LiteBIRD. Masashi Hazumi (KEK/ Kavli IPMU, Japan)
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1 LiteBIRD Lite (Light) Satellite for the Studies of B-mode Polarization and Inflation from Cosmic Background Radiation Detection Masashi Hazumi (KEK/ Kavli IPMU, Japan) 6th KIAS workshop on Cosmology and Structure Formation Nov. 3, 2014
2 LiteBIRD working group >70 members, internayonal and interdisciplinary. KEK Y. Chinone K. HaRori M. Hazumi (PI) M. Hasegawa Y. Hori N. Kimura H. Morii R. Nagata S. Oguri N. Sato T. Suzuki O. Tajima T. Tomaru H. Yamaguchi M. Yoshida Sokendai Y. Akiba Y. Inoue H. Ishitsuka Y. Segawa H. Watanabe Osaka Univ. S. Takakura 2014/11/3 JAXA H. Fuke I. Kawano H. Matsuhara T. Matsumura K. Mitsuda T. Nishibori K. Nishijo A. Noda S. Sakai Y. Sato K. Shinozaki H. Sugita Y. Takei T. Wada N. Yamasaki T. Yoshida K. Yotsumoto Okayama Univ. K. Ishino A. Kibayashi Y. Kibe Y. Yamada UC Berkeley W. Holzapfel A. Lee (US PI) P. Richards A. Suzuki McGill U. M. Dobbs LBNL J. Borrill Univ. of Tsukuba M. Nagai Korean participation anticipated (Prof. Eunil Won at Korea Univ.) Kavli IPMU N. Katayama H. Nishino MPA E. Komatsu Tohoku Univ. K. Ishidoshiro M. HaRori T. Morishima Yokohama Natl. Univ. K. Mizukami S. Nakamura K. Natsume Konan Univ. I. Ohta Osaka Pref. Univ. H. Ogawa K. Kimura M. Kozu N. Okada M. Inoue X-ray astrophysics (JAXA) Saitama Univ. M. Naruse NAOJ K. Karatsu T. Noguchi Y. Sekimoto NICT Y. Uzawa RIKEN K. Koga S. Mima C. Otani NIFS S. Takada CMB exp. (Berkeley, KEK, McGill, Eiichiro) IR astronomy (JAXA) JAXA engineering SE Mission Design Support Group 6th KIAS workshop on Cosmology and Structure Formation Superconductivity detector (Berkeley, Okayama, KEK, NAOJ, Riken etc.) Masashi Hazumi (KEK) 2
3 LiteBIRD Overview 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 3
4 LiteBIRD Overview n Candidate for JAXA s future missions on fundamental physics n Mission: Search for / characterize primordial gravitational waves n Method: Full-sky CMB polarization survey at degree angular scales n Full success: δr < (δr: total error on tensor-to-scalar ratio) Major Specifications n Orbit: L2 n Weight: ~1300kg n Power: ~2000W n Observing time: > 3 years n Spin rate: ~0.1rpm Cryogenics n JT/ST and ADR (Astro-H heritage) Optics n Continuously-rotating half-wave plate n Reflective mirrors w/ Cross-Dragone configuration at 4K n 30arcmin at 150GHz Detector n 100mK focal plane w/ multi-chroic superconducting detector array n 6 bands b/w 50 and 320 GHz 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 4
5 LiteBIRD Overview Prototype Mizuguchi-Dragone mirror 2ST/JT BBM Cryogenics Optics TES or MKID Detector Scan strategy like a spinning top w/ precession 2014/11/3 POLARBEAR as proof-of-principle experiment 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 5
6 Launch Vehicle H3 will be ready in 2020 ½ cost w/ same capability (comparison w/ H-II B) LiteBIRD s target launch year = /11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 6
7 Probing cosmic inflation with CMB polarization Primordial gravitational waves CMB CMB B-mode :curl patterns as fingerprints of inflation First stars Foregrounds Beginning of our universe Galaxy formation Reionization Dark Ages Recombination Hot Big Bang Inflation Cosmic age 10-38sec? yr 13.8Gyr CMB B-mode is the best probe for primordial gravitational waves 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 7
8 BICEP2 (2014) 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 8
9 B mode power spectra now arcmin Tensor-scalar ratio r (primordial signal) Gravitational lensing B mode POLARBEAR BICEP2 (2014 March 2014 March arxiv: arxiv: ApJ, 794, 171 (2014) PRL 112 (2014) ) 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 9
10 Planck 353 GHz (arxiv: ) Assumption in BICEP2 analysis is likely to be optimistic. 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 10
11 Foregrounds vs. CMB Polarization intensity CMB Observing frequency 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 11
12 LiteBIRD foreground subtraction exercise using a template method with 6 bands We apply the template method to the Planck sky model (Dust polarization fraction is set to be 3) using the 6 bands, and test the recovery of tensor-to-scalar ratio, r. Use l <47 and f sky of 50%. Method II: Δ-template with uniform β distribution Method II : Δ-template with a prior in β distribution Method III: iterative Δ-template r recover Planck CMB polarization data will be released in Nov and we will revisit this optimization with Planck data. r in Katayama et al. in prep. 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 12
13 LiteBIRD focal plane example tri-chroic(140/195/280ghz) 2022 TES bolometers T bath = 100mK UC Berkeley TES option tri-chroic(60/78/100ghz) Band centers can be distributed to increase the effective number of bands Spectra Polarization 95 GHz GHz More space to place <60GHz detectors 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 13
14 LiteBIRD expected precision If the inflationary signal (r) is large, LiteBIRD will determine the inflationary B-mode power spectra. If r is small, search for the inflationary B-mode down to δr < /11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 14
15 Stat. error NET 2x10-18 W/ Hz # sensors 2000 δr~0.4x10-3 Katayama-Komatsu 2011 foreground δr<0.001 Lensing δr~0.5x10-3 (stat error +lensing) requirement: < 0.57x10-3 Syst. error 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 15
16 Expected sensitivity on r Foreground residual with 2 effective years Foreground limited Lensing limited R. Nagata Cosmic variance limited Foreground limited Katayama -Komatsu Cosmic variance limited 2014/05/29 Seminar at Tohoku University Masashi Hazumi (KEK) 16
17 Why targeting δr < 0.001? - Bound from Lyth relation Many models predict r>0.01 à >10σ discovery. What if we do not see the signal? Single large-field models that satisfy slow-roll conditions give 2 60 r ' N m pl 2 Lyth relation Establishing a bound r < (95%C.L.) has a significant impact on primordial cosmology. More model-dependent studies come to the same conclusion (Note that this is conceptually different from the usual Lyth bound that gives an upper limit on Δφ when you see the primordial gravitational waves) 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 17
18 Why in space? Clear limitation on ground Frequency bands are limited à foreground rejection capability is limited Atmosphere is nuisance. Not only giving additional noise but may produce polarized signals at the level we want to reach. Hard to access the whole sky All the issues above do not exist in space. 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 18
19 Strategy Synergy X Satellite for ultimate meas. of r (δr<0.001) 2 < l < 200 Telescope arrays on ground 40 < l < 3000 e.g. Simons Array, Stage-4 Powerful Duo 2014/10/23 KEK-PH 2014 Masashi Hazumi (KEK) 19
20 Figure by K. Kohri 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 20
21 Simons Array goal (ground-based large telescopes) Figure by K. Kohri LiteBIRD goal 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 21
22 Physics of CMB B-mode GUT-scale physics V 1/4 = r /4 [GeV] Arguably the first observation of quantum fluctuation of space-time! 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 22
23 Other scientific topics Tensor tilt (n t ): δn t ~ 0.03 (@r=0.2) Other non-standard cosmology with BB, EB, EE Tests of superstring theory (e.g. non-zero C l EB ) Power spectra deviation from standard cosmology Loop quantum gravity Primordial magnetic field Cosmic strings Isocurvature Non Gaussianity Astronomy Reionization w/ cosmic-variance-limited EE meas. Galactic magnetic field Galactic haze emission from foreground studies 2014/05/29 Seminar at Tohoku University Masashi Hazumi (KEK) 23
24 Schedule and Project Status Working group phase MDR SRR Pre-project SDR Project Prototype model Flight model Launch Observations LiteBIRD is selected as one of the top-priority projects in Master Plan 2014 by Science Council of Japan. LiteBIRD is chosen as one of ten new projects in MEXT Roadmap for Large-scale Research Projects. 2014/11/3 6th KIAS workshop on Cosmology and Structure Formation Masashi Hazumi (KEK) 24
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