QUBIC: Exploring the primordial Universe with the Q&U Bolometric Interferometer

Transcription

1 QUBIC: Exploring the primordial Universe with the Q&U Bolometric Interferometer Aniello Mennella for the QUBIC collaboration University of Milan, Dept. of Physics INFN-Milan

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

3 Collaboration and funding agencies APC Paris, France CSNSM, France IAS Orsay, France IEF Orsay, France IRAP Toulouse, France LAL Orsay, France Università di Milano Bicocca INFN sezione di Milano Bicocca, Italy Università degli Studi di Milano, Italy INFN sezione di Milano, Italy Università La Sapienza, Roma, Italy INFN sezione di Roma, Italy Università di Tor Vergata, Roma, Italy INFN sezione di Roma2, Roma, Italy Maynooth University, Ireland Cardiff University, UK University of Manchester, UK Brown University, USA Richmond University, USA University of Wisconsin, USA Centro Atómico Constituyentes, Argentina GEMA, Argentina Comision Nacional de Energia Atomica, Argentina Facultad de Ciencias Astronómicas y Geofisicas, Argentina Centro Atómico Bariloche and Istituto Balseiro, Argentina Instituto de Tecnologias en Detección y Astropartículas, Argentina Instituto Argentino de Radioastronomía, Argentina Funding agencies

4 Hidden treasures Planck ESA mission Launched in 2009 Operative until 2013

5 Hidden treasures The CMB carries the imprint of the energy distribution in the primordial universe

6 Spherical harmonics

7 Spherical harmonics

8 ΛCDM universe Dark matter 26.8% Dark energy 68.3%

9 Thomson scattering and polarization Unpolarized e.m. waves The CMB is partially polarized because of Thomson scattering in an anisotropic environment In particular partial polarization is possible only if the CMB possesses a non zero quadrupolar anisotropy What are the mechanisms that generate a quadrupolar moment?

10 Thomson scattering and polarization Unpolarized e.m. waves The CMB is partially polarized because of Thomson scattering in an anisotropic environment In particular partial polarization is possible only if the CMB possesses a non zero quadrupolar anisotropy What are the mechanisms that generate a quadrupolar moment?

11 The effect of density (scalar) perturbations A quadrupolar anisotropy caused by density perturbations generates a so-called E-mode pattern (polarization direction is parallel to crests and perpendicular to troughs)

12 The effect of gravity (tensor) perturbations A quadrupolar anisotropy caused by gravity waves can generate either E-modes or B-modes (in the figure) depending on the orientation of the stretch and squeeze pattern with respect to the line-of-sightparallel to crests and perpendicular to troughs)

13 Inflation and primordial gravity waves The inflationary paradigm predicts the existence of both scalar and tensor perturbations. The amplitude of tensor perturbation is poorly constrained and depends on the assumed potential of the inflaton field

14 Angular power spectra

15 Angular power spectra Total intensity: measured with ultimate precision

16 Angular power spectra Total intensity: measured with ultimate precision E-modes: measured very precisely

17 Angular power spectra Total intensity: measured with ultimate precision E-modes: measured very precisely B-modes: undetected. Level not constrained by inflationary theories

18 Measurements state of the art Total intensity: measured with ultimate precision E-modes: measured very precisely B-modes: current measurements have detected only those caused by gravitational lensing (which act as a systematic effect)

19 Measurements state of the art Measurements require high sensitivity but, especially: Control of instrumental systematic effects Control of astrophysical foregrounds (synchrotron and dust emissions, gravitational lensing) Total intensity: measured with ultimate precision E-modes: measured very precisely B-modes: current measurements have detected only those caused by gravitational lensing (which act as a systematic effect)

20 Worldwide competition 2018 > 2017 Arctic flight + Tenerife ?

21 Worldwide competition 2018 > Simons observatory, , funded (~ 40 M$) + CMB S4, , not funded yet Arctic flight + Tenerife ?

22 Foreground control QUBIC frequencies QUBIC freqs. QUBIC will observe in a small patch of the sky relatively clean of foregrounds Dust contamination will evaluated measuring at two frequencies and exploiting existing data like Planck Planck collaboration et al, 2015, A&A, 594, A10

23 QUBIC in a nutshell the instrument

24 QUBIC in a nutshell the instrument

25 QUBIC in a nutshell the instrument

26 QUBIC in a nutshell the measurement Response to a point source in the far field

27 QUBIC in a nutshell the measurement Response to a point source in the far field

28 QUBIC in a nutshell the measurement Response to a point source in the far field

29 QUBIC in a nutshell the measurement Response to a point source in the far field

30 QUBIC in a nutshell the measurement Response to a point source in the far field Synthetized beam

31 QUBIC in a nutshell the measurement Response to a point source in the far field Signal measured at pixel d p at time t

32 QUBIC in a nutshell the measurement Response to a point source in the far field Signal measured at pixel d p at time t The knowledge of the synthetized beam allows us to use the same data analysis algorithms used for conventional imagers

33 QUBIC in a nutshell self calibration The response from equal baselines is in principle the same

34 QUBIC in a nutshell self calibration The response from equal baselines is in principle the same Self calibration mode: Observe an artificial source Acquire data with several baselines combinations Find instrumental parameters that minimize measurement differences for each baseline

35 QUBIC in a nutshell self calibration r = 10-1 r = 10-2 r = 10-3 Self calibration mode: Observe an artificial source Acquire data with several baselines combinations Find instrumental parameters that minimize measurement differences for each baseline Bigot-Sazy et al, A&A,

36 QUBIC in a nutshell self calibration 10 0 Leakage E B with no self calibration Self calibration mode: r = 10-1 r = 10-2 r = 10-3 Observe an artificial source Acquire data with several baselines combinations Find instrumental parameters that minimize measurement differences for each baseline Bigot-Sazy et al, A&A,

37 QUBIC in a nutshell self calibration s Leakage E B with no self calibration Self calibration mode: 10-2 r = 10-1 Observe an artificial source r = 10-2 Acquire data with several baselines combinations 10-4 r = 10-3 Find instrumental parameters that minimize measurement differences for each baseline Bigot-Sazy et al, A&A,

38 QUBIC in a nutshell self calibration s 10 s Leakage E B with no self calibration Self calibration mode: 10-2 r = 10-1 Observe an artificial source r = 10-2 Acquire data with several baselines combinations 10-4 r = 10-3 Find instrumental parameters that minimize measurement differences for each baseline Bigot-Sazy et al, A&A,

39 QUBIC in a nutshell self calibration s 10 s 100 s Leakage E B with no self calibration Self calibration mode: 10-2 r = 10-1 Observe an artificial source r = 10-2 Acquire data with several baselines combinations 10-4 r = 10-3 Find instrumental parameters that minimize measurement differences for each baseline Bigot-Sazy et al, A&A,

40 QUBIC in a nutshell spectro-imaging The synthetized beam has depends on frequency (in the example the difference between two beams at 140 and 160 GHz) This means that it is possible to reconstruct the frequency information within each band Achievable spectral resolution about 5% Courtesy of J.C. Hamilton

41 QUBIC in a nutshell spectro-imaging 238GHz 220 GHz data 218GHz 201GHz 159 GHz 150 GHz data 148 GHz Courtesy of J.C. Hamilton

42 QUBIC in a nutshell spectro-imaging 220 GHz data 238GHz 218GHz End-to-End Simulation (no systematics) 2 years σ(r)= GHz 159 GHz 150 GHz data 148 GHz Courtesy of J.C. Hamilton

43 QUBIC site ACT, Polarbear, ALMA... QUBIC, LLAMA

44 QUBIC site QUBIC LLAM A

45 QUBIC site quality

46 QUBIC site quality

47 QUBIC site quality With 12-hours per day spent doing self calibration Argentinian site yields a factor ~1.4 reduction in sensitivity compared to Antactica

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49 QUBIC cryostat at Rome La Sapienza (courtesy G. D Alessandro)

50 QUBIC HWP rotator at Rome La Sapienza (courtesy G. D Alessandro)

51 Feedhorn antennas at Milano Statale (courtesy F. Cavaliere)

52 Switches and electronics at Milano Bicocca (courtesy M. Zannoni)

53 He4 fridge at Manchester (courtesy A. May)

54 QUBIC mirrors alignment at Roma La Sapienza (courtesy M. De Petris and M. Zannoni)

55 QUBIC detectors at APC (courtesy S. Marnieros)

56 QUBIC mount development in Argentina (courtesy P. Ringegni and M. Mundo)

57 QUBIC shelter development in Argentina (courtesy R. Ringegni and M. Mundo)

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59 Next steps Autumn 2018 Technological demonstrator calibration in Paris First half of 2019 shipment and installation of Technological demonstrator in Argentina, parallel development of Final Instrument components (detectors, mirrors, switches). Second half of 2019 first light and data taking with Technological Demonstrator, shipment of Final Instrument parts and integration of Final Instrument in Salta Aim at first light with Final Instrument during 2019

60 Conclusions and perspectives CMB B-modes are a challenging quest. Measurements limited by systematic effects and foregrounds QUBIC responds with a challenging instrument with a design that is robust against instrumental effects. The TD will demonstrate the design, the first module will show the scientific potential Long-term plans foresee exploitation of the Argentinean site with deployment several modules with a wide frequency coverage

61 Collaboration and funding agencies APC Paris, France CSNSM, France IAS Orsay, France IEF Orsay, France IRAP Toulouse, France LAL Orsay, France Università di Milano Bicocca INFN sezione di Milano Bicocca, Italy Università degli Studi di Milano, Italy INFN sezione di Milano, Italy Università La Sapienza, Roma, Italy INFN sezione di Roma, Italy Università di Tor Vergata, Roma, Italy INFN sezione di Roma2, Roma, Italy Maynooth University, Ireland Cardiff University, UK University of Manchester, UK Brown University, USA Richmond University, USA University of Wisconsin, USA Centro Atómico Constituyentes, Argentina GEMA, Argentina Comision Nacional de Energia Atomica, Argentina Facultad de Ciencias Astronómicas y Geofisicas, Argentina Centro Atómico Bariloche and Istituto Balseiro, Argentina Instituto de Tecnologias en Detección y Astropartículas, Argentina Instituto Argentino de Radioastronomía, Argentina Funding agencies