Lite BIRD A Small Satellite for the Studies
Lite. BIRD 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 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 1
Ø Observing time > 2 years Ø LEO (or L 2) Ø Launch in ~2020 with JAXA’s
Lite. BIRD working group o An official working group for JAXA’s small satellite projects o Established in Sep. 2008, Pre-Phase A studies ongoing • • • • Y. Takei, H. Fuke, H. Matsuhara, K. Mitsuda, N. Yamazaki, T. Yoshida, S. Sakai (ISAS/JAXA), ASTRO-H, SPICA, DIOS, Balloon development K. Shinozaki, Y. Sato, H. Sugita, K. Yotsumoto, I. Kawano, A. Noda (ARD/JAXA), H. Ishino, A. Kibayashi, S. Mima, Y. Mibe (Okayama U. ), Adnan Ghribi、William Holzapfel、Adrian Lee、 Haruki Nishino、Paul Richards、Aritoki Suzuki、(UC Berkeley), POLARBEAR, EBEX, APEX, EPIC, BICEP, SPTPol Julian Borrill (LBNL), Planck 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), QUIET, POLARBEAR (Planck, BICEP, EBEX), Y. Inoue, A. Shimizu, H. Watanabe(SOKENDAI), S. Takada(Tsukuba U. ), E. Komatsu(UT Austin), WMAP Y. Uzawa, Y. Sekimoto, T. Noguchi(ATC/NAOJ), M. Hattori(Tohoku U. ), M. Dobbs (Mc. Gill U. ), APEX, SPT, EBEX, POLARBEAR, SPTpol 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) More than 50 members from CMB projects, as well as from X-ray and infrared astrophysics projects, and from THz community 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 3
Lite. BIRD roadmap POLARBEAR-2 Lite. BIRD POLARBEAR Ground. BIRD Ground-based projects as important steps Ø Verification of key technologies for Lite. BIRD Ø Good scientific results 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 4
Science 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 5
Cosmic inflation • An accelerating expansion at the very early universe. • The leading hypothesis to answer one of the grand questions in cosmology “what powered the big bang ? ” • We can probe the inflationary universe with CMB polarization ! (indeed inflation is the earliest period we can probe with cuttingedge technology) • Underlying quantum gravity theory, which is not yet understood, can also be tested by probing the inflationary universe. So, how does it work ? 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 6
CMB linear polarization map Probing inflation with CMB polarization Ey spectral analyses telescope Ex polarization power spectra 2012/04/04 W. Hu et al. astro-ph/0210096 • Ex 2 – Ey 2 • Ex. Ey E-mode pola arra rimete r y B-mode Smoking-gun signal of primordial gravitational wave, predicted by inflation theories CMB B-mode sensitive probe for inflation ISSTT 2012 Tokyo is the Masashimost Hazumi (KEK) 7
CMB polarization power spectra Satellite ! E mode Reionization Recombination Ground-based large telescopes, neutrino masses, dark energy (~ current limit) Primordial B mode (not yet detected) Determination of r (tensor-scalar ratio) 2012/04/04 Shed light on inflation energy scale 8 ISSTT 2012 Tokyo Masashi Hazumi (KEK)
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 V 1/4 = 1. 06 1016 (r/0. 01)1/4 Ge. V Unique probe of GUT scale physics ! 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 9
Search for r>0. 01 well motivated Current limit r > 0. 01 favored Theoretical predictions (including super-string theories in eleven dimensions !) 2012/04/04 ISSTT 2012 Pagano-Cooray-Melchiorri-Kamionkowski 2007 Tokyo Masashi Hazumi (KEK) 10
Lite. BIRD mission • Check representative inflationary models • requirement on the uncertainty on r (stat. ⊕ syst. ⊕ foreground ⊕ lensing) dr < 0. 001 No lose theorem of Lite. BIRD Ø Many inflationary models predict r>0. 01 >10 sigma 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 Lite. BIRD exclude representative inflationary models (i. e. r<0. 002 @ 95% C. L. ) Ø Early indication from ground-based projects power spectra at Lite. BIRD ! Huge impact on cosmology in any case 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 11
System 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 12
Bore sight Spin axis 2 ndary mirror (4 K) HWP Superconducting Focal plane (100 m. K) Primary mirror (4 K) Lite. BIRD system overview Cryocoolers (JT/ST + ADR) Solar panels 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) Standard bus system for JAXA’s small satellites 13
Major system requirements Item Requirements Remarks Orbit LEO (~500 km) or L 2 Epsilon or H 2 under consideration Observing time > 2 years Weight < 450 kg from Epsilon payload requirement Power < 500 W from JAXA’s standard bus system Total sensitivity < 3 m. Karcmin Angular resolution < 30 arcmin for 150 GHz Observing frequencies 50 -270 GHz (or wider) ≥ 4 bands 1/f knee (f) scan rate (R) R/f > 0. 06 rpm/m. Hz e. g. R>1. 2 rpm for f=20 m. Hz These requirements> may be modified in the feasibility studies Telemetry 10 GB/day w/ Planck-type data suppression Modulation/Demodulatio HWP rotation. Tokyo > 1 Hz ISSTT 2012/04/04 HWP = Half Masashi Hazumi (KEK)Wave Plate 14
Focal plane requirement Noise level: goal = 2 m. K・arcmin (requirement: < 3 m. K・arcmin) 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) To be well below “lensing floor” 15
Lite. BIRD observing bands • Foreground removal ≥ 4 bands in 50 -270 GHz N. Katayama and E. Komatsu, Ap. J 737, 78 (2011) (ar. Xiv: 1101. 5210) pixel-based polarized foreground removal (model-independent) very small bias r~0. 0006 with 60, 100, 240 GHz (3 bands) 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 16
Lite. BIRD focal plane design UC Berkeley TES option tri-chroic(95/150/240 GHz) Bolometers 100 GHz 150 GHz Sinuous antenna 220 GHz di-chroic(60/95 GHz) Fabricated Triplexer Filter Tbath = 100 m. K 2 bands/pixel 3 bands/pixel For more information 2012/04/04 § Aritoki Suzuki’s talk (this session) on multi-chroic TES development, § Tomotake Matsumura’s poster (P-48) on focal plane design and sensitivity ISSTT 2012 Tokyo Masashi Hazumi (KEK) 17
TES signal multiplexing Frequency-domain multiplexing (MUX) used in POLARBEAR, SPT, EBEX etc. (8 -16 MUX) toward Lite. BIRD Frequency-domain multiplexing Replace analog feedback loop with Digital Active Nulling (DAN) to achieve 64 MUX Berkeley-KEK-Mc. Gill-NIST led by Mc. Gill University (supported by CSA) 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 18
MKID option for higher MUX factor NAOJ • Talks in this session – by Ken’ichi Karatsu RIKEN – by Kensuke Koga • Posters KEK OKAYAMA – P-49 by Hiroki Watanabe – P-50 by Yoshiaki Kibe – P-52 by Masato Naruse 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 19
sfg (foreground rejection parameter) L 2 vs. LEO 3 sigma discovery region O E L L 2 case Katayama-Komatsu 2011 Both cases satisfy the requirement on statistical error 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 20
Development in ground-based projects 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 21
Lite. BIRD roadmap POLARBEAR-2 Lite. BIRD POLARBEAR Ground. BIRD Ground-based projects as important steps Ø Verification of key technologies for Lite. BIRD Ø Good scientific results 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 22
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 ! 3. 5 m 2012/04/04 Jupiter ISSTT 2012 Tokyo UC Berkeley, UCSD, KEK, Mc. Gill, Austin, Cardiff, Colorado, Dalhousie Imperial C. , LAC, LBNL Masashi Hazumi (KEK) 23
IEEE Transactions on THz science and technology 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 24
Yes he does Paul on POLARBEAR 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 25
POLARBEAR-2 receiver system Overview(Focal plane cryostat +Optical cryostat) (led by KEK) Pulse-tube cooler Sorption cooler (3 stage: 4 He+3 He) Antennacoupled TES array (f 380 mm) ADR(for upgrade) Ø Deployment in 2014 (Tbath = 250 m. K 100 m. K) Main cryostat at KEK Ø End-to-end demonstrations of Ø Large multi-chroic TES array (7588 TESes) Ø ADR (Tbath = 100 m. K) Ø Wide-band AR coating Ø Wide-band HWP w/ continuous rotation Ø More information on systematics and foregrounds 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 26
Ground. BIRD See Poster P-51 by Osamu Tajima for details “Satellite on the ground” 30% sky coverage from Atacama, Chile MKID TES Ø Low-l (l down to ~6) w/ better sensitivity than Planck Ø Test-bench for Lite. BIRD detector technologies Ø Initial deployment in Japan in 2014, then to Atacama 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 27
Discussions and summary 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 28
Why observation in space ? • Whole-sky survey required for reionization bump – lensing is subdominant even at r = 0. 001 • No atmospheric noise • No constraint in frequency band selection (except CO lines) – Important to remove foregrounds 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 29
Why small satellite ? 10 1 3 sigma discovery ~0. 5°angular resolution (@150 GHz) is sufficient region Mirror diameter ~60 cm does the job D IR Lite. B Ø Much less expensive Ø More launch options than a big satellite Ø Better in terms of mirror cooling Ø No compromise on r measurements Ø Ground-based telescopes for supporting measurements 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 30
Three key technologies to make Lite. BIRD light • Small mirrors (~60 cm) • Warm launch with mechanical coolers • Technology alliance with SPICA (JAXA technology) for pre-cooling (JT/Starling) • Alliance with DIOS (X-ray mission) for ADR • Multi-chroic focal plane • ~2000 TES (Tbath=100 m. K, dn/n ~ 0. 3), or equivalent MKIDs • Technology demonstration with ground-based projects (POLARBEAR-2, Ground. BIRD) 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 31
Take-home message • Current limit r~0. 2 • POLARBEAR-2 r~0. 01 • Lite. BIRD r~0. 001 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 32
Conclusion • CMB polarization is the frontier in post-Planck era – Best probe to discover primordial gravitational waves – Unique tests of inflation and quantum gravity • The goal of Lite. BIRD is to search for primordial gravitational waves with the sensitivity of r~0. 001, for testing all the representative inflationary models. • Focal plane technology is a key to the success. Technology verification in ground-based projects in next ~5 years will be crucial. Very exciting period and big challenge ahead of u 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 33
Backup slides 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 34
Major contribution to S/N ratio Foreground limited Lensing limited Cosmic variance limited Foreground limited Cosmic variance limited 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 35
Lite. BIRD optics HWP example 4 K Reflective Optics Boresight 30 cm HWP T. Matsumura, doctoral thesis Focal plane area 30 cm Primary mirror Prototype mirrors 50 cm 2012/04/04 Focal plane 2 ndary mirror ISSTT 2012 Tokyo Masashi Hazumi (KEK) 36
Lite. BIRD thermal design FP 2 -stage Stirling Cooler • Thermal studies on Precoolers (JT/ST) A solution w/reasonable margin (28. 8%) • Structure analysis was also OK • 3 -stage ADR (32 kg): Leak B-field is small enough: less than 0. 5 Gauss for > 100 mm from ADR 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 37
Lite. BIRD DAQ・telemetry data rate on-board data suppression required, and demonstrated using FPGAs requirements on antenna gain low-power options exist 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 38
y Lite. BIRD scan strategy x Spin axis Boresight z Spin axis 3 rpm Boresight = 34 degs : relative angle betw/n moon and boresight (60 degs) Anti-sun Satellite 6000 K = 76 degs 175 K Anti-sun 300 K altitude 600 km 150 Mkm Sun Earth - Spin axis rotation about anti-sun axis (i. e. satellite period around the earth) fs = 90 min - Boresight axis rotation about spin axis fb ~ 1 min 0. 38 Mkm Earth Moon scan uniformity cross link LEO 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 39
Discovery potential(>3 s)and model predictions 5 4 3 2 1 Single-field slow-roll w/ ns-r relations Power-law Chaotic p=8 SSB (Ne = 47 -62) Chaotic p=0. 1 String theory examples 1. N-flation, 2. Axion Monodromy, 3. Monodromy 4. Fiber inflation, 5. Warped D-brane, Kahler, Racetrack, . . Pagano-Cooray-Melchiorri. Kamionkowski 2008 Baumann, ar. Xiv: 0907. 5424 ~2016 ~2015 ~2014 Bound from Lyth relation (0. 002) ~2014 r ※ statistical and foreground uncertainties taken into account 2012/04/04 ~2020 ISSTT 2012 Competition BICEP 2, KECK(South pole) EBEX, SPIDER(balloon-bou etc. present upper limit Both sensitivity and schedule similar to POLARBEAR (95%C. L. ) Tokyo Masashi Hazumi (KEK) 40
Scientific Shopping List • Primordial gravitational wave (low-l B mode) – inflation model selection Cosmology and Fundamental physics – Tests of quantum gravity, even string theories ! • Lensing(high-l)B-mode precision measurements – neutrino mass, gravitinos etc. – (early) dark energy Bonus: Cross correlations w/ other frequencies • Beyond the Standard Model – parity violation in gravity (non-zero CEB etc. ) Astronomy • Cosmic reionization science (low l) • Foreground science Rich and important science from CMB ISSTT 2012 Tokyo Masashi Hazumi (KEK) 2012/04/04 polarization 41
Projects in the world 1. Ground 2. Balloon ACTPol 3. Satellite SPIDER QUIET POLARBEAR In addition, ABS, CLAS, . . . Atacama, Chile Planck EBEX PIPER SPTPol In addition, POLAR, . . . 2012/04/04 WMAP (obs. end in 2010) S-E L2 South Pole ISSTT 2012 Tokyo Masashi Hazumi (KEK) 42
Comparison with laser interferometer - my personal comment u CMB polarization is much more sensitive than interferometry. u 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. 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 43
Systems Engineering for Lite. BIRD Systemati cs Statistics dr<0. 001 Foregroun d 2012/04/04 ISSTT 2012 Lensing Tokyo Masashi Hazumi (KEK) 44
Sub-component status • Optics: – completed a baseline design and fabricated a prototype • Focal plane: – completed a baseline design • Thermal/mechanical design: – preliminary studies and found solutions w/ ~30% margin • Orbit/attitude control: – choose <1 rpm (requiring HWP) for feasibility studies • Telemetry: – requirements for L 2/LEO obtained, • Foreground studies: – dr=0. 0006 w/ 3 or more bands in 50 -270 GHz • Systematics: – Studying requirements to make a systematic error budget 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 45
KEK CMB Members (2007~ ) Various “previous lives” including Belle, Super. K, BESS, gravitational wave detection, sub-mm astronomy, theory. Also getting strong support from cryogenics center, electronics system group and machine shop at KEK. In total ~30 members 2012/04/04 ISSTT 2012 Tokyo Masashi Hazumi (KEK) 46
KEK CMB Group History • Nov. 2007:Established, joined QUIET Low frequencies • Jun. 2008:Joined POLARBEAR • Sep. 2008:Proposed Lite. BIRD, WG accepted by JAXA QUIET • Mar. 2009:CMB session established at JPS • Apr. 2009:MEXT Grant-in-Aid started (http: //cbr. kek. jp/) High frequencies • Oct. 2010:JSPS Brain Circulation program started • Dec. 2010:Initial results from QUIET • Apr. 2011: CMB B-mode and dark energy selected as two most POLARBEAR important cosmic connections by HEP community in Japan Ultimate • Aug. 2011: Official support on Lite. BIRD from Japanese radio astronomy community • Sep. 2011:POLARBEAR deployment in Chile started 2012/04/04 ISSTT 2012 Tokyo observations Lite. BIRD Masashi Hazumi (KEK) 47
- Slides: 47