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 On behalf of the Lite. BIRD working group 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 1
Lite. BIRD project overview n Scientific goal n CMB : Cosmic Microwave Background Stringent tests of cosmic inflation at the extremely early universe n Observations n Full-sky CMB (i. e. mm wave) polarization survey at a degree scale n Strategy n n Focus on signals of inflationary gravitational waves imprinted in CMB polarization Synergy with ground-based super-telescopes n Project status/plans n n 2012/07/03 Working group authorized by SCSS, supported by JAXA Studies toward mission definition review in progress, target launch year ~2020 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 2
Lite. BIRD roadmap POLARBEAR-2 Lite. BIRD POLARBEAR Presentations on these groundbased projects at this conference Ground. BIRD Ø Ground-based projects as important steps Ø Verification of key technologies Ø Good scientific results Ø International projects 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Tomotake Matsumura (Tue. 8452 -124) Aritoki Suzuki (Tue. 8452 -127) Tijmen de Haan (Wed. 8452 -13) Aritoki Suzuki (Wed. 8452 -16) Kenichi Karatsu (Wed. 8452 -25) Zigmund D. Kermish (Fri. 8452 -48) Kam. S. Arnold (Fri. 8452 -49) Takayuki Tomaru (Fri. 8452 -53) Osamu Tajima (Fri. 8452 -58) Amsterdam Masashi Hazumi (KEK) 3
Lite. BIRD working group v More than 50 members KEK Y. Chinone K. Hattori M. Hazumi (PI) M. Hasegawa K. Ishidoshiro* N. Kimura T. Matsumura H. Morii M. Nagai** R. Nagata N. Sato T. Suzuki O. Tajima T. Tomaru M. Yoshida ISAS/JAXA H. Fuke H. Matsuhara K. Mitsuda S. Sakai Y. Takei N. Yamazaki T. Yoshida Tsukuba U. S. Takada Okayama U. H. Ishino A. Kibayashi S. Mima Y. Mibe SOKENDAI Y. Inoue A. Shimizu H. Watanabe 2012/07/03 ARD/JAXA I. Kawano A. Noda Y. Sato K. Shinozaki H. Sugita K. Yotsumoto v International and interdisciplinary UC Berkeley A. Ghribi W. Holzapfel A. Lee (PI) H. Nishino P. Richards A. Suzuki Mc. Gill U. M. Dobbs UT Austin E. Komatsu IPMU N. Katayama Yokohama NU. S. Murayama S. Nakamura K. Natsume Y. Takagi LBNL J. Borrill ATC/NAOJ K. Karatsu T. Noguchi Y. Sekimoto Y. Uzawa RIKEN K. Koga C. Otani Tohoku U. M. Hattori Kinki U. I. Ohta CMB experimenters (Berkeley, KEK, Mc. Gill, Eiichiro) X-ray astrophysicists (JAXA) Infrared astronomers (JAXA) Superconducting Device JAXA engineers and (Berkeley, RIKEN, NAOJ Mission Design Support Group Okayama, KEK etc. ) SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 4
CMB linear polarization map Probing inflation with CMB polarization Ey spectral analyses telescope Ex polarization power spectra 2012/07/03 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 waves, predicted by inflation theories SPIE Astronomical Telescopes and Instrumentation CMB B-mode. Masashi is the most sensitive probe for inflation Amsterdam Hazumi (KEK) 5
CMB polarization power spectra Satellite ! E mode Reionization dozens of degrees Recombination ~2 degrees Ground-based large telescopes, neutrino masses, dark energy (~ current limit) Primordial B mode (not yet detected) Determination of r (tensor-scalar ratio) 2012/07/03 Shed light on inflation energy scale SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 6
Physics of inflation Leading hypothesis = new scalar field “Inflaton” Single-field slow-roll inflation = “standard model Higgs” in cosmology r (tensor-to-scalar ratio) is a key parameter V 1/4 = 1. 06 1016 (r/0. 01)1/4 Ge. V Inflation potential energy proportional to r Unique probe of GUT scale physics ! Current limit Inflationary model predictions (including superstring-motivated phenomenology) 2012/07/03 r > 0. 01 favored SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 7
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 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 8
Systems Engineering for Lite. BIRD Statistics Systemati cs dr<0. 001 Foregroun d 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Lensing Amsterdam Masashi Hazumi (KEK) 9
Bore sight Spin axis HWP Superconducting Focal plane (100 m. K) 2 ndary mirror (4 K) Primary mirror (4 K) Lite. BIRD system overview Cryocoolers (ST/JT + ADR) Solar panels 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) Standard bus system for JAXA’s small satellites 10
Three key technologies to make Lite. BIRD light • Small mirrors (~60 cm) • Warm launch with mechanical coolers • Technology alliance with SPICA for pre-cooling (ST/JT) • Alliance with DIOS (X-ray mission) for ADR Prototype crossed Mizuguchi. Dragone mirror 2 ST/JT BBM • Multi-chroic focal plane Bolometers 100 GHz Sinuous antenna 150 GHz • ~2000 TES (Tbath=100 m. K, dn/n ~ 0. 3), or equivalent MKIDs 220 GHz • Technology demonstration with groundbased projects (POLARBEAR, Fabricated Triplexer POLARBEAR-2, Ground. BIRD) Filter UC Berkeley TES option 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 11
Major system requirements Item Requirements Remarks Orbit LEO (~500 km) or L 2 Launch vehicle: Epsilon or H 2 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 2 m. Karcmin as the design goal Angular resolution < 30 arcmin for 150 GHz descoping requires justification Observing frequencies 50 -270 GHz (or wider) ≥ 4 bands Modulation/Demodulatio n HWP rotation > 1 Hz HWP = Half Wave Plate 1/f knee (f) scan rate (R) R/f > 0. 06 rpm/m. Hz (e. g. spec. for the case HWP stops R>1. 2 rpm for f=20 m. Hz) Telemetry > 10 GB/day w/ Planck-type data These requirements are still subject to modifications in the feasibility studies suppression 2 on SPIE Astronomical Instrumentation 2012/07/03 Total systematic errors Telescopes < 18 n. Kand CBB (l=2) Amsterdam Masashi Hazumi (KEK) 12
y Lite. BIRD scan strategy: LEO case Spin axis x Boresight z Spin axis 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 500 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 ~ 0. 6 rpm 0. 38 Mkm Earth Moon scan uniformity cross link LEO 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Masashi Hazumi (KEK) Amsterdam Uniformity and cross link nearly as good as those at L 2 13
Lite. BIRD optics HWP example 4 K Reflective Optics Crossed Mizuguchi-Dragone Boresight 30 cm HWP (f 30 cm) T. Matsumura, doctoral thesis super-conducting bearing wide-band AR (EBEX) Mirror diameter ~60 cm for ~0. 5°angular resolution (@150 GHz) is sufficient for both reionization and recombination bumps 2012/07/03 Focal plane 2 ndary mirror Primary mirror Prototype mirrors SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 14
Focal plane requirement Noise level: goal = 2 m. K・ arcmin (requirement: < 3 m. K・ arcmin) 2012/07/03 SPIE Astronomical Telescopes and Instrumentation To be well below “lensing floor” Amsterdam Masashi Hazumi (KEK) 15
Foreground removal and 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) 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 16
Lite. BIRD band selection for multi-chroic pixels 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 such as AR coating on a lenslet array, it is reasonable to limit the bandwidth to Δν/ν~1. 50 Above three constraints naturally 320 GHz put us to the band locations. CO Bolometers 100 GHz 150 GHz Sinuous antenna J 1 -0 Large pixel (Δν/ν=1) Δν/ν=0. 23 per band J 2 -1 J 3 -2 Small pixel (Δν/ν=1) Δν/ν=0. 3 per band 220 GHz Fabricated Triplexer Filter UC Berkeley TES option 2012/07/03 SPIE Astronomical Telescopes and Instrumentation 60 GHz 78 100 GHz Amsterdam 143 GHz 190 GHz 280 GHz Masashi Hazumi (KEK) 17
Lite. BIRD focal plane design tri-chroic(140/190/280 GHz) UC Berkeley TES option 2022 TES bolometer s Tbath = 100 m. K. 8 tri-chroic(60/78/100 GHz) 1. 8 m. Karcmin re St POLARBEAR focal plane as a prototype t ra l h 0 io> (w/ 2 effective years) 2 ST/JT BBM 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 18
Lite. BIRD focal plane design tri-chroic(140/190/280 GHz) UC Berkeley TES option 2022 TES bolometer s Tbath = 100 m. K Band centers can be distributed to increase the effective number of bands. 8 tri-chroic(60/78/100 GHz) t ra l h 0 io> re St POLARBEAR focal plane as a prototype 2012/07/03 SPIE Astronomical Telescopes and Instrumentation More space to place <60 GHz Amsterdam Masashi Hazumi detectors (KEK) 19
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) 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 20
MKID option for higher MUX factor NAOJ 300 m. K stage RIKE N 102 pixel MKID Lite. BIRD is currently the guiding force for the MKID development in Japan KEK OKAYAMA Si lens-array Double slot antenna + Al MKID Electrical noise measurement M. Naruse et al. 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 21
Expected sensitivity on r Foreground rejection parameter with 2 effective years Foreground limited Lensing limited Cosmic variance limited Foreground limited Katayama-Komatsu Cosmic variance limited 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 22
L 2 vs. LEO 3 sigma discovery region (statistical error only) LEO L 2 Both cases satisfy the requirement on statistical error 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 23
Advantages of Lite. BIRD • Not a pathfinder; small but no compromise in r sensitivity • More launch options than a big satellite • Less expensive – With Lite. BIRD plus ground-based super-telescopes (e. g. O(100 K) bolometers w/ arcminute angular resolution) as one package, science reach nearly as good as a large CMB polarization mission with ~1/5 total cost • Better in terms of cooling (mirrors and baffles) • The whole spacecraft can be tested in a large cryogenic test chamber – Better calibration data less systematic uncertainties – Better pre-flight investigations less chance of failure 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 24
Conclusion • CMB polarization will be 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 dr<0. 001, for testing all the representative inflationary models. • The strategy of Lite. BIRD is to focus on r measurements. The powerful duo (Lite. BIRD and ground-based super-telescopes) will be the most cost-effective way. • No show-stopper in design studies so far. Technology verification in ground-based projects in next ~3 years will be crucial. The Lite. BIRD roadmap includes such ground-based projects. 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 25
Backup slides 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 26
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 ? 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 27
Search for r>0. 01 well motivated Current limit r > 0. 01 favored Theoretical predictions (including super-string theories in eleven dimensions !) 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Pagano-Cooray-Melchiorri-Kamionkowski 2007 Amsterdam Masashi Hazumi (KEK) 28
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. 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 29
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 e. g. V-band never used on ground 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 30
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 2012/07/03 ~2016 ~2015 ~2014 Bound from Lyth relation (0. 002) ※ statistical and foreground uncertainties taken into account ~2020 ~2014 r present upper limit (95%C. L. ) SPIE Astronomical Telescopes and Instrumentation Amsterdam Competition BICEP 2, KECK(South pole) EBEX, SPIDER(balloon-bourne etc. Both sensitivity and schedule similar to POLARBEAR Masashi Hazumi (KEK) 31
Sub-component status • Optics: – completed a baseline design and fabricated a prototype • Focal plane: – completed a baseline design • Thermal/mechanical design: – preliminary studies made and solutions w/ ~30% margin found • 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 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 32
Sensitivity in foreground bands Recovered r (rin=0. 002) 1/(1 -α)2 - 4 u. Karcmin at 100 GHz (CMB channel) - 12 u. Karcmin at variable freq (Synch channel 2) CO J 1 -0 Large pixel (Δν/ν=1) Δν/ν=0. 23 per band 60 GHz 2012/07/03 78 100 GHz 140 GHz J 2 -1 - 4 u. Karcmin at 140 GHz (CMB channel) - 8 u. Karcmin at variable freq (Dust channel 2) J 3 -2 Small pixel (Δν/ν=1) Δν/ν=0. 3 per band 190 GHz 280 GHz SPIE Astronomical Telescopes and Instrumentation Masashi Hazumi (KEK) Amsterdam 33
Focal plane sensitivity Integration time = 2 effective years Tmirror = 4 K No dark bolo is included in the count. Band [GHz] Pixel size [mm] Pixel#/ wafer Bolo#/ wafer Sensitivity per wafer [u. Karcmin] # of wafer 60 18 19 38 29 8 10. 3 78 18 19 38 18 8 6. 4 100 18 19 38 13 8 4. 6 (912) 3. 5 Sub total 114 (total # of bolo on FP) Sensitivity per band [u. Karcmin] 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 (1110) 2. 1 (2022) 1. 8 Sub total 222 All We limit the total number of detectors as ~2000. The MUX factor of 48 (w/ 2 W/SQUID) will keep the readout power ~100 W. 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 34
Focal plane sensitivity Integration time = 2 effective years Tmirror = 10 K No dark bolo is included in the count. Band [GHz] Pixel size [mm] Pixel#/ wafer Bolo#/ wafer Sensitivity per wafer [u. Karcmin] # of wafer 60 18 19 38 45 8 16. 0 78 18 19 38 27 8 9. 5 100 18 19 38 17 8 6. 0 (912) 4. 8 Sub total 114 (total # of bolo on FP) Sensitivity per band [u. Karcmin] 140 12 37 74 12 5 5. 3 190 12 37 74 9 5 4. 0 280 12 37 74 11 5 4. 5 (1110) 2. 6 (2022) 2. 3 Sub total 222 All We limit the total number of detectors as ~2000. The MUX factor of 48 (w/ 2 W/SQUID) will keep the readout power ~100 W. 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 35
Lite. BIRD thermal design FP 2 -stage Stirling Cooler • Thermal studies on Precoolers (2 ST/JT): 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 2012/07/03 SPIE Astronomical Telescopes and Instrumentation 2 ST/JT BBM Amsterdam Masashi Hazumi (KEK) 36
Expected sensitivity on r Foreground rejection parameter with 2 effective years Foreground limited Lensing limited Cosmic variance limited Foreground limited Katayama-Komatsu Cosmic variance limited 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 37
Delensing with Super. POLARBEAR assumes 6 m. Karcmin for f_sky = 0. 75 (w/ many small patches) 5σ boundary 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 38
Angle miscalibration and fake B-mode power 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 39
Lite. BIRD DAQ・telemetry We need to transfer about 10 GB per day. We assume Planck like data compression (~0. 25) on board. Using the combinations of s- and x-bands, it will take < 1 h for LEO and a few hours for L 2 to downlink the data. requirements on antenna gain 2012/07/03 on-board data compression required, and demonstrated using SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 40
Launch vehicle (1): Epsilon 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 41
SPRINT program SPRINT-A “EXCEED” launch in 2013 With Epsilon rockets**, 2 launches/3 years from 2013. • “Lowering the hurdles to space” • Welcome new challenges Semi-Made-to-Order satellite ** Use of the Epsilon rocket is not the requirement but is assumed unless otherwise proposed. 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 42
Launch vehicle (2): H 2 rockets for medium/large payloads • “ASTRO” series (Suzaku, Akari etc. ) • ASTRO-H (X-ray) in 2014, • SPICA is a candidate for an ASTRO mission. 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 43
Two opportunities • SPRINT series (for science or technology) – Launch vehicle: Epsilon – Currently Lite. BIRD is a candidate among 12 others – So far LEO only • ASTRO series (for science) – Launch vehicle: H 2 A or H 2 B – Most likely together w/ other satellite(s) – Can go to L 2 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 44
Procedure toward launch • MDR proposal in March 2013 – Choose default orbit, launch vehicle, detector technology – Define risks and keep options as part of risk management • Joint work with JAXA’s Mission Design Support Group (MDSG) is ongoing. 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 45
Support by research communities • Japanese High Energy Physics (HEP) community has identified CMB polarization and dark energy survey as two important areas of their “cosmic frontier”. • Japanese radio astronomy community also expressed their support to Lite. BIRD. • Cosmology community (theory) is also supporting Lite. BIRD and contributing to the science case. 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 46
Japanese HEP community’s “The Final Report of the Subcommittee on Future Projects of High Energy Physics” 11 February 2012 An excerpt from the “Recommendations” part Some of the medium/small scale projects currently under consideration have the potential to develop into important research fields like neutrino physics in the future and should be promoted in parallel in pursuit of new physics from various directions. Flavor physics experiments such as muon experiments at the J-PARC, searches for dark matter and neutrinoless double beta decays, observations of CMB B-mode polarization and dark energy are considered as projects that have such potential. 2012/07/03 SPIE Astronomical Telescopes and Instrumentation Amsterdam Masashi Hazumi (KEK) 47
“Cosmic Background Radiation” selected as an “innovative areas for research” by MEXT (our funding agency) • Term: April 2009 – March 2014 • 10 areas selected our of ~200 proposal from all branches of science (except biology/medicine which are treated separately) Lite. BIRD • On-going ground-based projects and Lite. BIRD R&D are supported by this grant. CIB S. Matsuura 5 research (JAXA) groups under Foreground the flag of MKID M. Hattori Lite. BIRD C. Otani (RIKEN) (Tohoku) 2012/07/03 CMB Theory M. Hazumi H. Kodama (KEK) Amsterdam(KEK) SPIE Astronomical Telescopes and Instrumentation Masashi Hazumi (KEK) 48
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