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Search for B-modes in CMB Polarization - QUIET and other experiments

Ultimate High Energy Physics. Search for B-modes in CMB Polarization - QUIET and other experiments. QUIET collaboration photo Jun. 2009 at Fermilab. Osamu Tajima (KEK) The QUIET Collaboration. Today. History of the high energy physics  Looking at early universe. reheating

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Search for B-modes in CMB Polarization - QUIET and other experiments

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  1. Ultimate High Energy Physics Search for B-modes in CMB Polarization- QUIET and other experiments QUIET collaboration photo Jun. 2009 at Fermilab Osamu Tajima (KEK) The QUIET Collaboration

  2. Today History of the high energy physics  Looking at early universe reheating (Big-Bang) Inflation LHC : ~10 TeV Observation of Inflationary Epoch Ultimate Theory ? 1016 Very Exiting Experiment !! Inflation potential : Parameterized with “ r “ : tensor-scalar ratio (T/S) 10~16GeVUltimate HEP !!

  3. Today Primordial Gravitational Waves (PGW) Inflation Ultimate Theory ? Accelerated expansion of space creates PGW 1016

  4. Two approaches for PGW observation B-modes in CMB Polarization PGW Cosmic gravitational wave Inflation Today (13.7 Billion yr) 10-34 sec 380K yr ( last scattering surface ) • CMB polarization is much more sensitive. • Discovery (on ground or in space) of PGW from CMB polarization will give a specific target for future gravitational wave detection experiments. a very strong science case can be made. B-modes “fingerprints” of PGW Interferometer LISA (space) LIGO (ground)

  5. No PGW, E-modes only At the early stage of universe, radiations (photons) were scattered by free electrons E-modes (even parity) Anisotropy of universe  Parity even polarization pattern

  6. With PGW, B-modes and E-modes B-modes: Smoking gun signal of PGW B-modes (odd parity) E-modes (even parity)

  7. Since B-modes are pattern in CMB polarization, experimental approach is; Measure CMB polarization “map” on the sky E-modes B-modes

  8. Since B-modes are pattern in CMB polarization, experimental approach is; Measure CMB polarization “map” on the sky Characterize them in Fourier space 2 deg. 0.2 deg. ~20deg. E-modes Spherical harmonics (like 2-D Fourier Transformation) B-modes A few tens of degrees region are sufficient for B-modes search  observation from the ground Multipolel (=180o/q)

  9. Experimental results at present Currently, ground base experiments lead this competition Because they can use cutting edge polarization detector arrays E-modes QUIET aims to detect B-modes from ground ! Smoking gun signal of PGW B-modes （U.L. ９５％CL） Direct bound r < 0.7 (BICEP) Regions favored by many inflationary modelsr = 0.01 ~ 0.1

  10. The QUIET Collaboration 5 countries, 14 institutes, ~35 scientists QUIET collaboration photo Jun. 2009 at Fermilab

  11. The QUIET Collaboration 5 countries, 14 institutes, ~35 scientists QUIET-1 observation: Oct. 2008 – Dec. 2010 at Atacama, Chile (5,080m) CMB patch scan

  12. Observation Patches Visible region along earth rotation ~20o 4 CMB patches were chosen (~3% of full sky) Observing them DEEPLY (Galaxy observation when CMB patches are not visible) Map precision on 1°x1°: ~1μK (7.5 months at 43GHz)

  13. CMB QUIET Telescope CMB QUIET polarization detector 90 detectors array at 95 GHz Receiver ( detector array inside) Digital Camera Telephoto Lens ~30cm

  14. Large number of detectors “Detector Array” is essential for all CMB-pol. experiments Limitation of single detector sensitivity More detectors  smaller statistical error, i.e. better sensitivity Several hundreds ~ thousand detectors are necessary to cover inflationary model favored region: r ~ 0.01  QUIET-1 is intermediated phase to proof of technology QUIET-1 (2008-2010) 95 GHz detector CAPMAP (2003-2005) Pol. detector at 95GHz QUIET-1 (2008-2010) 90 detectors array at 95 GHz 1/10 size 3cm ~30cm ~30cm

  15. QUIET-1 observation at Atacama, Chile 5,080m ~30cm ~30cm > 11,000 H 19 detectors at 43GHz array sensitivity 69uKs1/2 90 detectors at 95GHz array sensitivity ~70uKs1/2 7.5 months 1.5 years

  16. [arXiv:1012.3191] Good Achievement for Calibration ~4 min scan time for each Taurus Crab nebula (TauA) Tpol = 5mK Q Q by Y. Chinone Polarization signal hieht TQ(U) cos(2(q-g)) Dgabsolute = 1.7° (at 43GHz) U Rotate parallactic angle with keeping the line of sight QUIET telescope θ

  17. QUIET Polarization Map for Galactic Center • Detector • Calibration • Low-level analysis QUIET Stokes, U Stokes, Q WMAP (5-year)

  18. [arXiv:1012.3191] QUIET CMB Polarization Map Point sources are masked in analysis

  19. [arXiv:1012.3191] E-modes • Detector • Calibration • Low-level analysis • High-level analysis Strong proof of instrument and analysis Significant power is detected at 1st , 2nd peak region Consistent with LCDM model QUIET / LCDM = 0.87 ± 0.10 PTE from LCDM 14% for EE + BB + EB

  20. [arXiv:1012.3191] B-modes : r < 2.2 @95%CL(zero-consistent : r=0.35+1.06-0.87) Second best upper limits whereas short observation time Limits from QUIET 43GHz (7.5 months ~1/3 of BICEP-1 data) Expected limits with 95GHz data Predictions from major inflationary models Expected Limits in QUIET-2 w/ 500 detectors ( = 180o/q） 19 detectors QUIET 2 500 detectors 90 detectors

  21. Ground-based telescopes QUIET 1 (2008－2010) QUIET 2 (201x－) POLARBEAR (2011－) They are also going to implement several hundreds ~ thousand detectors SPT SPTPol Chile, Atacama (~5,000m) (2010-) (2011-) チリ Not shown here are ABS, ACTPol, (Atacama) Polar (South Pole) South Pole (2,800m) Image: S. Richter

  22. Balloon-borne telescopes Satellite Telescopes ~2020 - COrE LiteBIRD Planck (2009-) EPIC SPIDER（2011, 2012） EBEX （2009-2011） PIPER（2013-） Not optimized for polarization meas.

  23. B-modes Search in Future QUIET-1 initial data set at 43GHz Predictions from major models QUIET-1 full data set Sensitivity of Future Experiments e.g. QUIET-2 All coming experiments claim good sensitivity r = O(0.01) or better sensitivity with several hundreds to thousand detectors ( = 180o/q） The most important subject for future: Good systematic error control

  24. [arXiv:1012.3191] QUIET-1 initial results at 43GHzLeast systematic error to date I  Q/U Leakage (fake pol.signal): < 1% Possible Angle Uncertainty: 1.7o Possible residual contamination B-modes:r= 0.1 (Inflationary models favor r = 0.01~0.10) Extensive study of systematic errors • Strong proof of our technology for future • Good prospects for further syst. error reduction • We improved 95GHz instruments and calibrations

  25. Summary • “B-modes” in CMB polarization is smoking gun signature of inflationary universe • Ultimate High Energy Physics: 10~16GeV • Many experiments are going on, search limits are improved almost year-by-year • It is very exciting period now • Experimental technique is still in its infancy • Especially, systematic error control • QUIET-1 initial results achieved least systematic error to date [arXiv:1012.3191] e.g. fake polarization signal: < 1% • Many rooms for contribution by new comers from different fields, e.g. particle physicists

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