Cosmic Inflation and Neutrino Masses at POLARBEAR CMB Polarization Experiment

Transcription

1 KEK Inter-University Research Institute Corporation High Energy Accelerator Research Organization Institute of Particle and Nuclear Studies Cosmic Inflation and Neutrino Masses at POLARBEAR CMB Polarization Experiment WIN2015, June 12, 2015 Masaya Hasegawa (KEK) On behalf of POLARBEAR/ Simons Array Collaboration

2 POLARBEAR Collaboration JAPAN/Oceania KEK/Sokendai IPMU JAXA NIFS PI : Adrian Lee (UC Berkeley) U. Melbourne 1 Europe Imperial College APC SISSA Cardiff Univ Americas 65 UC Berkeley 22 LBNL 5 UC San Diego 21 UC Irvine 1 CU Boulder 3 NASA GSFC 1 Argonne NL 1 Princeton 1 McGill Univ. 4 Catolica 2 Dalhousie 4 8 countries, 20 institutes, ~100 people

3 KEK Outline ν

4 What s POLARBEAR? POLARBEAR is Ground-based CMB Polarization Experiment

5 What s POLARBEAR? POLARBEAR is Ground-based CMB Polarization Experiment Aiming the detection/characterization of B-mode (odd-parity) polarization pattern originating primordial gravitational wave and gravitational lensing effect.

6 What s POLARBEAR? POLARBEAR is Ground-based CMB Polarization Experiment Aiming the detection/characterization of B-mode (odd-parity) polarization pattern originating primordial gravitational wave and gravitational lensing effect. Science targets are Inflation and Neutrino masses!

7 Science with CMB B-mode Thomson Scattering on LSS

8 Science with CMB B-mode Thomson Scattering on LSS E-mode

9 Science with CMB B-mode Gravitational Wave Thomson Scattering on LSS E-mode

10 Science with CMB B-mode Gravitational Wave Thomson Scattering on LSS B-mode E-mode

11 Science with CMB B-mode Inflation Gravitational Wave Thomson Scattering on LSS B-mode E-mode

12 Science with CMB B-mode Inflation Gravitational Wave Thomson Scattering on LSS B-mode E-mode B-mode is a smoking gun signature of inflationary universe!

13 Science with CMB B-mode Inflation Gravitational Wave Thomson Scattering on LSS B-mode E-mode B-mode power is proportional to tensor-to-scalar ratio, r B-mode is a smoking gun signature V 1/4 = ( r ) 1/4 GeV 0.01 of inflationary universe!

14 Science with CMB B-mode Inflation Gravitational Wave Thomson Scattering on LSS x LHC (13TeV) B-mode E-mode 10 5 x GZK cut-off (10 20 ev) à CMB B-mode is a potential window onto the truly-unexplored ultra-high energy phenomenon B-mode power is proportional to tensor-to-scalar ratio, r B-mode is a smoking gun signature V 1/4 = ( r ) 1/4 GeV 0.01 of inflationary universe!

15 Neutrino Mass Neutrino Oscillation Δm 2 atm ~ 10-3 ev 2 Δm 2 sol ~ 10-5 ev 2 à Σm ν > 0.10 (IH) or 0.05eV(NH) Normal hierarchy Inverted hierarchy Oscillation experiments confirmed non-zero neutrino masses, but its absolute scale is still unknown. The region of interest is sub-ev region ev < Σ m ν < ~ 1.3 ev Neutrinos are relativistic at LSS.

16 Neutrino Oscillation Single Δm 2 Beta atm ~ 10 Decay -3 ev 2 Δm 2 sol ~ 10-5 ev 2 Neutrino Mass Probes to sub-ev Neutrino Mass (Particle physics) Effective Mass KATRIN will reach à Σm ν > 0.10 (IH) or 0.05eV(NH) 200meV sensitivity in ~5 years. Normal hierarchy (Cosmology and Astrophysics) Inverted hierarchy Large Scale Structure Oscillation experiments confirmed non-zero neutrino (Particle and Nuclear Physics) masses, but its absolute scale is still unknown. 0-ν Double Beta Decay The region of Majorama interest Mass is sub-ev region. Sensitivity below 100 mev in 5 years 0.05 ev < Σ m ν < ~ 1.3 ev (KamLAND ) With massive neutrinos w/o massive neutrinos Sum of ν Masses Sensitivity below oscillation limit in ~5 years. Neutrinos are relativistic at LSS. Probe Σm ν is complementary to that from particle physics.

17 Neutrino Oscillation Single Δm 2 Beta atm ~ 10 Decay -3 ev 2 Δm 2 sol ~ 10-5 ev 2 Neutrino Mass Probes to sub-ev Neutrino Mass (Particle physics) Effective Mass KATRIN will reach à Σm ν > 0.10 (IH) or 0.05eV(NH) 200meV sensitivity in ~5 years. Normal hierarchy (Cosmology and Astrophysics) Inverted hierarchy Large Scale Structure Oscillation experiments confirmed non-zero neutrino (Particle and Nuclear Physics) masses, but its absolute scale is still unknown. 0-ν Double Beta Decay The region of Majorama interest Mass is sub-ev region. Sensitivity below 100 mev in 5 years 0.05 ev < Σ m ν < ~ 1.3 ev (KamLAND ) With massive neutrinos w/o massive neutrinos Sum of ν Masses Sensitivity below oscillation limit in ~5 years. Neutrinos are relativistic at LSS. Probe Σm ν is complementary to that from particle physics.

18 Lensing B-mode

19 Lensing B-mode Pure E-mode Distorted by gravitational lensing E-mode leaks into B-mode

20 Lensing B-mode Pure E-mode Distorted by gravitational lensing E-mode leaks into B-mode B-mode is the signature of lensing, and good tracer of LSS.

21 ensing B-mode Power 1.8deg. 0.18deg. B-mode power [µk 2 ] Σm ν = 0 ev = 0.05eV = 0.10eV Primordial B-mode Multipole Moment ell = 180/θ (Size of polarization pattern) The lensing B-mode amplitude is sensitive to Σm ν.

22 KEK POLARBEAR Experiment

23 POLARBEAR Site Atacama, Chile (~5200m altitude) Huan Tran Telescope

24 Huan Tran Telescope (HTT) Primary mirror (3.5m) Guard ring CMB Secondary mirror (not seen) Off-axis Gregorian-Dragone 2.5m primary precision machined mirror à FWHM = 3.5 achieved Good enough angular resolution to measure the lensing B-mode signal

25 POLARBEAR-1 Focal Plane 1 cm Lenslet 637 pixels (91 pixels/wafer x 7wafers) 1274 TES bolometers Array sensitivity : 23µK s

26 POLARBEAR-1 Focal Plane 91 pixels (182bolometers) per 1 cm Superconducting Transition Edge Sensor (TES) wafer under AR-coated lenslet. Lenslet * ) =0; JTHU(TES) 637 pixels (91 pixels/wafer x 7wafers) 1274 TES bolometers Polarization is measured PFGSIMQLONERKU (150GHz) Antenna (/>,6 :96,;4C,=498 Dual-polarization Slot /9>-60 <69= /4:960,8=088, ) Antenna by pair-differencingdd Array sensitivity Micro stripbolometers) filter (150GHz) Total: 7 wafers: = 637 pixels ( µK s +,10; 79/>60 MASAYA HASEGAWA * ) =0;< />,6 :96,;4C,=498 /9>-60 <69= /4:960,8=088, KEK

27 POLARBEAR-1 Focal Plane 1 cm Lenslet 637 pixels (91 pixels/wafer x 7wafers) 1274 TES bolometers Array sensitivity : 23µK s

28 Observation Time (hours) Small patch (3deg x 3deg) run for lensing B-mode Large patch (15deg x 15deg) run for lens. & inflation B-mode / / / /06 We started observation in May. 2012, and have collected more than hour data. Released three lensing B-mode results using 1 st season data.

29 Observation Time (hours) Small patch (3deg x 3deg) run for lensing B-mode First-Season data for three B-mode analysis Large patch (15deg x 15deg) run for lens. & inflation B-mode / / / /06 We started observation in May. 2012, and have collected more than hour data. Released three lensing B-mode results using 1 st season data.

30 Observation Time (hours) Small patch (3deg x 3deg) run Large patch (15deg x 15deg) run First season polarization data for lensing B-mode for lens. & inflation B-mode First-Season data for three B-mode analysis Q=EX 2 -EY 2 X Y B U=EA 2 -EB 2 A 4000 Three fields, 24.5 deg 2 total sky area 2000 Map depth : 5.5 µk-arcmin 0 The cosmological polarized signal is 2012/ /07 visible in the 2014/07 map domain. 2015/06 F 5 5 ( ) We started observation in May. 2012, and have collected more than hour data. Released three lensing B-mode results using 1 st season data.

31 First-Season POLARBEAR Results (1) BB Power Spectrum Astrophys. J. 794, 171 A L =1.12±0.61(stat.) (sys.) First measurement of lensing-b mode spectrum. 97.2% rejection of no lensing B-mode Amplitude is consistent with ΛCDM expectation

32 First-Season POLARBEAR Results (2) Lensing deflection power spectrum d d

33 First-Season POLARBEAR Results (2) Lensing deflection power spectrum d d d :deflection field Observed direction POLARBEAR observer True direction

34 First-Season POLARBEAR Results (2) Lensing deflection power spectrum 4.2σ rejection of no lensing B-modes First measurement of polarization lensing with CMB data alone d d PRL 112, (2014). (Editor s suggestion) d :deflection field Observed direction POLARBEAR observer True direction

35 First-Season POLARBEAR Results (2) Lensing deflection power spectrum 4.2σ rejection of no lensing B-modes First measurement of polarization lensing with CMB data alone d d PRL 112, (2014). (Editor s suggestion) (3) Cross correlation with Cosmic Infrared Background d Cosmic Infrared Background Data (Herschel/SPIRE)

36 First-Season POLARBEAR Results (2) Lensing deflection power spectrum 4.2σ rejection of no lensing B-modes First measurement of polarization lensing with CMB data alone d d PRL 112, (2014). (Editor s suggestion) (3) Cross correlation with Cosmic Infrared Background 4.0σ evidence of gravitational lensing of CMB polarization d Cosmic Infrared Background Data PRL 112, (2014). (Editor s suggestion) (Herschel/SPIRE)

37 First-Season POLARBEAR Results (2) Lensing deflection power spectrum 4.2σ rejection of no lensing B-modes First measurement of polarization lensing with CMB data alone PRL 112, (2014). (Editor s suggestion) d d (3) Cross correlation with Cosmic Infrared Background 4.0σ evidence of gravitational lensing of CMB polarization d Cosmic Infrared Background Data PRL 112, (2014). (Editor s suggestion) (Herschel/SPIRE)

38 First-Season POLARBEAR Results (2) Lensing deflection power spectrum 4.2σ rejection of no lensing B-modes First measurement of polarization lensing with CMB data alone PRL 112, (2014). (Editor s suggestion) d d Opening the new era of (3) Cross correlation with Cosmic Infrared Background B-mode cosmology d! 4.0σ evidence of gravitational lensing of CMB polarization Cosmic Infrared Background Data PRL 112, (2014). (Editor s suggestion) (Herschel/SPIRE)

39 Next: POLARBEAR-2 POLARBEAR-2 focal plane POLARBEAR detector array Φ190mm x6 Φ365mm Slot antenna Sinuous antenna (broad band) Larger focal plane (Φ365) 7588 bolometers (~6x increase in mapping speed) Multi-chroic pixels with 95/150GHz frequency coverage. MASAYA HASEGAWA KEK

40 PB2 receiver KEK 250mK focal plane (6x the PB1 bolometers) 1.0m Re-imaging lenses(4k), IR filter(50k) 1.9m The receiver will be shipped to Chile next spring. (Start taking data in early summer next year) MASAYA HASEGAWA KEK

41 Simons Array Simons Array (= 3 x PB2) Ar0st s concep0on Polarbear- 1 Leverage POLARBEAR experience to rapidly increase sensitivity 95/150-22,764 bolometers - Resolution : - frequency bands /150 (95/150/220GHz) - Wide sky survey (f sky =65%) Measurement of B-mode spectrum with unprecedented precision /220

42 Simons Array (projected) sensitivity polarized 95GHz p=15%, fsky=65% r=0.1 polarized 95GHz p=15%, fsky=5% polarized 95GHz p=15%, fsky=65% r= % c.l. upper limit on the foreground residual polarized 95GHz p=15%, fsky=5% Foreground rejection with 95/150/220 GHz, Planck, & C-BASS data Inflation σ(r=0.1) = 6x10-3 (4x10-3 ) Neutrino mass σ(σmν) = 40 mev (19 mev) w/ DESI, BAO Simons array can contribute to cosmology and particle physics significantly.

43 Summary POLARBEAR is a ground-based CMB polarization experiment, aiming to reveal the inflationary universe and neutrino absolute mass scale. POLARBEAR-1 : the first measurement of lensing B-mode signal at 4.7σ with CMB data alone, and successfully laid the groundwork for neutrino mass measurement. POLARBEAR-2/Simons Array is being prepared. Stay Tuned!