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Cressiot C. (2006).
Abstract: Training period report (advisor: Michel Piat)
Programme: 915
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Polenta G. and the BRAIN collaboration. (2007). The Brain CMB polarisation experiment. New astronomy reviews, 3(4), 256–259.
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Piat M. (2007). Precise measurement of CMB polarisation from Dome-C: the BRAIN experiment.
Abstract: Workshop Submm/FIR astronomy from Antarctica, CEA Saclay – June 25-27th – Framework: ARENA
Programme: 915
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Polenta G. for the BRAIN collaboration. (2007). The BRAIN experiment.
Abstract: in proceedings of the 11th Marcel Grossmann meeting, (R. Ruffini, H. Kleinert, R. Jantzen editors)
Programme: 915
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Silvia Masi for the BRAIN collaboration. (2004). Precision CMB Polarization from Dome-C: the BRAIN experiment.
Abstract: in EAS Publications Series, volume 14, page 87-92, 2005
Programme: 915
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Giordano C. (2005). BRAIN: un polarimetro per lo studio del fondo a microonde da Dome Concordia.
Abstract: degree thesis, advisors Paolo de Bernardis and Silvia Masi
Programme: 915
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Maiello M. (2006). Misure di polarizzazione del fondo cosmico a microonde con l'esperimento BRAIN.
Abstract: degree thesis, advisor Silvia Masi
Programme: 915
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Silvia Galli. (2007). Bolometric interferometry demonstrator to measure the Cosmic Microwave Background Polarization.
Abstract: report of a Master degree, advisor Michel Piat
Programme: 915
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Battistelli E, others, . (2011). QUBIC: The QU Bolometric Interferometer for Cosmology
. Astropart.Phys., 34, 705–716.
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. (2011). QUBIC: the Q&U Bolometric Interferometer for Cosmology
. Springer Netherlands.
Abstract: The primordial B-mode polarisation of the Cosmic Microwave Background is the imprints of the gravitational wave background generated by inflation. Observing the B-mode is up to now the most direct way to constrain the physics of the primordial Universe, especially inflation. To detect these B-modes, high sensitivity is required as well as an exquisite control of systematics effects. To comply with these requirements, we propose a new instrument called QUBIC (Q and U Bolometric Interferometer for Cosmology) based on bolometric interferometry. The control of systematics is obtained with a close-packed interferometer while bolometers cooled to very low temperature allow for high sensitivity. We present the architecture of this new instrument, the status of the project and the self-calibration technique which allows accurate measurement of the instrumental systematic effects.
Keywords: Physics and Astronomy,
Programme: 915
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