Cosmological inflation and the QUBIC mm-telescope S. Loucatos APC Paris and Irfu CEA- Saclay Polar Bear HEP Democritos Athens 2019 QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 1 INFN, Pisa, March 2nd 2016 2 Radiation emitted at 3000K → cooled by universe expansion to 2.77 K QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 3 INFN, Pisa, March 2nd 2016 Environmet of the detectors < TCMB Thermometers (bolometers) cooled at 100 -300 mK → minimize the thermal noise (phonons) QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 4 INFN, Pisa, March 2nd 2016 Many pixels = imager Planck sky scan QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 5 INFN, Pisa, March 2nd 2016 CMB: Tremendous progress over the last 15 years 1999 2016 Huge success : thousands of independent points fitted with less than 10 parameters and a χ2/ndf about 1 Theoretical curve predicted in 1987 [Bond & Efstathiou] without any data. [Also by Zeldovitch, Sunyaev et al. in 1972 !!!] QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 6 INFN, Pisa, March 2nd 2016 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 7 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 CMB Polarization (~10%) • Generated by Thomson scattering ★ electrons in quadrupolar motion falling into Dark Matter potential wells before decoupling • Stokes Parameters (linear pol.) W. Hu • Scalar E and B fields EE>-modes E< (even) 0 0 B>0 B<0 } (odd) B-modes QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 8 INFN, Pisa, March 2nd 2016 Necessary and sufficient conditions for generating polarisation • You need to have two things to produce linear polarisation 1. Scattering 2. Anisotropic incident light • However, the Universe does not have a preferred direction. How do we generate anisotropic incident light? QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 9 INFN, Pisa, March 2nd 2016 http://background.uchicago.edu/~whu/polar/ webversion/polar.html QUBIC A CMB polarizationJ.-Ch. Hamiltonprimer QU Bolometric Interferometer for Cosmology 10 Wayne Hu,INFN, Martin Pisa, March White 2nd 2016 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 11 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 12 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 13 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 Laser interferometers LIGO and VIRGO detected GW from binary Blackholes and NS, with the wavelength of thousands of kilometres But, the primordial GW affecting the CMB has a wavelength of billions of light-years!! How do we find it? QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 14 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 15 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 16 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 17 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 18 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 Polarisation QUBIC seeks to measure the effect of inflation on the cosmic microwave background. There should be a specific mode of polarization that would be the result of inflation. Image by the BICEP2 instrument. The erroneous result is due to the contribution of the galactic "dust". QUBIC – Steve Torchinsky URSI France – Obs de Versailles, 27 March 2019 19 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 20 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 21 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 22 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 QUBIC E. Komatsu “EuropeanJ.-Ch. Hamilton Coordination of QU Bolometric Interferometer for Cosmology 23 the CMB ProgrammeINFN, Pisa, March”, Florence 2nd 2016 20/9/18 Important Message E. KomatsuE.omatsu • Do not take it for granted if someone told you that detection of the primordial gravitational waves would be a signature of “quantum gravity”! • Only the homogeneous solution corresponds to the vacuum tensor metric perturbation. There is no a priori reason to neglect an inhomogeneous solution! • Contrary, we have several examples in which detectable B-modes are generated by sources [U(1) and SU(2)] QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 24 INFN, Pisa, March 2nd 2016 Density Field Transfer Function Early Universe Acoustic CMB Primordial Density Geometry Oscillations Observations Fluctuations I Q P(k) U Open Closed Flat Fourier mode k • Perturbations evolve from end of inflation to decoupling P(k) Evolved power due to matter-radiation oscillations. spectrum • The transfer function depends upon « simple physics » and cosmological parameters • Allows to fit both cosmology and primordial spectra (including inflationary physics) Fourier mode k QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 25 INFN, Pisa, March 2nd 2016 Planck Planck Results: (ESA Mission) ΛCDM firmly Established Factor 3 improvement w.r.t. WMAP Planck TT spectrum Current step: Inflation Physics through CMB Polarization QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 26 INFN, Pisa, March 2nd 2016 You said ΛCDM firmly established? (Parenthesis: diverging H0 Measurements Riess et al arXiv:1903.07603 Close the parenthesis) QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 27 INFN, Pisa, March 2nd 2016 Scalar and tensor modes - E & B polarization • Scalar perturbations: • Density fluctuations • Temperature • E polarization • No B polarization • Tensor perturbations: t • Specific prediction from inflation! • = Primordial gravitational waves • Temperature • E polarization • B Polarization detecting primordial B-modes: ~ ratio between ⇒ B and E modes ‣ Direct detection of tensor modes ‣ «smoking gun» for inflation ‣ Measurement of its energy scale QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 28 INFN, Pisa, March 2nd 2016 New landscape for B-modes We have entered into the measurement era Before Today Detected signal is Dust + Lensing [Planck+BICEP2] Let’s go deeper & cleaner ! QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 29 INFN, Pisa, March 2nd 2016 Possible instruments P. Timbie • Imagers with bolometers: Imager ★ No doubt they are nice detectors for CMB: Good sensitivity - wide band - low noise ★ Diffraction on external optical elements, ground pickup, Polarization, … may be an issue • Interferometers: ★ Long history in CMB - CMB anisotropies in the late 90s (CAT: 1st detection of subdegree anisotropies, VSA) Good control - CMB polarization 1st detection (DASI, CBI) ofInterferometer systematics ★ Clean systematics: - No telescope (lower ground-pickup & cross-polarization) - Angular resolution set by receivers geometry (well known) ★ Technology used so far - Antennas + HEMTs : higher noise - Correlators : hard to scale to large #channels Can these two devices be combined ? • Both ➡ Bolometric Interferometry QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 30 INFN, Pisa, March 2nd 2016 Primordial B-modes with QUBIC Focal Plane: -17 -1/2 Very weak 2048 TES with NEP ~ 4x10 W.Hz 128:1 SQUIDs+ASIC Mux Readout signal End-To-End Sims. show σ(r)=0.01 with 2 years Cryogenic Optics after HWP and Polarizer + Full power detectors Instrumental Polarization has no effect Instrumental systematics 400 elements Interferometer Synthesized Imaging (well controlled beam) – angular resolution 23.5 arcmin Self-Calibration using switches + active source Two wide bands: 150 and 220 GHz 1 focal plane for each channel Polarized Spectro-Imaging allows to form ≳ 2+3 bands foregrounds Increased Frequency Resolution More Complex dust models can be constrained QUBIC – Steve Torchinsky URSI France – Obs de Versailles, 27 March 2019 31 Collaboration More than 130 6 countries members 22 labs QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology INFN, Pisa, March 2nd 2016 QUBIC concept: Quasi optical correlator Fringes successfuly observed in 2009 with MBI-4 [Timbie et al. 2006] 45 cm Sky Half-wave plate 1K 1 horn open Polarizing grid 1K Primary horns MBI-4 data 1K <1K 2009 campaign (PBO- Cold box Switches 1K Wisc.) 1 baseline Secondary horns 1K 220 GHz bolometer 1 & 2 array (~30x30) 1 baseline Dichroic 1 & 3 <1K 1 baseline 2 & 3 1K total signal 300 mK Cryostat (all baselines)2 & 4 150 GHz bolometer array QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 33 INFN, Pisa, March 2nd 2016 QUBIC Layout 1.547m high 1.42m diameter Outer cryostat: Roma About 800kg 1K Box / detectors: