LiteBIRD A Small Satellite for the Studies of B-mode Polarization and Inflation from Cosmic Background Radiation Detection Masashi Hazumi Institute of Particle and Nuclear Studies High Energy Research Accelerator Organization (KEK) Tsukuba, Japan On behalf of the LiteBIRD working group 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 1 My background POLARBEAR - from particle physics to experimental cosmology 2007: KEK CMB Group 2012: Now officially established 2005: my “cosmic survey” à chose CMB ! 1994-2008: B Factory at KEK QUIET Discovered CP violation in B decays à Kobayashi-Maskawa Nobel 2008 KEK CMB group as of 2012 u ~30 members incl. supporting staffs u Two features http://www.nobelprize.org/ u Bringing HEP-based technologies to experimental nobel_prizes/physics/ Cosmology (RF, cryogenics, electronics, computing etc.) u International collaborations 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 2 1. Introduction 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 3 LiteBIRD roadmap POLARBEAR2 LiteBIRD POLARBEAR GroundBIRD Ø Ground-based projects as important steps Ø Verification of key technologies for LiteBIRD Ø Good scientific results Ø International projects QUIET 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 4 POLARBEAR (led by UC Berkeley) Ø 150 GHz TES bolometer array (1274 TESes) w/ 8 MUX Ø Deployment started in Atacama in 2011 Ø First light in Jan 2012 Jupiter 3.5m TauA UC Berkeley, UCSD, KEK, McGill, Austin, Cardiff, Colorado, Dalhousie, Imperial C., LAC, LBNL 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 5 POLARBEAR2 receiver system (led by KEK) 90+150GHz Overview(Focal plane cryostat at the beginning +Optical cryostat) Pulse-tube cooler will add 220GHz later Sorption cooler (3stage: 4He+3He+3He) Antenna- coupled TES array (φ380mm) ADR(for upgrade) Ø Deployment in 2014 (Tbath 250mK à 100mK) Main cryostat at KEK Ø End-to-end demonstrations of Ø Large multi-chroic TES array (7588 TESes) Ø ADR (Tbath = 100mK) Ø Wide-band AR coating Ø Wide-band HWP w/ continuous rotation Ø More information on systematics and foregrounds 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 6 GroundBIRD Ø Cold mirrors Ø Rotary joint Ø Good cryogenic stability MKID Ø Sparse wire grid for TES absolute angle cal. Ø Spinning telescope (20rpm) à atmospheric noise suppression Ø Access to low-l (fsky=30%) Ø Test-bench for LiteBIRD technologies Ø Initial deployment in Japan in 2014, then to Atacama 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 7 • Talks and posters on POLARBEAR, POLARBEAR2 and GroundBIRD will be given at the SPIE conference in Amsterdam next week. • More details and new pieces of information will be shown there. 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 8 How LiteBIRD was started • Suggestions by JAXA people to apply for the small satellite program in 2008 • Ideas for a small satellite to study CMB B-mode – Warm launch (SPICA technology) – Multi-chroic focal plane (Berkeley technology) – Small mirrors • Proposal to form an official working group under JAXA in Sep. 2008 à accepted ! 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 9 LiteBIRD working group JAXA engineers and Mission Design Support Group X-ray astrophysicists CMB experimenters (JAXA) (Berkeley, KEK, McGill) Superconducting sensor Developers (Berkeley, Infrared astronomers RIKEN, NAOJ, Okayama, (JAXA) KEK etc.) v More than 50 members v International and interdisciplinary 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 10 LiteBIRD member list • Y. Takei, H. Fuke, H. Matsuhara, K. Mitsuda, N. Yamazaki, T. Yoshida, S. Sakai （ISAS/JAXA）, • K. Shinozaki, Y. Sato, H. Sugita, K. Yotsumoto, I. Kawano, A. Noda （ARD/JAXA）, • H. Ishino, A. Kibayashi, S. Mima, Y. Mibe (Okayama U.), • A. Ghribi、W. Holzapfel、A. Lee、 H. Nishino、P. Richards、A. Suzuki、(UC Berkeley）, Julian Borrill (LBNL), • I. Ohta(Kinki U.), • M. Yoshida, K. Ishidoshiro, N. Katayama, N. Sato, O. Tajima, Y. Chinone, M. Nagai, R. Nagata, M. Hazumi (PI), K. Hattori, M. Hasegawa, T. Matsumura, H. Morii , N. Kimura, T. Suzuki, T. Tomaru （KEK）, • Y. Inoue, A. Shimizu, H. Watanabe(SOKENDAI), • S. Takada(Tsukuba U.), • E. Komatsu（UT Austin）, • Y. Uzawa, Y. Sekimoto, T. Noguchi（ATC/NAOJ）, • M. Hattori（Tohoku U.）, • M. Dobbs (McGill U.), • K. Natsume, Y. Takagi, S. Nakamura, S. Murayama(Yokohama Nationar U.), • K. Koga, C. Otani (RIKEN) • Supervisors: H. Kodama (KEK), T. Nakagawa (JAXA), R. Kawabe (NAOJ) 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 11 LiteBIRD overview Ø Full success = The total error on r < 0.001 Ø Observing time > 2 years Ø LEO ~500km or L2 Ø Launch in ~2020 with JAXA’s Epsilon (LEO) or H2 (L2) rocket Ø High Energy Physics (HEP) oriented Ø International collaboration from the beginning Ø Three key technologies Ø Multi-chroic focal plane Ø JT/ST/ADR cooling chain Ø Small (~60cm) cold mirrors (4K) 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 12 2. Mission and system 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 13 LiteBIRD mission • Check representative inflationary models • requirement on the uncertainty on r （stat. ⊕ syst. ⊕ foreground ⊕ lensing) δr < 0.001 No lose theorem of LiteBIRD Ø Many inflationary models predict r>0.01 à >10sigma discovery Ø Representative inflationary models (single-large-field slow-roll models) have a lower bound on r, r>0.002, from Lyth relation. Ø no gravitational wave detection at LiteBIRD à exclude representative inflationary models (i.e. r<0.002 @ 95% C.L.) Ø Early indication from ground-based projects à power spectra at LiteBIRD ! Huge impact on cosmology in any case 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 14 Bore sight Spin axis LiteBIRD HWP 2ndary mirror (4K) system Super- conducng Primary Focal mirror overview plane (4K) (100mK) Cryocoolers (JT/ST + ADR) Solar panels Standard bus Beyond COrE workshop Paris Masashi system for 2012/06/25 Hazumi (KEK) JAXA’s small satellites 15 LiteBIRD optics HWP example 4K Reflective Optics Boresight 30cm 2ndary T. Matsumura, HWP doctoral thesis mirror super-conducting bearing wide-band AR (EBEX) Focal Primary plane Focal plane area mirror 30cm Prototype mirrors 50cm 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 16 Major system requirements Item Requirements Remarks Orbit LEO (~500km) or L2 Launch vehicle: Epsilon or H2 Observing time > 2 years Weight < 450kg from Epsilon payload requirement Power < 500W from JAXA’s standard bus system Total sensitivity < 3µKarcmin 2µKarcmin as the design goal Angular resolution < 30arcmin for 150GHz descoping requires justification Observing frequencies 50-270 GHz (or wider) ≥ 4 bands 1/f knee (f) × scan rate (R) R/f > 0.06 rpm/mHz (e.g. spec. for the case HWP stops R>1.2rpm for f=20mHz) Telemetry > 10GB/day w/ Planck-type data suppression Modulation/Demodulation HWP rotation > 1Hz HWP = Half Wave Plate Total systematic errors < 18nK2 on CBB (l=2) These requirements are still subject to modifications in the feasibility studies 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 17 Systems Engineering for LiteBIRD Statistics Systematics δr<0.001 Foreground Lensing 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 18 Focal plane requirement Noise level: goal = 2µK・arcmin To be well below (requirement: < 3µK・arcmin) “lensing floor” 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 19 Foreground removal and observing bands • Foreground removal à ≥4 bands in 50-270GHz N. Katayama and E. Komatsu, ApJ 737, 78 (2011) (arXiv:1101.5210) pixel-based polarized foreground removal （model-independent） very small bias r~0.0006 with 60,100,240GHz (3 bands) 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 20 Expected sensitivity on r Foreground limited Foreground rejection parameter Lensing limited Cosmic variance limited Foreground limited Katayama-Komatsu Cosmic variance limited 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 21 Expected sensitivity on r Foreground limited Foreground rejection parameter Lensing limited Cosmic variance limited Foreground limited Katayama-Komatsu Cosmic variance limited 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 22 LiteBIRD Band We chose the band locations with the following reasons. 1. Katayama-Komatsu (2010) suggested the range of frequency from 50-270 GHz based on the template subtraction. 2. We want to exclude the CO lines. 3. From the practical consideration like AR coating on a POLARBEAR single wafer module lenslet array, it is reasonable to limit the bandwidth to Δν/ ν=1. Above three constraints naturally put CO us to the band locations. J1-0 J2-1 J3-2 Bolometers 100GHz Sinuous antenna Large pixel (Δν/ν=1) Small pixel (Δν/ν=1) 150GHz Δν/ν=0.23 per band Δν/ν=0.3 per band 220GHz 60 78 100 143 190 280 Fabricated Triplexer Filter GHz GHz GHz GHz GHz GHz UC Berkeley TES option 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 23 Sensitivity in foreground bands Recovered r (rin=0.002) Recovered r (rin=0.002) 2 1/(1-α) 1/(1-α)2 - 4 uKarcmin at 100 GHz (CMB channel) - 12 uKarcmin at variable freq (Synch channel2) - 4 uKarcmin at 140 GHz (CMB channel) - 8 uKarcmin at variable freq (Dust channel2) CO J1-0 J2-1 J3-2 Large pixel (Δν/ν=1) Small pixel (Δν/ν=1) Δν/ν=0.23 per band Δν/ν=0.3 per band 60 78 100 140 190 280 GHz GHz GHz GHz GHz GHz 2012/06/25 Beyond COrE workshop Paris Masashi Hazumi (KEK) 24 Focal plane sensitivity Integration time = 2 effective years Tmirror = 4 K No dark bolo is included in the count. Band Pixel size Pixel#/ Bolo#/ Sensitivity # of wafer Sensitivity per band [GHz] [mm] wafer wafer per wafer (total # of [uKarcmin] [uKarcmin] bolo on FP) 60 18 19 38 29 8 10.3 78 18 19 38 18 8 6.4 100 18 19 38 13 8 4.6 Sub total 114 (912) 3.5 140 12 37 74 8.8 5 4.0 190 12 37 74 7.0 5 3.1 280 12 37 74 9.2 5 4.1 Sub total 222 (1110) 2.1 All (2022) 1.8 We limit the total number of detectors as ~2000.