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: APC, CSNSM / IRAP Fridges: Manchester Optics: Roma / Maynooth / Cardiff
Currently cold and under test at APC
QUBIC – Steve Torchinsky URSI France – Obs de Versailles, 27 March 2019 34 QUBIC Main Features
• TES Focal planes High Sensitivity -17 -1/2 r < 0.01 @ 95%C.L.(No ★ 2048 TES with NEP ~ 4x10 W.Hz foregrounds) r < 0.02 @ ★ 128:1 SQUIDs+ASIC Mux Readout 95%C.L.(inc. foregrounds)
• 400 Elements Bolometric Interf. Synthesized imager ★ Synthesized imaging on focal planes scanning the sky ★ 23.5 arcmin FWHM Perfect beam control
• Dual Band operations Dust Polarisation ★ One focal plane for each band contamination ★ 150 and 220 GHz removal
• Switches on each horn ★ Ability to reconstruct baselines individually Unprecedented ★ Self-Calibration like an interferometer control of systematics with Self-Calibration
QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 35 INFN, Pisa, March 2nd 2016 TES Detector Array
TES fabrication: CSNSM Readout electronics: APC & IRAP
QUBIC – Steve Torchinsky URSI France – Obs de Versailles, 27 March 2019 36 Detection chain • Focal plane: ★ TD: 2x256 NbSi TESs (CSNSM, IEF) ★ Support structure and readout (APC)
4 février 2016 CMB prospective: QUBIC instrument QUBIC J.-Ch. Hamilton 37 QU Bolometric Interferometer for Cosmology 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 38 INFN, Pisa, March 2nd 2016 Cryostat and cryogenics
• Cryogenic system ★ 2x1W pulse tubes (Roma Sapienza) ★ 40K-4K and 4K-1K heat switches (Manchester) ★ 1K adsorption fridge (Manchester) ★ 300mK adsorption fridges (Manchester)
4 février 2016 CMB prospective: QUBIC instrument QUBIC J.-Ch. Hamilton 39 QU Bolometric Interferometer for Cosmology INFN, Pisa, March 2nd 2016 Mount • Alt-az mount • Boresight rotation: +/- 15° • In a warm environment (à la BICEP2)
4 février 2016 CMB prospective: QUBIC instrument QUBIC J.-Ch. Hamilton 40 QU Bolometric Interferometer for Cosmology INFN, Pisa, March 2nd 2016 telecon MDP - April 5th, 2019ForeBaffle completed in Argentina
41 QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology INFN, Pisa, March 2nd 2016 telecon MDP - April 5th, 2019 GroundShield under construction in Argentina: almost completed
42 QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology INFN, Pisa, March 2nd 2016 QUBIC Site: near San Antonio de los Cobres (Salta, Argentina) Vulcano Tuzgle
QUBIC LLAMA
Road Gazoduct + Optical 51 fiber
5000m a.s.l. Logistics + mount : Argentina Access road built, works started on site and in Salta city (integration hall)
QUBIC – Steve Torchinsky URSI France – Obs de Versailles, 27 March 2019 43 Site Construction well advanced (ready by June 2019)
Integration Hall in Salta New road to QUBIC site
Internet link QUBIC site
QUBIC – Steve Torchinsky URSI France – Obs de Versailles, 27 March 2019 44 San Antonio de los Cobres (3775m a.s.l. - 5000 habitants)
45 QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 46 INFN, Pisa, March 2nd 2016 Bolometric Interferometry
Primary horn array Synthesized beam (on the sky)
150-220 GHz, 20x20 horns, Synthesized beam used to scan 13 deg. FWHM, D=1.2 cm the sky as with an imager
QUBIC – Steve Torchinsky URSI France – Obs de Versailles, 27 March 2019 47 QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 48 INFN, Pisa, March 2nd 2016 Synthesized Beam
NB: Synthesized beam predicted in 2011. See Battistelli et al. 2011 Fig. 5
QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology 49 INFN, Pisa, March 2nd 2016 Profile of a point source on a reconstructed map
1st replication: 23.5 arcmin nothing remains FWHM in map !
QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology INFN, Pisa, March 2nd 2016 Spectro Imaging Synthesized beam: Depends on horns configuration AND on frequency ! - ex: a point source emitting at 140 and 160 GHz There is spatial + frequency information ! Multi-frequency map-making with the same TOD Spectral resolution Δν/ν~0.05 Shown to be quasi-optimal with simulations article being finalized
QUBIC – Steve Torchinsky URSI France – Obs de Versailles, 27 March 2019 51 QUBIC Spectro Imaging 238GHz End-to-End Simulation (no systematics) 2 years 218GHz σ(r)=0.01
TOD(220 GHz)
201GHz
159 GHz
TOD(150 GHz) 148 GHz
=> Increased Spectral Resolution Sky: => Dust subtraction Infinite Instrument: Data Analysis: => More complex models can be constrained bands 2 wide bands 5 narrow bands
QUBIC – Steve Torchinsky URSI France – Obs de Versailles, 27 March 2019 52 Systematics: Self-Calibration • Unique possibility to handle systematic errors Use horn array redundancy to calibrate systematics - In a perfect instrument redundant baselines should see the same signal - Differences due to systematics - Allow to fit systematics with an external source on the field Unique specificity of Bolometric Interferometry [Bigot-Sazy et al., A&A 2012, arXiv:1209.4905] Redundant baselines : same Example: exact horns locations (figure exagerated !!) Fourier Mode
Nominal Real Real Recovered
Real - Recovered
Nominal - Real
Actual horn positions (red) are not well know Actual horn positions (red) are recovered Horns positions (mm) One uses ideal ones (blue) in map reconstruction thanks to self calibration (green) Horn position knowledge improvement ⇒ Systematics in maps, E/B leakage ⇒ E/B leakage is reduced
QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology INFN, Pisa, March 2nd 2016 QUBIC in a worldwide perspective Project Lead Location Status Frequencies Ang. Science goals Res. No foregrounds With Foregrounds QUBIC 1st module France Antarctica / 2020 150, 220 Low r = 0.01 (95%CL) r=0.02 (95%CL) Argentina ? BICEP/Keck U.S.A Antarctica Running 95, 150, 220 Low r = 0.01 - ABS U.S.A. Chile Running 150 Low Technological (HWP) CLASS U.S.A. Chile 40, 90, 150, 220 Low r = 0.02 - SPTpol U.S.A. Antarctica Running 95 High Lensing (neutrinos) + r (but l > ~300) ACTpol U.S.A. Chile Running 100, 150 High Lensing (neutrinos) + r (but l > ~300) PolarBear U.S.A. Chile Running 95, 150, 220 High Lensing (neutrinos) + r (but l > ~300) LSPE Italy Arctic > 2019 43, 90, 95, 145, 245 Low r = 0.03 - EBEX U.S.A. Antarctica 150, 250, 410 Med. r = 0.01 + lensing PIPER U.S.A. Multiple 200, 270, 350, 600 Med. r = 0.01 + lensing SPIDER2015 U.S.A. Antarctica Early2020 2015 95, 150 (220 later) Low 2025r = 0.01 - Stage III Stage IV Space r ~ 0.01 r ~ 0.001 Mission ? Many separate projects Many instruments in Synergy International Collaboration Technological exploration Distributed over good sites ESA / NASA / JAXA ? Advanced QUBIC as a Stage IV Instrument ?
QUBIC J.-Ch. Hamilton QU Bolometric Interferometer for Cosmology INFN, Pisa, March 2nd 2016 Summary QUBIC is a novel instrumental concept First Bolometric Interferometer Dedicated to CMB polarimetry and inflationary physics High sensitivity with ~2000 TES bolometers Optimized to handle systematics: - Self Calibration allowed by observing individual fringe patterns (Unique to QUBIC) Spectro-Imaging with two physical bands (150 / 220 GHz) and 5-10 sub- bands: - Foregrounds contamination control and removal with up to 10 bands (unique to QUBIC) Target : - First module (150-220 GHz): σ(r)=0.01 (incl. dust) - Stage IV evolution of QUBIC σ(r)=0.01 hopefully through a wider European collaboration + CMB-S4 tube(s) QUBIC deployment is on the way: TD Integration and test ongoing at APC Initial Calibration measurements in the lab First light in Argentina end-2019 Upgrade to Full focal plane in 2020
QUBIC – Steve Torchinsky URSI France – Obs de Versailles, 27 March 2019 55