The LiteBIRD Satellite Project Masashi Hazumi (KEK CMB Group) 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 1 Lite (Light) Satellite for the Studies of B-mode Polarization LiteBIRD and Inflation from Cosmic Background Radiation Detection n JAXA-based working group (more than 60 members from JAXA, Kavli IPMU, KEK, NAOJ, Berkeley/LBNL, McGill, Riken, MPA and Japanese universities) n Scientific objectives n Tests of cosmic inflation and quantum gravity theories n Full success: δr < 0.001 (stat. ⊕ syst. ⊕ foreground ⊕ lensing) n δr is the total error on tensor-to-scalar ratio n Observations n Full-sky CMB polarization survey at a degree scale (30arcmin @ 150 GHz) n 6 bands b/w 50 and 320 GHz n Strategy v Continuously-rotating n Part of technology verification from ground-based projects HWP w/ 30cm diameter v 60cm Primary Mirror n Synergy with ground-based super-telescopes w/ Cross-Dragone config. n Synergy with X-ray mission R&D v 100mK Focal Plane w/ Multi-chroic n Project status/plan Superconducting n Selected as one of eight most important future projects by Detector Array v JT/ST + ADR astronomy/astrophysics division of w/ Heritages Science Council of Japan of X-ray Missions n Recognized as one of key future JAXA missions in fundamental physics n Target launch year ~2020 LEO ~ 600km 2013/08/30 The CMB and theories of the primordial(L2 universe,as an option) Kyoto University, Japan, Masashi Hazumi (KEK) 2 LiteBIRD working group v 67 members (as of June. 1, 2013) v International and interdisciplinary KEK JAXA UC Berkeley MPA ATC/NAOJ RIKEN Y. Chinone H. Fuke A. Ghribi E. Komatsu K. Karatsu K. Koga K. Hattori I. Kawano W. Holzapfel T. Noguchi S. Mima M. Hazumi (PI) H. Matsuhara A. Lee (US PI) IPMU Y. Sekimoto C. Otani M. Hasegawa K. Mitsuda P. Richards N. Katayama Y. Uzawa K. Kimura T. Nishibori A. Suzuki H. Nishino Tohoku U. N. Kimura A. Noda Saitama U. M. Hattori McGill U. Yokohama NU. M. Naruse K. Ishidoshiro T. Matsumura S. Sakai S. Murayama H. Morii Y. Sato M. Dobbs K. Morishima S. Nakamura Osaka Pref. U. R. Nagata K. Shinozaki LBNL K. Natsume H. Ogawa Kinki U. S. Oguri H. Sugita J. Borrill I. Ohta N. Sato Y. Takei T. Suzuki T. Wada Tsukuba U. CMB experimenters O. Tajima N. Yamasaki M. Nagai (Berkeley, KEK, McGill, Eiichiro) T. Tomaru T. Yoshida M. Yoshida K. Yotsumoto X-ray astrophysicists (JAXA) SOKENDAI Okayama U. Y. Akiba H. Ishino Infrared astronomers Y. Inoue A. Kibayashi H. Ishitsuka Y. Kibe (JAXA) A. Shimizu Superconducting Device H. Watanabe National Inst. for Fusion JAXA engineers, Mission Design (Berkeley, RIKEN, NAOJ, Osaka U. Science Support Group, SE office Okayama, KEK etc.) S. Takakura S. Takada 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 3 Outline 1. Introduction 2. Pre LiteBIRD Era 3. LiteBIRD Era 4. Post-LiteBIRD Era 5. Conclusion 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 4 1. Introduction 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 5 CMB polarization projects 1. Ground 3. Satellite 2. Balloon ACTPol WMAP EBEX (obs. end QUIET in 2010) Planck POLARBEAR Atacama, SPIDER In addition, Chile ABS, CLASS, POLARBEAR-2, GroundBIRD, Simons Array, MuSE, … LSPE PIXIE COrE SPTPol LiteBIRD South EPIC Pole (CMBpol) In addition, BICEP3, POLAR, QUBIC, … PIPER PRISM In addition, QUIJOTE in Canary island, AMiBA in Hawaii 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 6 Why so exciting ? Experimental cosmologists dream of • Discovery of Primordial Gravitational Waves (PGW) ! • Determination of energy scale of inflation ! • Experimental quantum gravity ! Measuring CMB polarization is the only neat thing to do ! 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 7 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 8 CMB polarization power spectra Satellite ! E mode Reionization dozens of degrees Ground-based Recombination large telescopes, ~2 degrees neutrino masses, dark energy Primordial B mode (not yet detected) Determination of r (tensor-scalar ratio) Shed light on inflation energy scale 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 9 Physics of inflation Leading hypothesis = new scalar field “Inflaton” In case of single-field slow-roll inflation (= so-to-speak “standard model Higgs” in cosmology) r (tensor-to-scalar ratio) is a key parameter Inflation potential proportional to r V1/4 = 1.06 × 1016 × (r/0.01)1/4 GeV Unique probe of GUT scale physics ! 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 10 Current limit on r from CMB temperature r < 0.11 (95% C.L.) Cosmic variance limited à Hope is in polarization measurements. 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 11 Pagano-Cooray-Melchiorri-Kamionkowski 2007 Current measurement Predictions (95%C.L.) on r Current upper limit (95%C.L.) Large-field inflation (Δφ > MPl） Lower limit from Lyth relation Small-field inflation s (Δφ < MPl） • Targeting r=0.01 is well motivated. • Targeting r=0.001 is needed to fully test large-field models. 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 12 2. Pre-LiteBIRD Era 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 13 Current Status of polarization measurements E-mode • Observed • Consistent with ΛCDM B-mode • Not observed yet • Best limit on r from B-mode is r < 0.7 (95%C.L.) by BICEP (3yr data, preliminary) 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 14 CMB Polarization Data in the Can • BICEP-2/Keck Array • Planck • POLARBEAR-1 • SPTpol These experiments will • ABS publish results in the • QUIJOTE near future with sensitivity • EBEX at r~0.1 or even better. 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 15 Four obstacles Statistics Systematics Goal δr < 0.01 Foreground Lensing 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 16 International collaboration including KEK, Kavli IPMU, POLARBEAR UCSD, UC Berkeley from Asia Pacific regions POLARBEAR-1 project led by UC Berkeley • Search for inflationary B-modes Primary mirror to r=0.025 (95%C.L.) and detect gravitational lensing B-modes POLARBEAR Site: Atacama, • 3.5m primary mirror and Chile large focal plane with (5150m 1274 TES bolometers above Secondary sea level) • First light in Chile in mirror (not seen) Jan. 2012 and large amount of data already recorded Receiver system • Roadmap: – 7588 TESes in 2014 (POLARBEAR-2) • r<0.01 (95%C.L.) – >22000 TESes in 2016(Simons Array) 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 17 POLARBEAR Site: Atacama, Chile Overview (5150m above sea level) 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 18 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 19 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 20 1 cm POLARBEAR-1 Focal Plane Lenslet TES 637 pixels (91 pixels/wafer x 7 wafers) 1274 TES bolometers 21 µK√s array NET Wafer module (achieved typically assembly 2 TES bolometers/pixel with dual-polarization during observations) double-slot dipole antenna 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 21 Observation ( 36 hour cycle) Dec=90 Synchrotron Dust Intensity map (FDS) RA=-180 RA=0 3 patches w/ small dust components 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 22 Systematic Error Mitigation Beam effect forecast Suppression Differential gain with sky rotation Diff Ellipticity Suppression w/ stepped HWP Diff Pointing Diff Rotation • Sky rotation is effective • Small-enough beams Diff Beam Width à peak in leakage at high-l • Comoving shields against sidelobes • Evaluation w/ data in progress 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 23 POLARBEAR-1 (First year of data) 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 24 POLARBEAR-2 (led by KEK) 150GHz micro-strip filter Al-Ti Bolometer Sinuous-antenna developed at UC Berkeley Focal Plane Detector 95GHz micro-strip filter 4K stage 300mK stage • 7588 TES bolometers • 95GHz and 150GHz broadband 365mm AR coated 2K stage lenslet • r<0.01 @ 95%C.L. 400mK stage • σ(Σmv)=65meV (w/ Planck) 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 25 Solutions • Cryogenic • Gaussian beam Detector Statistics Systematics • Modulation Array • Calibrations Goal δr < 0.01 • Multi-band • Clean patches • Delensing Foreground Lensing • Large sky 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 26 How to reach r=0.001 ? Statistics Systematics δr < 0.001 Foreground Lensing 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 27 Satellite(s) ! • All sky à at low l, lensing is subdominant even at r=0.001 • No atmospheric fluctuation • No limitation in observing frequency • Long observing time 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 28 End of ground-based CMB projects in ~5 years ? No ! 2013/08/30 The CMB and theories of the primordial universe, Kyoto University, Japan, Masashi Hazumi (KEK) 29 CMB polarization with large telescopes (l>500 + Planck) • Sum of neutrino masses to ~0.05ev – Hierarchy may be understood • Constrain other new particles (e.g.