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DECIGO and B-DECIGO Masaki Ando (Univ. of Tokyo / NAOJ) On behalf of - PowerPoint PPT Presentation

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Science and Design of DECIGO and B-DECIGO Masaki Ando (Univ. of Tokyo / NAOJ) On behalf of DECIGO Working Group Credit: S.Sato The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan) DECIGO Members Masaki Ando,

  1. Science and Design of DECIGO and B-DECIGO Masaki Ando (Univ. of Tokyo / NAOJ) On behalf of DECIGO Working Group Credit: S.Sato The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  2. DECIGO Members Masaki Ando, Seiji Kawamura, Naoki Seto, Takashi Nakamura, Kimio Tsubono, Shuichi Sato, Takahiro Tanaka, Ikkoh Funaki, Kenji Numata, Nobuyuki Kanda, Kunihito Ioka, Takeshi Takashima, Jun'ichi Yokoyama, Tomotada Akutsu, Mitsuru Musha, Akitoshi Ueda, Koh-suke Aoyanagi, Kazuhiro Agatsuma, Hideki Asada, Yoichi Aso, Koji Arai, Akito Araya, Takeshi Ikegami, Takehiko Ishikawa, Hideharu Ishizaki, Hideki Ishihara, Kiwamu Izumi, Kiyotomo Ichiki, Hiroyuki Ito, Yousuke Itoh, Kaiki T. Inoue, Ken-ichi Ueda, Takafumi Ushiba, Masayoshi Utashima, Satoshi Eguchi, Yumiko Ejiri, Motohiro Enoki, Toshikazu Ebisuzaki, Yoshiharu Eriguchi, Naoko Ohishi, Masashi Ohkawa, Masatake Ohashi, Kenichi Oohara, Yoshiyuki Obuchi, Kenshi Okada, Norio Okada, Koki Okutomi, Nobuki Kawashima, Fumiko Kawazoe, Isao Kawano, Kenta Kiuchi, Naoko Kishimoto, Hitoshi Kuninaka, Hiroo Kunimori, Kazuaki Kuroda, Sachiko Kuroyanagi, Hiroyuki Koizumi, Feng-Lei Hong, Kazunori Kohri, Wataru Kokuyama, Keiko Kokeyama, Yoshihide Kozai, Yasufumi Kojima, Kei Kotake, Shiho Kobayashi, Rina Gondo, Motoyuki Saijo, Ryo Saito, Shin-ichiro Sakai, Masaaki Sakagami, Shihori Sakata, Norichika Sago, Misao Sasaki, Takashi Sato, Masaru Shibata, Kazunori Shibata, Ayaka Shoda, Hisaaki Shinkai, Aru Suemasa, Naoshi Sugiyama, Rieko Suzuki, Yudai Suwa, Kentaro Somiya, Hajime Sotani, Tadashi Takano, Kakeru Takahashi, Keitaro Takahashi, Hirotaka Takahashi, Fuminobu Takahashi, Ryuichi Takahashi, Ryutaro Takahashi, Takamori Akiteru, Hideyuki Tagoshi, Hiroyuki Tashiro, Nobuyuki Tanaka, Keisuke Taniguchi, Atsushi Taruya, Takeshi Chiba, Dan Chen, Shinji Tsujikawa, Yoshiki Tsunesada, Morio Toyoshima, Yasuo Torii, Kenichi Nakao, Kazuhiro Nakazawa, Shinichi Nakasuka, Hiroyuki Nakano, Shigeo Nagano, Kouji Nakamura, Yoshinori Nakayama, Atsushi Nishizawa, Erina Nishida, Yoshito Niwa, Taiga Noumi, Tatsuaki Hashimoto, Kazuhiro Hayama, Tomohiro Harada, Wataru Hikida, Yoshiaki Himemoto, Hisashi Hirabayashi, Takashi Hiramatsu, Mitsuhiro Fukushima, Ryuichi Fujita, Masa-Katsu Fujimoto, Toshifumi Futamase, Mizuhiko Hosokawa, Hideyuki Horisawa, Kei-ichi Maeda, Hideo Matsuhara, Nobuyuki Matsumoto, Yuta Michimura, Osamu Miyakawa, Umpei Miyamoto, Shinji Miyoki, Shinji Mukohyama, Toshiyuki Morisawa, Mutsuko Y. Morimoto, Shigenori Moriwaki, Kent Yagi, Hiroshi Yamakawa, Toshitaka Yamazaki, Kazuhiro Yamamoto, Shijun Yoshida, Taizoh Yoshino, Chul-Moon Yoo, Yaka Wakabayashi (On April 1 st , 2016) The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  3. Future Plan ・ KAGRA Collaborators are working hard to complete the observatory; there will be no future without it. ・ On the other hand, having future vision is also important not to loose our way in the GW field. The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  4. KAGRA and DECIGO B-DECIGO (~2020s) KAGRA (~2018) Space observatory Ground-based Detector  Low-freq. GWs  High-freq. GW event ( CBC, SN, …) (CBC, IMBH, Cosmology) The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  5. After the First Detection ... ・ New mysteries and issues after the first detection: - Origin of heavier mass ( 30𝑁 ⨀ ) BBH. - Other GW sources: BNS, SN, Pulsar,…. - Sky localization and EM Follow-up observations. - Test of GR, Cosmology. ・ Network of 2 nd -gen. GW antennae (aLIGO, AdVIRGO, KAGRA, LIGO-India) will be formed in several years. ・ Two ways after that for Astronomy and Cosmology: - 3 rd – gen. ground-based GW antennae (ET , CE). - Space GW antennae ( LISA, DECIGO, ASTROD,…). The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  6. Multiple-band Observation ・ Electro-Magnetic Observations : Multiple-band observations CMB Radio (Radio, Optical/IR, X-ray, g -ray)  Variety of knowledge corr. to IR x-ray the Energy and Temperature γ -ray GRBs of the target. ・ Gravitational-wave Observations : Frequency of radiated GW ~ 1/ (Time scale of source motion)  Variety of knowledge corr. to the Time scale and Mass of sources. The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  7. GW Science at Low Frequency ・ Low-Freq. (~0.1Hz) GW antennae will provide original sciences: * Mass and orbital parameters of binaries, * Intermediate-Mass Black Hole binaries, * Stochastic background GW. ・ Fruitful sciences by space-borne GW antennae B-DECIGO: ℎ~10 −23 Hz −1/2 (0.1Hz). ・ Cosmological Observation by DECIGO : ℎ~10 −24 Hz −1/2 (0.1Hz). The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  8. DECIGO The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  9. Conceptual Design DECIGO (DECI-hertz interferometer Gravitational wave Observatory) Arm length: 1000 km Finesse: 10 Mirror diameter: 1 m Mirror mass: 100 kg Laser power: 10 W Laser wavelength ： 532 nm Arm cavity S/C: drag free Laser Mirror Photo- 3 interferometers Drag-free S/C detector The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  10. DECIGO Observation Band ‘Bridge’ the obs.gap between Space GW antenna LISA and Terrestrial detectors Obs. band around 0.1 Hz 10 –16 Terrestrial Detectors 10 –18 1/2 ] (Ad. LIGO, KAGRA, etc) Strain [1/Hz 10 –20 LISA 10 –22 10 –24 DECIGO 10 –26 10 –4 10 –2 10 0 10 2 10 4 Frequency [Hz] The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  11. Targets and Science IMBH binary inspiral Galaxy formation (Massive BH) Binary BH (or NS) inspiral Cosmology (Inflation, Dark energy) Stochastic background Fundamental physics GW amplitude [Hz -1/2 ] 10 -18 10 -20 DECIGO Merger (1 unit) 3month 10 -22 Merger 10 -24 DECIGO (Correlation) 10 -26 NS inspiral (z~1) 10 -4 10 -2 10 0 10 2 10 4 Frequency [Hz] The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  12. Observation of the Early Universe インフレーション -35 からの重力波 Background: original figure by NASA/WMAP Science Team The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  13. ‘Window’ for the Early Universe DECIGO band is open window for direct observation of the early universe. critical density of the universe) 𝛁 𝐇𝐗 (GW energy ratio for PPTA KAGRA LISA CMB Pol. ET , CE Compact GW from Inflation DECIGO MBH-MBH Binaries Frequency [Hz] Kuroyanagi+, PRD (2009) Pablo, PRD (2011) The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  14. GW Energy Density and Amplitude ・ GW energy density ratio GW energy density Ω GW 𝑔 = 1 𝑒𝜍 GW (𝑔) 𝜍 𝑑 𝑒 ln 𝑔 Critical energy density of the universe Equivalent GW Amplitude Hubble’s constant 2 3𝐼 0 2 ℎ GW 𝑔 = 10𝜌 2 𝑔 3 Ω GW 𝑔 The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  15. GW Energy Density and Amplitude 2 3𝐼 0 2 ℎ GW 𝑔 = 10𝜌 2 𝑔 3 Ω GW 𝑔 ℎ GW [Hz -1/2 ] 𝑔 −1.5 Ω GW Freq. [Hz] Freq. [Hz] Smaller amplitude in high freq. The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  16. ‘Window’ for the Early Universe DECIGO band is open window for direct observation of the early universe. critical density of the universe) 𝛁 𝐇𝐗 (GW energy ratio for PPTA KAGRA LISA CMB Pol. ET , CE Compact GW from Inflation DECIGO MBH-MBH Binaries Frequency [Hz] Kuroyanagi+, PRD (2009) Pablo, PRD (2011) The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  17. Observation of GW from Inflation BICEP2, (POLARBEAR,…) DECIGO, (KAGRA, aLIGO,…) CMB B-mode polarization GWB observation by observation by micro-wave GW telescope. telescope. CMB pol. telescope Primordial Gravitation EM Wave (microwave) al Wave Gravitational Wave Inflation GW telescope Original figure by Tajima (Kyoto 2011) The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  18. GW from Inflation Energy density ∝ Tensor-Scalar Ratio ( 𝑠 ). Power spectrum : Evolution history of the Universe. DECIGO Correlation ・ Spectrum Power.  Energy scale of inflation ・ Cut-off freq.  Energy scale of Reheating Nakayama+, Journal of Cosmology and Astroparticle Physics 06 (2008) 020. The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  19. B-DECIGO The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

  20. Updated Roadmap for DECIGO Figure: S.Kawamura 2014 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 R&D R&D R&D Fabrication Fabrication Fabrication Mission DECIGO Ground test B-DECIGO Pathfinder SDS- DECIGO + Piggy- 1/SWIM (DPF) back opportunity . Purpose Demonstration and test Sciences by GW GW Astronomy of space IFO observation and Cosmology technique Micro-g experiment FF with 3 S/C Design 3 S/C , 3 arms. FP cavity + Drag-free 3-4 IFO units The 3rd KAGRA International Workshop (May 21st, 2017, Academia Sinica, Taipei, Taiwan)

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