The QUBIC Experiment

Home , POLARBEAR, Qubic experiment, Spider (polarimeter)

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

~10 cm 4K

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 2.0 2.0 2.0 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 5 5 5 5 5 2.0 5 5 52.0 5 5 5 5 5 5 5 6 6 0 1.5 0 1.5 0 1.5 0 4 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

1.0 1.0 1.0 1.5 1.5 1.5

-5 -5 -5 -5 2 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 0 1.5 1.5 4 1.5 4 0.5 0.5 0.5 1.0 1.0 1.0 -10 0.0 -10 0.0 -10 2 2 1.00.0 -10 2 1.0 0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 5 10 -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 10.0 baseline-10 -10 0.0 -10 0.0 10.0 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

BS 3 BS 3 BS 3 BS 4 BS 4 BS 4 BS 5 BS 5 BS 5 Resulting signalResulting signal Resulting signal Each pixel/bolometer measures a linear combination of all 10 • 10 10 10 8 10 10 10 10 10 10 10 10 8 8

visibilities2.5 2.5 with2.5 different2.5 2.5 coefﬁcients2.5 2.5 (controlled2.5 2.5 or geometrical 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

phase shifts)

0 0 0 1.5 0 1.5 0 1.5 0 1.5 0 1.5 0 1.5 0 1.5 0 1.5 0 1.5 0 4 4 4

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 2 2 2 Observables0.5 0.5 0.5 in 0.5interferometry0.5 0.5 =0.5 Visibilities0.5 0.5 (modes of sky FT)

• Invert the linear system to get the visibilities... [Charlassier et al., arxiv:0806.0380, A&A 497 (2009) 963] [Hyland et al., arXiv :0808.2403v1, MNRAS 393 (2009) 531]

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 Statistical sensitivity comparison with imagers 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

Nh=576 - FWHMIm= 1.00 - FWHMHI= 14.0 - FWHMBI= 14.0 BS 3 BS 4 1.2BS 5 Resulting signal

10 10 10 Direct10 Imager / Heterodyne Interferometer8 Sensitivity to B-mode ? 2.5 2.5 2.5 Direct Imager / QUBIC 1.0 ✓ 5 5 5 5 Direct Imager / QUBIC6 2.0 2.0 2.0 2.0 1.0 Noise only 0 1.5 0 1.5 0 1.5 0 Sample variance 4 included Factor 2-3 penalty in 1/2 1.0 1.0 1.0 NETIm = 200 µK/Hz -5 -5 -5 -5 2 1/2 0.5 0.5 0.5 NETBI = 200 µK/Hz NET = 346 µK/Hz1/2 stat. sensivity (only) HI -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 0.8 [Hamilton et al., arxiv:0807.0438, A&A 491-3 (2008)] (updated with Bandwidth, accurate NET calculations 0.6 and others... + QUBIC discussions)

0.4

Error ratio on PS : Imager / Interferometer ✓ Bandwidth ? (OK, 1.6 0.2 sensitivity penalty only!) κ = 1.344 Bandwidth = 25% [Charlassier et al., arxiv:0910.1864, A&A in press (2010)] 0.0 20 40 60 80 100 120 140 l multipole

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 Technological1.0 1.0 developments in QUBIC -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

10 10 10 • Polarization-sensitive10 8 detectors in focal plane:

2.5 2.5 2.5 5 5 5 5 6 2.0 2.0 2.0 - Filled array + polarized grid

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 - Antenna-coupled array

-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

- KIDS array • Modulation of polarization + systematic control: - Rotating Half-Wave Plate + switches - Controlled phase shifters

R&D going on inside QUBIC, choices will be soon made

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 Systematics1.5 0 1.5 control/removal with

1.0 2 1.0 1.0 -5 -5 -5 -5 0.5 1 redundant0.5 0.5 baselines: a preview -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 Primary feedhorns 5 5 5 5 6 2.0 2.0 2.0 looking at the sky 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

Two redundant baselines Two different baselines

• Calibration mode: switch off all the horns but 2 • Ideal instrument: all redundant visibilities equal • Real instrument: slight differences allowing the instrument calibration

[Work in progress...]

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 The QUBIC program 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

• BRAIN Pathﬁnder 2007 BS 3 BS 4 BS 5 Resulting signal

10 10 10 • Site testing,10 logistics 8 2.5 2.5 2.5 5 5 5 • Atmosphere5 characterization6 at Dome C 2.0 2.0 2.0 2008

(effective temperature, polarization ...) 0 1.5 0 1.5 0 1.5 0 4

1.0 1.0 • 1.0 3 campaigns, January 2006, 2007 and 2010 MBI-4 -5 -5 -5 -5 2 0.5 0.5 0.5 BRAIN -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 Pathﬁnder 2009

• MBI-4 Prototype • 4 horns bolometric interferometer • works in Wisconsin (2008 and 2009) 2010 • Fringes observed ! 2011 • QUBIC • Search for primordial B-modes (50 < l < 150) • Bolometric interferometer QUBIC 2012 • 2x3 modules 144/256/512 horns (90,150, 220GHz) ﬁrst module • 25% Bandwidth • Full instrument in 2013... at Dome C 2013 • Target : r ~ 0.01 in 1 year of data QUBIC full size

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 Dôme C : best site on Earth for 0 3 0 0 1.5 0 1.5

1.0 2 1.0 1.0 -5 -5 -5 -5 0.5 1 0.5Astronomy0.5 ? -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

Low PWV level hence low Tatm...

BS 3 BS 4 BS 5 Resulting signal (increasing integration time by at least a factor 2 10 10 10 10 8

2.5 2.5 2.5 5 5 5 5 6 by comparison with Chajnantor...) 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

BRAIN Pathﬁnder: Jan. 2010 data being analysed

Latitude : 75 deg Height : 3220 m asl Pressure : 645 hPa Summer : -30 C Winter : -60 C 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 MBI-4 @ Pine Bluff 1.0 2 IT1.0 WORKS!1.0 -5 -5 -5 -5 Observatory in Wisconsin 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 • MBI-4,2.5 Bolometric interferometer 5 5 5 5 6 2.0 2.0 2.0

0 1.5 0 1.5 0 prototype 1.5 0 : 90GHz, 4 4 horns, 16 spiderweb

1.0 1.0 1.0 -5 -5 -5 -5 2 0.5 0.5 bolometers,0.5 330mK 3He cryostat

-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

• Fringes observed as expected...

DATA SIMULATION

Preliminary results

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 The1.0 QUBIC1.0 Experiment - Summary -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

10 10 10 10 8

2.5 2.5 Targeting2.5 primordial B-modes 5 5 5 • 5 6 2.0 2.0 2.0

0 1.5 0 1.5 0 (l~100)1.5 0 @ r~0.01 4 for 2013

1.0 1.0 1.0 -5 -5 -5 -5 2 0.5 0.5 0.5

-10 0.0 -10 0.0 -10 Collaboration0.0 -10 0 between Europe & USA (only post- -10 -5 0 5 10 -10 -5 0 5 10 -10 -5 0 •5 10 -10 -5 0 5 10

Planck European project) • A novel technology: deep study of concept & sensitivity already + exp. validation • Several technological possibilities (choices will be made soon) • A uniq way to handle/remove systematics • details/references on www.qubic.org

Romain Charlassier - The QUBIC Collaboration - Rencontres de Moriond on Cosmology 2010