BS -1 BS 0 BS 1 BS 2 10 10 10 10 2.5 5 2.5 2.5 5 5 2.0 5 The5 QUBIC Experiment 4 2.0 2.0 1.5 0 3 0 0 1.5 0 1.5 1.0 2 A1.0 bolometric interferometer1.0 to measure -5 -5 -5 -5 0.5 1 0.5 0.5 -10 0 -10 0.0 -10 the0.0 -10B modes of 0.0 the polarized CMB fluctuations -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 BS 3 BS 4 BS 5 Resulting signal 10 10 10 10 8 2.5 2.5 2.5 5 5 5 5 6 2.0 2.0 2.0 0 1.5 0 1.5 0 1.5 0 4 1.0 1.0 1.0 -5 -5 -5 -5 2 0.5 0.5 0.5 Romain Charlassier (APC Paris) -10 0.0 -10 0.0 -10 0.0 -10 0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 on behalf of the QUBIC collaboration BS -1 BS 0 BS 1 BS 2 10 10 10 10 2.5 5 2.5 2.5 5 5 2.0 5 5 4 2.0 2.0 1.5 0 3 0 0 1.5 0 1.5 1.0 2 Getting1.0 the1.0 B modes will be very hard... -5 -5 -5 -5 0.5 1 0.5 0.5 -10 0 -10 0.0 -10 0.0 -10 0.0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 BS 3 BS 4 BS 5 Resulting signal wmap5y + quad (ade et al. 2007) 10 10 10 10 8 100.000 2.5 2.5 2.5 5 5 5 5 6 2.0 2.0 2.0 tt 0 1.5 0 1.5 0 1.5 0 4 c 1.0 1.0 1.0 -5 -5 -5 -5 2 10.000 0.5 0.5 0.5 -10 0.0 -10 0.0 -10 • Detecting 0.0 -10 B modes requires:0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 te c k] - A very high statistical sensitivity µ 1.000 ) [ π An extremely good control of cee - BICEP 2009 systematics t/s=0.1 0.100 - A reliable foreground subtraction sqrt(l(l+1)cl/2 t/s=0.01 (true for all-sky but what about a cbb t/s=0.001 clean small field ?) 0.010 cbb lensing 0.001 1 10 100 1000 ell Romain Charlassier - The QUBIC Collaboration - Rencontres de Moriond on Cosmology 2010 BS -1 BS 0 BS 1 BS 2 10 10 10 10 2.5 5 2.5 2.5 5 5 2.0 5 5 4 2.0 2.0 1.5 0 3 0 0 1.5 0 1.5 1.0 2 Current1.0 and1.0 future B-mode experiments -5 -5 -5 -5 0.5 1 0.5 0.5 -10 0 -10 0.0 -10 0.0 -10 0.0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 • Imagers (Bolometric: BICEP, EBEX, PolarBear, Spider..; BS 3 BS 4 BS 5 Resulting signal 10 10 10 10 8 2.5 2.5 Heterodyne:2.5 QUIET): 5 5 5 5 6 2.0 2.0 2.0 0 1.5 0 1.5 0 - Very1.5 0 good sensitivity 4 with large bolometers arrays, large 1.0 1.0 1.0 -5 -5 -5 -5 2 0.5 0.5 bandwidth0.5 + very well known technology -10 0.0 -10 0.0 -10 0.0 -10 0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 - Systematics handling ? HWP + scan. • Heterodyne interferometers (CHIP project) - Worked by the past (VSA, CBI, DASI) - Not very scalable (NxN correlator very expensive) ? HEMTs not competitive in space - Better for systematics Bolometric interferometer (QUBIC): Could combine the advantages of both techniques ? Romain Charlassier - The QUBIC Collaboration - Rencontres de Moriond on Cosmology 2010 BS -1 BS 0 BS 1 BS 2 10 10 10 10 2.5 5 2.5 2.5 5 5 2.0 5 5 4 2.0 2.0 1.5 0 3 0 0 The1.5 0 QUBIC 1.5 collaboration 1.0 2 1.0 1.0 -5 -5 -5 A-5 merging of MBI (USA/UK) with BRAIN (France/Italy/UK) 0.5 1 0.5 0.5 -10 0 -10 0.0 -10 0.0 -10 0.0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 BS 3 BS 4 BS 5 Resulting signal 10 10 10 10 8 2.5 2.5 2.5 5 5 5 5 6 2.0 2.0 2.0 0 1.5 0 1.5 0 1.5 0 4 1.0 1.0 1.0 -5 -5 -5 -5 2 0.5 0.5 0.5 -10 0.0 -10 0.0 -10 0.0 -10 0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 APC Paris, France IAS Orsay, France CSNSM Orsay, France CESR Toulouse, France IUCAA, Pune, India Maynooth University, Ireland Universita di Milano-Bicocca, Italy Universita La Sapienza, Roma, Italy University of Manchester, UK Richmond University, USA Brown University, USA University of Wisconsin, USA Romain Charlassier - The QUBIC Collaboration - Rencontres de Moriond on Cosmology 2010 BS -1 BS 0 BS 1 BS 2 10 10 10 10 2.5 5 2.5 2.5 5 5 2.0 5 5 4 2.0 2.0 incoming 1.5 0 3 0 0 1.5 0 1.5 1.0 The QUBIC instrument concept radiation 2 1.0 1.0 -5 -5 -5 -5 0.5 1 0.5 0.5 -10 0 -10 0.0 -10 0.0 -10 0.0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 Sky BS 3 BS 4 BS 5 Resulting signal ~35 cm 10 10 10 10 8 2.5 2.5 2.5 horns 5 5 5 5 6 4K 2.0 2.0 2.0 0 1.5 0 1.5 0 1.5 0 4K4 switches ? 1.0 1.0 1.0 -5 -5 -5 -5 2 0.5 0.5 0.5 back 4K -10 0.0 -10 0.0 -10 0.0 -10 0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 horns Half-Wave Plate 4K ~60 cm ~40 cm ~10 cm 4K Polarization sensitive detectors 300 mK Cryostat ~70 cm Romain Charlassier - The QUBIC Collaboration - Rencontres de Moriond on Cosmology 2010 BS -1 BS 0 BS 1 BS 2 10 10 10 10 2.5 5 2.5 2.5 5 5 2.0 5 5 4 2.0 2.0 incoming 1.5 0 3 0 0 1.5 0 1.5 1.0 The QUBIC instrument concept radiation 2 1.0 1.0 -5 -5 -5 -5 0.5 1 0.5 0.5 -10 0 -10 0.0 -10 0.0 -10 0.0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 Sky BS 3 BS 4 BS 5 Resulting signal ~35 cm 10 10 10 10 8 2.5 2.5 2.5 horns 5 5 5 5 6 4K 2.0 2.0 2.0 0 1.5 0 1.5 0 1.5 0 4K4 switches ? 1.0 1.0 1.0 -5 -5 -5 -5 2 0.5 0.5 0.5 back 4K -10 0.0 -10 0.0 -10 0.0 -10 0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 horns Half-Wave Plate 4K ~60 cm ~40 cm ~10 cm 4K Polarization sensitive detectors 300 mK Cryostat ~70 cm Romain Charlassier - The QUBIC Collaboration - Rencontres de Moriond on Cosmology 2010 BS -1 BS 0 BS 1 BS 2 10 10 10 10 2.5 5 2.5 2.5 5 5 2.0 5 5 4 2.0 2.0 incoming 1.5 0 3 0 0 1.5 0 1.5 1.0 The QUBIC instrument concept radiation 2 1.0 1.0 -5 -5 -5 -5 0.5 1 0.5 0.5 -10 0 -10 0.0 -10 0.0 -10 0.0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 Sky BS 3 BS 4 BS 5 Resulting signal ~35 cm 10 10 10 10 8 2.5 2.5 2.5 horns 5 5 5 5 6 4K 2.0 2.0 2.0 0 1.5 0 1.5 0 1.5 0 4K4 switches ? 1.0 1.0 1.0 -5 -5 -5 -5 2 0.5 0.5 0.5 back 4K -10 0.0 -10 0.0 -10 0.0 -10 0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 horns Half-Wave Plate 4K ~60 cm ~40 cm ~10 cm 4K Polarization sensitive detectors 300 mK Cryostat ~70 cm Romain Charlassier - The QUBIC Collaboration - Rencontres de Moriond on Cosmology 2010 BS -1 BS 0 BS 1 BS 2 10 10 10 10 2.5 5 2.5 2.5 5 5 2.0 5 5 4 2.0 2.0 incoming 1.5 0 3 0 0 1.5 0 1.5 1.0 The QUBIC instrument concept radiation 2 1.0 1.0 -5 -5 -5 -5 0.5 1 0.5 0.5 -10 0 -10 0.0 -10 BS -1 BS -1 0.0 -10 BS 0 0.0 BS 0 BS 1 BS 1 BS 2 BS 2 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 10 10 10 10 10 10 10 10 2.5 2.5 Sky 5 5 2.5 2.5 2.5 2.5 5 5 5 5 2.0 5 2.0 5 5 5 BS 3 BS 4 BS 5 Resulting signal ~35 cm 4 4 2.0 2.0 2.0 2.0 10 10 10 10 8 1.5 1.5 2.5 2.5 2.5 0 0 3 0 3 0 0 0 1.5 0 1.5 0 horns 1.5 1.5 5 5 5 5 6 4K 2.0 2.0 2.0 1.0 1.0 2 2 1.0 1.0 1.0 1.0 0 1.5 0 1.5 0 1.5 0 4 -5 -5 -5 -5 4K -5 -5 -5 -5 0.5 0.5 switches ? 1.0 1.0 1.0 1 1 0.5 0.5 0.5 0.5 -5 -5 -5 -5 2 0.5 -100.5 -10 0.5 0 -10 0 -10 0.0 -10 0.0 -10 0.0 -10 0.0 -10 4K0.0 0.0 -10 -5 -100 -55 100 5 10 -10 -5 -100 -55 100 5 10 -10 -5 -100 -55 100 5 10 -10 -5 -100 back-55 100 5 10 -10 0.0 -10 0.0 -10 0.0 -10 0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 horns Half-Wave Plate 4K BS -1 BS BS-1 3 BS BS-1 3 BS 0 BSBS 0 4 BSBS 0 4 BS 1 BSBS 1 5 BSBS 1 5 BS 2 ResultingBS 2 signalResultingBS 2 signal 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 8 8 2.5 2.5 2.5 5 5 2.5 5 2.5 2.5 2.5 2.5 2.5 2.5 2.5 2.5 2.5 2.5 2.5 2.0 5 5 5 5 5 ~60 5cm 5 5 5 5 2.0 5 5 52.0 5 5 5 5 5 5 5 6 6 4 4 2.0 4 2.0 2.0 2.0 2.0 2.0 2.0 2.0 2.0 2.0 2.0 2.0 1.5 1.5 1.5 0 0 0 0 0 3 0 3 1.5 0 03 1.5 0 0 0 1.5 0 0 1.5 0 0 1.5 0 1.5 1.5 0 01.5 1.5 0~40 0 1.5cm 1.5 4 1.5 4 1.0 1.0 1.0 2 2 1.0 2 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 2 2 0.5 0.5 0.5 1 1 0.5 1 0.5 0.5 0.5 0.5 0.5 0.5 0.5 0.5 0.5 0.5 0.5 -10 -10 -10 -10 -10 0 1 horn-10 0 0.0 -10 -10 0 0.01 baseline-10 -10 0.0 -10 0.0 0.01 baseline-10 -10 0.0 0.0 -10 -10 0.0 1 baseline-10 0.0 0.0 -10 -10 0.0 0.0 total-10 -10 signal0.0 0.0 0 0.0 0 -10 -5 -100 -10 -55 -5 -10100 -10 0 -55 -55 100 -10 100 5 -55 10 -100 10 -10 -55 -5 -10100 -10 0 -55 -55 100 -10 100 5 -55 10 -100 10 -10 -55 -5 -10100 -10 0 -55 -55 100 -10 100 5 -55 10 -100 10 -10 -55 -5 -10100 -10 0 -55 -55 100 100 5 5 10 10 4K ~10 cm BS 3 BS 3 BS 3 BS 4 BS 4 BS 4 BS 5 BS 5 BS 5 Resulting signalResulting signal Resulting signal Polarization sensitive 10 10 10 10 10 10 detectors 10 10 10 10 10 Cryostat10 8 8 8 300 mK 2.5 2.5 2.5 2.5 2.5 2.5 2.5 2.5 2.5 5 5 5 5 5 5 5 5 5 5 5 5 6 6 6 2.0 2.0 2.0 2.0 2.0 2.0 2.0 2.0 2.0 0 0 0 1.5 0 1.5 0 1.5 0 1.5 0 1.5 0~701.5 cm0 1.5 0 1.5 0 1.5 0 4 4 4 1.0 Romain Charlassier1.0 - 1.0The QUBIC Collaboration1.0 - 1.0Rencontres 1.0de Moriond on 1.0Cosmology 20101.0 1.0 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 2 2 2 0.5 0.5 0.5 0.5 0.5 0.5 0.5 0.5 0.5 -10 -10 -10 0.0 -10 0.0 -10 0.0 -10 0.0 -10 0.0 -10 0.0 -10 0.0 -10 0.0 -10 0.0 -10 0 0 0 -10 -5 -100 -55 -10100 -55 100 -10 5 -5 10 -100 -55 -10100 -55 100 -10 5 -5 10 -100 -55 -10100 -55 100 -10 5 -5 10 -100 -55 -10100 -55 100 5 10 BS -1 BS -1 BS 0 BS 0 BS 1 BS 1 BS 2 BS 2 10 10 10 10 10 10 10 10 2.5 2.5 BS -1 BS 0 BS 1 BS 2 10 10 10 5 10 5 2.5 2.5 2.5 2.5 2.5 5 5 5 5 2.0 5 2.0 5 5 5 5 2.5 2.5 4 4 2.0 2.0 2.0 2.0 5 5 2.0 5 5 4 2.0 2.0 1.5 1.5 1.5 0 0 3 0 3 0 0 0 1.5 0 1.5 0 1.5 1.5 0 3 0 0 1.5 0 1.5 1.0 1.0 1.0 Dirty2 2 image on the focal 1.0plane1.0 1.0 1.0 2 1.0 1.0 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 -5 0.5 0.5 0.5 1 10.5 1 0.5 0.5 0.5 0.5 0.5 -10 0 -10 0.0-10 -10 -10 00.0 -10 -10 0 -10 0.0 0.0 -10 0.0 -10 0.0 -10 0.0 -10 0.0 0.0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 -100 -55 100 5 10 -10 -5 -100 -55 100 5 10 -10 -5 -100 -55 100 5 10 -10 -5 -100 -55 100 5 10 • Image in focal plane = filtered sky (baselines modes only) BS 3 BS 4 BS 5 Resulting signal 10 10 10 10 8 BS -1 BS BS-1 3 BS BS-1 3 BS 0 BSBS 0 4 BS BS 0 4 = “dirtyBS 1 image”BSBS 1 5 BSBS 1in 5 interferometryBS 2 ResultingBS 2 signalResultingBS 2 signal 2.5 10 10 2.510 10 10 10 2.5 10 10 10 10 10 10 10 10 10 10 10 10 10 10 8 8 2.5 2.5 2.5 5 5 5 5 6