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The Japanese Space Gravitational Wave Antenna DECIGO

The Japanese Space Gravitational Wave Antenna DECIGO. TAUP2007 @Sendai, Japan Aug 11, 2007

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The Japanese Space Gravitational Wave Antenna DECIGO

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  1. The Japanese Space Gravitational Wave Antenna DECIGO TAUP2007 @Sendai, Japan Aug 11, 2007 Seiji Kawamura, Masaki Ando, Takashi Nakamura, Kimio Tsubono, Takahiro Tanaka, Ikkoh Funaki, Naoki Seto, Kenji Numata, Shuichi Sato, Nobuyuki Kanda, Takeshi Takashima, Kunihito Ioka, Kazuhiro Agatsuma, Tomotada Akutsu, Tomomi Akutsu, Koh-suke Aoyanagi, Koji Arai, Yuta Arase, Akito Araya, Hideki Asada, Yoichi Aso, Takeshi Chiba, Toshikazu Ebisuzaki, Motohiro Enoki, Yoshiharu Eriguchi, Masa-Katsu Fujimoto, Ryuichi Fujita, Mitsuhiro Fukushima, Toshifumi Futamase, Katsuhiko Ganzu, Tomohiro Harada, Tatsuaki Hashimoto, Kazuhiro Hayama, Wataru Hikida, Yoshiaki Himemoto, Hisashi Hirabayashi, Takashi Hiramatsu, Feng-Lei Hong, Hideyuki Horisawa, Mizuhiko Hosokawa, Kiyotomo Ichiki, Takeshi Ikegami, Kaiki T. Inoue, Koji Ishidoshiro, Hideki Ishihara, Takehiko Ishikawa, Hideharu Ishizaki, Hiroyuki Ito, Yousuke Itoh, Shogo Kamagasako, Nobuki Kawashima, Fumiko Kawazoe, Hiroyuki Kirihara, Naoko Kishimoto, Kenta Kiuchi, Shiho Kobayashi, Kazunori Kohri, Hiroyuki Koizumi, Yasufumi Kojima, Keiko Kokeyama, WataruKokuyama, Kei Kotake, Yoshihide Kozai, Hideaki Kudoh, Hiroo Kunimori, Hitoshi Kuninaka, Kazuaki Kuroda, Kei-ichi Maeda, Hideo Matsuhara, Yasushi Mino, Osamu Miyakawa, Shinji Miyoki, Mutsuko Y. Morimoto, Tomoko Morioka , Toshiyuki Morisawa, Shigenori Moriwaki, Shinji Mukohyama, Mitsuru Musha, Shigeo Nagano, Isao Naito, Noriyasu Nakagawa, Kouji Nakamura, Hiroyuki Nakano, Kenichi Nakao, Shinichi Nakasuka, Yoshinori Nakayama, Erina Nishida, Kazutaka Nishiyama, Atsushi Nishizawa, Yoshito Niwa, Masatake Ohashi, Naoko Ohishi, Masashi Ohkawa, Akira Okutomi, Kouji Onozato, Kenichi Oohara, Norichika Sago, Motoyuki Saijo, Masaaki Sakagami, Shin-ichiro Sakai, Shihori Sakata, Misao Sasaki, Takashi Sato, Masaru Shibata, Hisaaki Shinkai, Kentaro Somiya, Hajime Sotani, Naoshi Sugiyama, Yudai Suwa, Hideyuki Tagoshi, Kakeru Takahashi, Keitaro Takahashi, Tadayuki Takahashi, Hirotaka Takahashi, Ryuichi Takahashi, Ryutaro Takahashi, Takamori Akiteru, Tadashi Takano, Keisuke Taniguchi, Atsushi Taruya, Hiroyuki Tashiro, Mitsuru Tokuda, Masao Tokunari, Morio Toyoshima, Shinji Tsujikawa, Yoshiki Tsunesada, Ken-ichi Ueda, Masayoshi Utashima, Hiroshi Yamakawa, Kazuhiro Yamamoto, Toshitaka Yamazaki, Jun'ichi Yokoyama, Chul-Moon Yoo, Shijun Yoshida, Taizoh Yoshino

  2. 10-18 have moved Above LISA band 10-20 will move into TD band 10-22 10-24 What is DECIGO? Deci-hertz Interferometer Gravitational Wave Observatory (Kawamura, et al., CQG 23 (2006) S125-S131) • Bridges the gap between LISA and terrestrial detectors • Low confusion noise  Extremely high sensitivity Terrestrial detectors (e.g. LCGT) LISA Strain [Hz-1/2] DECIGO Confusion Noise 10-4 102 100 104 10-2 Frequency [Hz]

  3. Pre-conceptual design Differential FP interferometer Arm length: 1000 km Mirror diameter: 1 m Laser wavelength：0.532 m Finesse: 10 Laser power: 10 W Mirror mass: 100 kg S/C: drag free 3 interferometers Arm cavity Arm cavity Laser Mirror Photo- detector Drag-free S/C

  4. Shorten arm length Implement FP cavity Radiation pressure noise f-2 Shorten arm length Shot noise f1 Shot noise Implement FP cavity FP cavity type Better best- sensitivity Why FP cavity? Transponder type (e.g. LISA) Radiation pressure noise f-2 Shot noise f1 Strain Shot noise Transponder type (e.g. LISA) Frequency

  5. S/C I S/C II Drag free and FP cavity: compatible? Mirror

  6. S/C I S/C II FP cavity and drag free : compatible? Relative position between mirror and S/C Local sensor Mirror Thruster Thruster

  7. No signal mixture S/C I S/C II Drag free and FP cavity: compatible? Relative position between mirror and S/C Local sensor Mirror Thruster Thruster Actuator Interferometer output (GW signal)

  8. Orbit and constellation (preliminary) Earth Correlation for stochastic background Record disk Sun Increase angular resolution

  9. BH binary (1000 M◎ z=1) Coalescence 5 years 3 months NS binary (z=1) Inflation Coalescence Goal Sensitivity and Science 10-19 10-20 10-21 10-22 10-23 10-24 10-25 10-26 Formation of Super-massive BH 1 unit Radiation pressure noise Strain [Hz-1/2] Acceleration of Universe ⇓ Dark energy Shot noise Correlation (3 years) Verification of inflation 10-3 10-2 10-1 1 10 102 103 Frequency [Hz]

  10. Requirements • Acceleration noise should be suppressed below radiation pressure noise • Force noise: DECIGO = LISA/50 (Acceleration noise in terms of h: 1, Distance: 1/5000, Mass: 100) • Fluctuation of magnetic field, electric field, gravitational field, temperature, pressure, etc. • Sensor noise should be suppressed below shot noise. • Phase noise: DECIGO = LCGT×10 (Sensor noise in terms of h: 1, storage time: 10) • Frequency noise, intensity noise, beam jitter, etc. • Thruster system should satisfy range, noise, bandwidth, and durability.

  11. Roadmap R&D Fabrication R&D Fabrication R&D Fabrication DICIGO Pathfinder (DPF)  Ando’ s talk Pre-DECIGO DECIGO

  12. Interim organization PI: Kawamura (NAOJ) Deputy: Ando (Tokyo) Executive Committee Kawamura (NAOJ), Ando (Tokyo), Seto (NAOJ), Nakamura (Kyoto), Tsubono (Tokyo), Tanaka (Kyoto), Funaki (ISAS), Numata (Merryland), Sato (NAOJ), Kanda (Osaka city), Takashima (ISAS), Ioka (Kyoto) Pre-DECIGO Sato (NAOJ) Detector Numata (Merryland) Ando (Tokyo) Science, Data Tanaka (Kyoto) Seto (NAOJ) Kanda (Osaka city) Satellite Funaki (ISAS) Design phase DECIGO pathfinder Leader: Ando (Tokyo) Deputy: Takashima (ISAS) Mission phase Detector Ando (Tokyo) Laser Ueda (ILS) Musya (ILS) Housing Sato (NAOJ) Drag free Moriwaki (Tokyo) Sakai (ISAS) Thruster Funaki (ISAS) Bus Takashima (ISAS) Data Kanda (Osaka city)

  13. Current status • There are now 140 members from 50 institutes in DECIGO working group • Budget request (DECIGO R&D and fabrication of DPF, $20M, 6 years) was rejected. • We will submit budget request (R&D for DECIGO and DP, $10M, 5-6 years) this year again. • DPF working group was formally approved by JAXA/ISAS. • Budget request (R&D for DPF, $65K, 1 year) to JAXA/ISAS was approved.

  14. Summary • DECIGO can not only bridge the gap between terrestrial detectors and LISA, but also open a very deep window at 0.1 – 10 Hz. • DECIGO will use FP arm cavity to further improve the sensitivity. • We have obtained some budget to initiate R&D for DPF. • We hope that we will obtain a bigger budget for DECIGO R&D, and that DPF mission will be approved soon!

  15. Acceleration of Expansion of the Universe Expansion＋Acceleration? DECIGO GW NS-NS (z～1) Output Template (No Acceleration) Strain Real Signal ? Phase Delay～1sec (10 years) Time Seto, Kawamura, Nakamura, PRL 87, 221103 (2001)

  16. Clamp Release Release Release Hold Hold Hold Ground-based simulator(juggling interferometer) • Realize continual free-fall condition • Measure force noise • Test clamp release system • High GW sensitivity at 0.1 – 10 Hz • Might be applied to future terrestrial detectors Moving up and down Continually Freely falling ~ 2 m Position ~ 1 sec Time

  17. Fortune Cookie

  18. History of DECIGO 1999 the LISA study group convened by Tsubono 2000 Short-arm space antenna suggested by Kawamura 2001 Space GW antenna WG convened as one of the possible future projects in NAOJ 2001 Named as DECIGO in the PRL paper 2002 1st DECIGO workshop 2003 2nd DECIGO workshop (FP-type DECIGO suggested by Ando) 2005 3rd DECIGO workshop 2006 4th DECIGO workshop (FP-type DECIGO adopted as a pre-conceptual design) 2007 5th DECIGO workshop

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