at a very affordable cost. The PEGASO payload was also developed as a single source system integrating science, housekeeping and operational control of the entire balloon borne configuration.Satellite telemetry sent the scientific (magnetometric) data, house-keeping (temperature, solar panel voltage and current, altitude and time) and telecommand (four ballast, two parachute release system, system reset), and powered the terminate system. Data flows through the IRIDIUM telephone service. The onboard systems were kept inside a vessel (white painted and pressurizzed vessel due to power dissipation) except for external flexible solar panels and magnetometer, attached to an external boom. Two redundant tracking systems have been used: a first GPS was integrated inside the on-board telemetry system, necessary to reconstruct position and time of scientific data, while an independent GPS-ARGOS system gave the balloon trajectory, including its descent. Continuous trajectory predictions were made during the missions; they have been necessary, in particular, for the flight safety requirements of the northern hemisphere. The evaluation of the statistical error is proposed. The PEGASO payload was developed to be a light, cost effective way to explore the potential of Ultra-Light Long Duration Ballooning for science as well as an introduction to the earth-space possibilities for students.

Published
2006

15. Olimpo: a multi-wavelength survey of galaxy clusters and of the cosmic sub-mm/mm background

Author

Federico Nati, Nati, L., Conversi, L., Silvia Masi, Calvo, M., Paolo de Bernardis, Marco De Petris, De, G., Troia, Iacoangeli, A., Lamagna, Luca, Marini Bettolo, C., Alessandro Melchiorri, Melchiorri, F., Francesco Piacentini, Polenta, Gianluca, Ade, P., Hargrave, P., Mauskopf, P., Orlando, A., Giampaolo Pisano, Savini, G., Tucker, C., Boscaleri, A., Peterzen, S., Colafrancesco, S., Rephaeli, Y., Romeo, G., Salvaterra, L., Delbart, A., Juin, J. B., Magneville, C., Pansart, J. P., and Yvon, D.

Published
2006

16. Development of a long duration balloon program in the polar regions - Svalbard, Norway

Author

Peterzen S., Rabbia S., Cardillo A., Musso I., and Leonardi A.

Subjects
Balloon flight in polar regions, Stratospheric balloons, Long duration balloon flight
Abstract

The Italian Space Agency (Agenzia Spaziale Italiana, ASI) in a joint effort with Andøya Rocket Range (ARR), anticipates launching a total of 3 'Pathfinder' balloons from Svalbard (Norway) during the 2003 summer. The balloons will carry a payload of a GPS/Argos transmitter for tracking. This campaign is designed to prove concept for launching larger Long Duration Balloons (LDB) in the future from this high latitude location. These small (75 cubic meters/0.265 mcf) balloons reach an altitude of +/- 5mb (127kft) and will circumnavigate the polar region between 78 and 80 deg. N. Making use of the Pathfinder balloons with a GPS/ARGOS payload for tracking purposes, this investigation will obtain a trajectory showing the stratospheric circulation pattern of stratospheric winds, diurnal excursions, and potential termination/impact locations for the future LDB flights.

Published
2003

17. THE BRAIN EXPERIMENT

Author

POLENTA, G., primary, CALVO, M., additional, CONVERSI, L., additional, de BERNARDIS, P., additional, GIORDANO, C., additional, IACOANGELI, A., additional, MAIELLO, M., additional, MARINI-BETTOLO, C., additional, MASI, S., additional, NATI, F., additional, NATI, L., additional, PETERZEN, S., additional, PIACENTINI, F., additional, SORDINI, R., additional, VENEZIANI, M., additional, BARTLETT, J., additional, BRÉELLE, E., additional, DUFOUR, C., additional, GALLI, S., additional, GANGA, K., additional, GHRIBI, A., additional, GIRAUD-HERAUD, Y., additional, GUGLIELMI, L., additional, HAMILTON, J.C., additional, KAPLAN, J., additional, PIAT, M., additional, GERVASI, M., additional, SIRONI, G., additional, SPINELLI, S., additional, TARTARI, A., additional, ZANNONI, M., additional, MAFFEI, B., additional, PICCIRILLO, L., additional, PISANO, G., additional, ADE, P., additional, ORLANDO, A., additional, SAVINI, G., additional, BROSSARD, J., additional, GIARD, M., additional, LANDÉ, J., additional, BERGÉ, L., additional, DUMOULIN, L., additional, JUILLARD, A., additional, MARNIEROS, S., additional, PAJOT, F., additional, and ROSSET, C., additional

Published
2008
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18. The OLIMPO experiment

Author

Nati, F., primary, Ade, P., additional, Boscaleri, A., additional, Brienza, D., additional, Calvo, M., additional, Colafrancesco, S., additional, Conversi, L., additional, de Bernardis, P., additional, De Petris, M., additional, Delbart, A., additional, Hargrave, P., additional, Iacoangeli, A., additional, Juin, J.B., additional, Magneville, C., additional, Marini Bettolo, C., additional, Masi, S., additional, Mauskopf, P., additional, Melchiorri, F., additional, Nati, L., additional, Orlando, A., additional, Rephaeli, Y., additional, Romeo, G., additional, Pansart, J.P., additional, Peterzen, S., additional, Piacentini, F., additional, Pisano, G., additional, Polenta, G., additional, Salvaterra, L., additional, Savini, G., additional, Tucker, C., additional, and Yvon, D., additional

Published
2007
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19. Precision CMB Polarization from Dome-C: the BRAIN experiment

Author

Masi, S., primary, de Bernardis, P., additional, Giordano, C., additional, Nati, F., additional, Piacentini, F., additional, Polenta, G., additional, Veneziani, M., additional, Gervasi, M., additional, Sironi, G., additional, Tartari, A., additional, Zannoni, M., additional, Peterzen, S., additional, Bartlett, J., additional, Giraud-Heraud, Y., additional, Piat, M., additional, Rosset, C., additional, Giard, M., additional, Pons, R., additional, Maffei, B., additional, Ade, P., additional, Gear, W., additional, Mauskopf, P., additional, Piccirillo, L., additional, Pisano, G., additional, and Savini, G., additional

Published
2005
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20. Background Microwave Radiation and Intracluster Cosmology

Author

Silvia Masi, Calvo, M., Conversi, L., Paolo de Bernardis, Marco De Petris, Troia, G., Iacoangeli, A., Lamagna, Luca, Marini Bettolo, C., Alessandro Melchiorri, Melchiorri, F., Nati, L., Federico Nati, Francesco Piacentini, Polenta, G., Valiante, E., Ade, P., Hargrave, P., Mauskopf, P., Orlando, A., Giampaolo Pisano, Savini, G., Tucker, C., Boscaleri, A., Peterzen, S., Colafrancesco, S., Rephaeli, Y., Romeo, G., Salvaterra, L., Delbart, A., Juin, J. B., Magneville, C., Pansart, J. P., Yvon, D., Multi Frequency Survey Of Galaxy Clusters And Of The Cosmic Millimetric Background, Olimpo A., and In Melchiorri, F.

21. DUSTER (Dust in the Upper Stratosphere Tracking Experiment and Retrieval) . PRELIMINARY ANALYSIS

Author

Ciucci, A., Palumbo, P., Brunetto, R., Della Corte, V., Angelis, S., Rotundi, A., Rietmeijer, F. J. M., Zona, E., Colangeli, L., Francesca Esposito, Mazzotta Epifani, E., Mennella, V., Inarta, S., Peterzen, S., Masi, S., Ibba, R., Ciucci, Alessandra, P., Palumbo, R., Brunetto, V., Della Corte, DE ANGELIS, Simone, A., Rotundi, F. J. M., Rietmeijer, E., Zona, L., Colangeli, F., Esposito, E., Mazzotta Epifani, V., Mennella, S., Inarta, S., Peterzen, S., Masi, and R., Ibba

Subjects
laboratory analyse, Stratospheric dust, FESEM-EDX
Abstract

The DUSTER project is aimed at uncontaminated collection and retrieval of stratospheric solid aerosol particles, in the submicron/micron range. The Earth stratosphere contains extraterrestrial dust, dust from natural and anthropogenic activities. Our main target is the study of dust originated in our planetary system. We present here the preliminary results of the June 2008 campaign. After recovery, collected particles were identified by comparing FESEM images taken on the pre-flight collector with those obtained on the post-fight collector. Possible contamination was monitored by FESEM observation of the 'Blank'. Morphology, dimension, and composition of collected particles were defined using a FESEM equipped with an EDX system. The collected sample are in the size range 0.5-150 μm, ≈30% of aerosols sizing 0.5-1.5 μm, a range poorly studied so far.

22. DUSTER (Dust in the Upper Stratosphere Tracking Experiment and Return):. a balloon-borne dust particle collector

Author

Della Corte, V., Palumbo, P., Angelis, S., Ciucci, A., Brunetto, R., Rotundi, A., Rietmeijer, F. J. M., Zona, E., Bussoletti, E., Colangeli, L., Esposito, F., Mazzotta Epifani, E., Vito Mennella, Peterzen, S., Masi, S., Ibba, R., V., Della Corte, P., Palumbo, DE ANGELIS, Simone, Ciucci, Alessandra, R., Brunetto, A., Rotundi, F. J. M., Rietmeijer, E., Zona, E., Bussoletti, L., Colangeli, F., Esposito, E., Mazzotta Epifani, V., Mennella, S., Peterzen, S., Masi, and R., Ibba

Subjects
Interplanetary dust, Stratospheric aerosol collection, balloon-borne
Abstract

The DUSTER (Dust in the Upper Stratosphere Tracking Experiment and Retrieval) project is aimed at uncontaminated collection and retrieval of stratospheric solid aerosol particles, in the submicron/micron range, from the upper stratosphere. The approach implies: (1) in-situ particles collection; (2) sample recovering; and (3) laboratory analyses. The scientific aim is deriving the dust size distribution, the concentration, chemistry and mineralogy of the collected stratospheric aerosols. The main characteristics of the instrument are: (1) Capability of working autonomously during balloon flight at 30-40 km altitude, temperatures down to -80°C; (2) sampling at least 20 m3 of air to collect several hundreds of aerosol particles); (3) Samples storage and retrieval under controlled conditions. A detailed description of the experiment is reported here.

23. Ultralight to heavy long duration balloon development from Svalbard, Norway

Author

Peterzen, S. E., Ibba, R., Bøen, K., Dragoy, P., Silvia Masi, Cardillo, A., Musso, I., and Spoto, D.

Subjects
Long Duration Balloon Flight, Circumpolar trajectory
Abstract

Science teams world wide have made use of stratospheric research balloons to conduct experimentation through various disciplines and for as many reasons. High altitude balloons have been the vehicle to carry on investigations of space, our atmosphere, and our planet. Balloons have proven to be a cost efficient and rapidly deployable means to gain access to the heavens. In a joint effort, the Italian Space Agency (ASI) and Andoya Rocket Range (ARR) have initiated the development of a European balloon center in Svalbard, Norway. This new facility, Nobile / Amundsen Stratospheric Balloon Center - Svalbard, has arguably the ideal location for performing Long Duration Balloon (LDB) campaigns.

24. The OLIMPO experiment

Author

Federico Nati, Nati, L., Conversi, L., Silvia Masi, Calvo, M., Paolo de Bernardis, Marco De Petris, Troia, G., Iacoangeli, A., Lamagna, Luca, Marini Bettolo, C., Alessandro Melchiorri, Melchiorri, F., Nati, F., Francesco Piacentini, Polenta, G., Valiante, E., Ade, P., Hargrave, P., Mauskopf, P., Orlando, A., Giampaolo Pisano, Savini, G., Tucker, C., Boscaleri, A., Peterzen, S., Colafrancesco, S., Rephaeli, Y., Romeo, G., Salvaterra, L., Delbart, A., Juin, J. B., Magneville, C., Pansart, J. P., and Yvon, D.

25. OLIMPO: A multi-frequency survey of galaxy clusters and of the cosmic millimetric background

Author

Silvia Masi, Calvo, Martino, Conversi, Luca, Paolo de Bernardis, Marco De Petris, Troia, Grazia, Iacoangeli, Armando, Lamagna, Luca, Marini Bettolo, Cecilia, Alessandro Melchiorri, Melchiorri, Francesco, Nati, Lavinia, Federico Nati, Francesco Piacentini, Polenta, Gianluca, Valiante, E., Ade, P., Hargrave, P., Mauskopf, P., Orlando, A., Giampaolo Pisano, Savini, G., Tucker, C., Boscalieri, A., Peterzen, S., Colafrancesco, S., Rephaeli, Y., Romeo, G., Salvaterra, L., Delbart, A., Juin J, B., Magneville, C., Pansart J, P., and Yvon, D.

26. A balloon-borne survey of the mm/sub-mm sky: OLIMPO

Author

Silvia Masi, Calvo, Martino, Conversi, Luca, Paolo de Bernardis, Marco De Petris, Troia, Grazia, Iacoangeli, Armando, Lamagna, Luca, Marini Bettolo, Cecilia, Melchiorri, Francesco, Alessandro Melchiorri, Nati, Lavinia, Federico Nati, Francesco Piacentini, Polenta, Gianluca, Valiante, E., Ade, P., Hargrave, P., Mauskopf, P., Orlando, A., Giampaolo Pisano, Savini, Giorgio, Tucker, C., Boscaleri, A., Peterzen, S., Colafrancesco, S., Rephaeli, Y., Romeo, G., Salvaterra, L., Delbart, A., Juin, J. B., Magneville, C., Pansart, J. P., and Yvon, D.

27. Mapping clusters of galaxies with a stratospheric balloon experiment

Author

Masi, S., Brienza, D., Conversi, L., Paolo de Bernardis, Petris, M., Fiadino, P., Iacoangeli, A., Lamagna, L., Bettolo, C. M., Moncelsi, L., Nati, L., Nati, F., Piacentini, F., Polenta, G., Rispoli, R., Ade, P. A. R., Hargrave, P., Mauskopf, P., Pisano, G., Savini, G., Tucker, C., Boscaleri, A., Peterzen, S., Spoto, D., Carpinteri, D., Colafrancesco, S., Rephaeli, Y., Di Stefano, G., Romeo, G., Delbart, A., Doumoulin, L., Camus, P., Juin, J. B., Magneville, C., Pansart, J. P., Yvon, D., Gromov, V., and Maslov, I.

Subjects
Clusters of galaxies, Cosmology, Long duration stratospheric balloons

28. QUBIC: the Q&U Bolometric Interferometer for Cosmology

Author

Massimo Gervasi, C. Giordano, A. Passerini, Andrei Korotkov, E. Bréelle, Jean Christophe Hamilton, A. Ghribi, L. Vibert, Gregory S. Tucker, Emory F. Bunn, Angelo Cruciani, B. Maffei, P. de Bernardis, Michel Piat, J. Martino, G. Curran, A. Bounab, L. Guglielmi, F. Voisin, Elia S. Battistelli, Alessandro Schillaci, Roberto Sordini, R. Charlassier, F. Piacentini, Andrea Tartari, A. Baù, Lucio Piccirillo, G. Bordier, Y. Giraud-Heraud, Maria Salatino, M. Maiello, Martino Calvo, D. Bennett, S. Peterzen, L. Dumoulin, Peter Timbie, Silvia Masi, J. Kaplan, D. Prêle, S. Malu, Victor Haynes, Giampaolo Pisano, Martin Giard, M.-A. Bigot-Sazy, David Romano, J. Lande, Sophie Collin, Mario Zannoni, Federico Nati, Créidhe O'Sullivan, Laurent Bergé, Robert A. Watson, Marcin Gradziel, Gianluca Polenta, François Pajot, L. A. Montier, C. Parisel, A. Gault, S. Spinelli, C. Rosset, Anna Murphy, S. Marnieros, J.-P. Bernard, G. Sironi, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), QUBIC, Piat, M, Battistelli, E, Bau', A, Bennett, D, Berge, L, Bernard, J, de Bernardis, P, Bigot Sazy, M, Bordier, G, Bounab, A, Breelle, E, Bunn, E, Calvo, M, Charlassier, R, Collin, S, Cruciani, A, Curran, G, Dumoulin, L, Gault, A, Gervasi, M, Ghribi, A, Giard, M, Giordano, C, Giraud Heraud, Y, Gradziel, M, Guglielmi, L, Hamilton, J, Haynes, V, Kaplan, J, Korotkov, A, Lande, 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, Prele, 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, Zannoni, M, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CSNSM INSTR, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), CSNSM PS1, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Dipartimento di Fisica, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Dipartimento di Fisica 'Giuseppe Occhialini' = Department of Physics 'Giuseppe Occhialini' [Milano-Bicocca], Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Department of Experimental Physics, National University of Ireland Maynooth (Maynooth University), Université Paris-Sud - Paris 11 (UP11), CNRS/Université de Toulouse, Physics Department, University of Richmond, Richmond, Department of Physics [Madison], University of Wisconsin-Madison, University of Manchester [Manchester], Brown University, Università degli Studi di Siena = University of Siena (UNISI), Raman Research Institute, ASI Science Data Center, Bergé, L, A., B, Bréelle, E, Coppolecchia, A, Giraud Héraud, Y, Landé, J, O’Sullivan, C, de Petris, M, and Prêle, D

Subjects
Bolometric interferometry, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Astrophysics, 01 natural sciences, Cosmology, law.invention, Gravitational wave background, law, bolometer, cosmic microwave background, polarisation, interferometer, Cosmic Microwave Background, General Materials Science, Interferometer, 010303 astronomy & astrophysics, Instrumentation, Polarisation, media_common, Physics, instrumentation, Astrophysics::Instrumentation and Methods for Astrophysics, bolometric interferometry, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Interferometry, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], media_common.quotation_subject, Bolometer, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology, Cosmic Microwave Background, Inflation, Instrumentation, Bolometric interferometry, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FIS/05 - ASTRONOMIA E ASTROFISICA, Materials Science(all), 0103 physical sciences, inflation, 010306 general physics, cosmology, Instrumentation and Methods for Astrophysics (astro-ph.IM), Inflation (cosmology), 010308 nuclear & particles physics, Gravitational wave, Astronomy, Astronomy and Astrophysics, Inflation, Universe, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
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
2012

29. The BRAIN CMB polarization experiment

Author

R. Pons, Mario Zannoni, M. Giard, S. Peterzen, G. Sironi, Silvia Masi, J. Bartlett, E. Bréelle, Peter A. R. Ade, F. Piacentini, M. Piat, M. Veneziani, Federico Nati, P. de Bernardis, Y. Giraud-Héraud, Giampaolo Pisano, Massimo Gervasi, C. Giordano, Giorgio Savini, C. Rosset, Bruno Maffei, G. Polenta, Lucio Piccirillo, C. Dufour, Luca Conversi, Angiola Orlando, Andrea Tartari, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Paolo de Bernardis, Marco De Petris, Luca Lamagna, Roberto Maoli, Silvia Masi and Alessandro Melchiorri, BRAIN, Polenta, G, Ade, P, Bartlett, J, Bréelle, E, Conversi, L, de Bernardis, P, Dufour, C, Gervasi, M, Giard, M, Giordano, C, Giraud Heraud, Y, Maffei, B, Masi, S, Nati, F, Orlando, A, Peterzen, S, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Pons, R, Rosset, C, Savini, G, Sironi, G, Tartari, A, Veneziani, M, Zannoni, M, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Polarimetry, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 98.80.−k, 95.75.Hi, 95.75.Kk, 98.70.Vc, 7. Clean energy, 01 natural sciences, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, FIS/05 - ASTRONOMIA E ASTROFISICA, law, 0103 physical sciences, Astronomical interferometer, Stokes parameters, 010303 astronomy & astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Bolometer, background radiation, cosmology, interferometry, polarimetry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Cryocooler, Polarization (waves), Cosmology, Interferometry, 13. Climate action, Space and Planetary Science, Background radiation, symbols
Abstract

International audience; In the standard cosmological scenario tensor perturbations of the metric produce a rotational component in the Cosmic Microwave Background polarization, called B-modes. The expected signal is of the order of not, vert, similar0.1 μK, well beyond the sensitivity of current experiments. In this paper, we introduce the BRAIN experiment, a bolometric interferometer devoted to measure the B-modes polarization of the CMB from Concordia station in Antarctica. This experiment will take advantage of both high sensitivity of bolometer arrays and low level of systematic effects of interferometers. We report the results obtained during the first campaign we carried out this austral summer at Dome-C. Using a pathfinder experiment, we demonstrated that a cryocooler based cryogenic system can work in such environmental conditions. We also carried out preliminary observations of the atmospheric emission at 145 GHz from Dome-C, and during the next campaign we'll extend the measurements to all the Stokes parameters I, Q, U, V all over the winter.

Published
2006

30. Precision CMB Polarization from Dome-C: the BRAIN experiment

Author

Giorgio Savini, J. Bartlett, Walter Kieran Gear, R. Pons, Mario Zannoni, Lucio Piccirillo, S. Peterzen, Andrea Tartari, Bruno Maffei, F. Piacentini, Philip Daniel Mauskopf, M. Giard, P. de Bernardis, Massimo Gervasi, C. Giordano, G. Polenta, Y. Giraud-Héraud, Federico Nati, Peter A. R. Ade, C. Rosset, M. Veneziani, Giampaolo Pisano, G. Sironi, M. Piat, Silvia Masi, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), M. Giard, F. Casoli, F. Paletou, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Masi, S, de Bernardis, P, Giordano, C, Nati, F, Piacentini, F, Polenta, G, Veneziani, M, Gervasi, M, Sironi, G, Tartari, A, Zannoni, M, Peterzen, S, Bartlett, J, Giraud Heraud, Y, Piat, M, Rosset, C, Giard, M, Pons, R, Maffei, B, Ade, P, Gear, W, Mauskopf, P, Piccirillo, L, Pisano, G, Savini, G, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Polarimetry, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Cosmology, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FIS/05 - ASTRONOMIA E ASTROFISICA, 0103 physical sciences, 010303 astronomy & astrophysics, QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Linear polarization, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, General Engineering, Astronomy, Astronomy and Astrophysics, Polarization (waves), Interferometry, CMB, Polarimetry, Cosmology, Bolometers, Interferometry, Pathfinder, Space and Planetary Science, Big Bang, Bolometric interferometer, CMB polarization
Abstract

In the current cosmological scenario, part of the linearly polarized emission of the CMB is expected to be rotational (B-modes). This component is due to tensor perturbations of the metric produced by primordial gravitational waves, which are generated a split-second after the Big Bang. The signal expected is of the order of

Published
2005

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