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The Japanese Space Gravitational Wave Antenna - DECIGO

The Japanese Space Gravitational Wave Antenna - DECIGO. Amaldi6 @Okinawa June 22, 2005

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The Japanese Space Gravitational Wave Antenna - DECIGO

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  1. The Japanese Space Gravitational Wave Antenna - DECIGO Amaldi6 @Okinawa June 22, 2005 Seiji Kawamura, Takashi Nakamura, Masaki Ando, Kimio Tsubono, Naoki Seto, Shigeo Nagano, Takahiro Tanaka, Takehiko Ishikawa, Ken-ichi Ueda, Mitsuru Musha, Takashi Sato, Mizuhiko Hosokawa, Kenji Numata, Hisashi Hirabayashi, Tadashi Takano, Masa-Katsu Fujimoto, Atsushi Taruya, Yoshiaki Himemoto, Chul-Moon Yoo, Kenichi Nakao, Tomohiro Harada, Kunihito Ioka, Norichika Sago, Wataru Hikida, Shuichi Sato, Keiko Kokeyama, Mitsuhiro Fukushima, Hiroo Kunimori, Toshitaka Yamazaki, Masashi Ohkawa, Tatsuaki Hashimoto, Koh-suke Aoyanagi, Kazuhiro Agatsuma, Tomotada Akutsu, Hideki Asada, Yoichi Aso, Koji Arai, Akito Araya, Takeshi Ikegami, Koji Ishidoshiro, Kiyotomo Ichiki, Yousuke Itoh, Kaiki T. Inoue, Yoshiharu Eriguchi, Naoko Ohishi, Masatake Ohashi, Kenichi Oohara, Akira Okutomi, Shogo Kamagasako, Nobuki Kawashima, Mari Kawamura, Nobuyuki Kanda, Katsuhiko Ganzu, Kenta Kiuchi, Hideaki Kudoh, Kazuaki Kuroda, Kazunori Kohri, Yoshihide Kozai, Yasufumi Kojima, Shiho Kobayashi, Motoyuki Saijo, Masaaki Sakagami, Shihori Sakata, Misao Sasaki, Masaru Shibata, Hisaaki Shinkai, Naoshi Sugiyama, Hajime Sotani, Hirotaka Takahashi, Ryuichi Takahashi, Ryutaro Takahashi, Hideyuki Tagoshi, Hiroyuki Tashiro, Keisuke Taniguchi, Takeshi Chiba, Shinji Tsujikawa, Yoshiki Tsunesada, Masao Tokunari, Isao Naito, Hiroyuki Nakano, Kouji Nakamura, Atsushi Nishizawa, Yoshito Niwa, Choetsu Nozawa, Kazuhiro Hayama, Takashi Hiramatsu, Toshifumi Futamase, Kei-ichi Maeda, Hideo Matsuhara, Hiromi Mizusawa, Yasushi Mino, Osamu Miyakawa, Shinji Miyoki, Shinji Mukohyama, Toshiyuki Morisawa, Kazuhiro Yamamoto, Jun'ichi Yokoyama, Shijun Yoshida, and Taizoh Yoshino

  2. Contents • What is DECIGO? • Current Status • Budget Situation • Preliminary Experiment • Summary

  3. 10-18 10-20 10-22 10-24 Gap between TerrestrialDetectors and LISA LISA Terrestrial Detectors (e.g. LCGT) Strain [Hz-1/2] Gap 10-4 102 100 104 10-2 Frequency [Hz]

  4. 10-18 10-20 10-22 10-24 DECIGO Bridges the Gap The Japanese Space Gravitational Wave Antenna - DECIGO Deci-hertz Interferometer Gravitational Wave Observatory LISA Terrestrial Detectors (e.g. LCGT) Strain [Hz-1/2] DECIGO 10-4 102 100 104 10-2 Frequency [Hz]

  5. Importance of Bridgingthe Gap New window brings new science! • Observe inspiral sources that have moved above the LISA band • Observe inspiral sources that have not yet moved into the ground-based detector band • Especially inspiral of IMBH • Completely new sources could be detected • Completely new science could be obtained

  6. 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)

  7. Past Now Near Future Far Future TAMA LCGT 1st Priority DECIGO DECIGO as a Future Gravitational Wave Detection Project in Japan

  8. History of DECIGO 1999 the LISA study group convened by Tsubono 2000Short-arm space antenna suggested by Kawamura 2001Space GW antenna WG convened as one of the possible future projects in NAOJ 2001 Named as DECIGO in the PRL paper by Seto, Kawamura, Nakamura (DECIDE and GO) 2002 1st DECIGO-WG meeting 2003 2nd DECIGO-WG meeting (FP-type DECIGO suggested by Ando) 2005 3rd DECIGO-WG meeting

  9. Roadmap for DECIGO 06 07 08 09 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 R&D Advanced R&D PF1 Observation Design & Fabrication PF2 Design & Fabrication Observation DECIGO 06 07 08 09 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24

  10. Pre-Conceptual Designfor DECIGO • LISA-type DECIGO - Shorter arm length • Fabry-Perot-Cavity-type DECIGO - Even shorter arm length - Resonance of light in the cavity For both types - Better shot noise (higher power, shorter wavelength, larger mirror) - Better force noise (heavier mass)

  11. Fabry-Perot Type DECIGO Around Lagrange Point Fabry-Perot cavity Drag-Free Satellite

  12. Actuating Force in FP-DECIGO Anti-Gravity +Anti-GW Outer Satellite The distance should be kept constant Proof Mass Anti-Drag + Anti-Gravity +Anti-GW

  13. Sensitivity of DECIGO Force noise= 1/100 of LISA’s

  14. Preliminary Simulatorfor LISA-type DECIGO • Built a preliminary simulator for DECIGO as a simulator for detecting the Earth’s gravity field around the Earth Distance: 50 km Satellite 1 Satellite 2 vMAX: 1 cm/s （Doppler Shift: 20 kHz 地球

  15. Schematic Diagram ofthe Preliminary Simulator Monitor FB to DDS Lock to mid-fringe by AOD Simulate Doppler shift by AOD Stabilized Frequency using 5 layer shielded cavity (like LISA) Simulate distance by optical fiber

  16. Sensitivity ofthe Preliminary Simulator

  17. Budget Situation for DECIGOand other GW Projects in Japan • Budget request for “Frontier of All Wavelength Gravitational Wave Astronomy” to be submitted this fall - TAMA and CLIO - R&D for DECIGO - Pulsar Timing - Super-high frequency G.W. detection • (Budget request for LCGT submitted this year from ICRR)

  18. R&D for DECIGO Overall Tests Ground-based DECIGO Simulator (S. Kawamura, NAOJ) DECIGO-Pathfinder (M. Ando, Univ. of Tokyo) Key Technologies Measurement System (K. Tsubono, Univ. of Tokyo) Frequency Stabilization (T. Sato, Niigata Univ.) Drag-free System (T. Ishikawa, JAXA-ISAS) Evaluation of Light Source (M. Hosokawa, NICT) Satellite Technologies (?, JAXA-ISAS) Light Source (K. Ueda, ILS)

  19. Objectives of the R&D • R&D of subsystems • Overall tests by ground-based simulator and DECIGO-Pathfinder1 • R&D for optional technologies • Defining the objectives and conceptual design of DECIGO-PF2 • Establishing the conceptual design of DECIGO

  20. Ground-Based Simulater • Test the system on earth as much as possible • Investigate the system at low frequencies • Observe GW at low frequencies LF Pendulum LF Pendulum Laser Seismic Isolation System Seismic Isolation System

  21. Pathfinder • Test the system which can be tested only in space (Drag-free system) • Check if the measurement system works in space • Observe GW at low frequencies • This effort couples with the JAXA-ISAS’s new satellite plan Measurement System Laser Resonated Drag Free System One Small Satellite

  22. Summary • It is important to bridge the gap between terrestrial detectors and LISA. • The Japanese space antenna DECIGO can bridge the gap. • We have started serious investigation of DECIGO. • We will submit a budget request for DECOGO R&D this fall. • We hope that we will be able to start the R&D for DECIGO soon.

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