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The Japanese Space Gravitational Wave Antenna: DECIGO. HEPL Seminar Feb. 11, 2009 @ Stanford Univ. Seiji Kawamura (National Astronomical Observatory of Japan). Sora. Outline. Gravitational wave DECIGO DECIGO pathfinder Summary Appendix Displacement noise free interferometer

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  1. The Japanese Space Gravitational Wave Antenna: DECIGO HEPL Seminar Feb. 11, 2009 @ Stanford Univ. Seiji Kawamura (National Astronomical Observatory of Japan) Sora

  2. Outline • Gravitational wave • DECIGO • DECIGO pathfinder • Summary • Appendix • Displacement noise free interferometer • Juggling interferometer

  3. Gravitational wave • Predicted by Einstein • Emitted from accelerating objects • Propagates as tidal distortion of space Distortion of space ~ 10-23 Not yet detected!

  4. GW Sources • Neutron star / black hole binaries • Supernova • Beginning of the universe • Etc.

  5. GW 10 -43 sec (Planck time） Neutrino EM 1 sec (Formation of Proton, Neutron) 380,000 year (Transparent to radiation) How far (old) can we see? Beginning of the universe 13.7 billion year (Now)

  6. Gravitational wave astronomy

  7. Detection of GWby laser interferometer Suspended Mirror Suspended Mirror Detector Beam splitter Interfering beam Laser

  8. The longer arm length gives larger signals! Mirror Mirror Mirror Laser Photodetector Mirror Laser Photodetector

  9. Large-scale detectors GEO (600 m) TAMA (300 m) LIGO (4 km) LCGT (3 km) CLIO (100 m) VIRGO (3 km) LIGO (4 km)

  10. Standard optical configuration Fabry-Perot arm cavity Fabry-Perot arm cavity Enhance GW signals Recycling mirror: Increase effective laser power

  11. Laser Interferometer in Space • Signal increased - Due to longer interaction between GW and light - Cancellation of signals at higher frequencies • Noise reduced - Lower seismic noise and gravity gradient noise Sensitivity improved at lower frequencies

  12. LISA • Arm length: 5,000,000km • Frequency range: 1 mHz - 0.1 Hz • Target Source: White dwarf binary, Giant BH coalescence • Optical configuration: Light transponder LISA project

  13. 10-18 moved above LISA band 10-20 To be moved 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]

  14. 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

  15. 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

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

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

  18. 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)

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

  20. BH binary (1000 M◎ z=1) Coalescence Science by DECIGO (1) 10-19 10-20 10-21 10-22 10-23 10-24 10-25 10-26 Formation of Super-massive BH 1 cluster Radiation pressure noise Strain [Hz-1/2] Shot noise 10-3 10-2 10-1 1 10 102 103 Frequency [Hz]

  21. 5 years 3 months NS binary (z=1) Coalescence Science by DECIGO (2) 10-19 10-20 10-21 10-22 10-23 10-24 10-25 10-26 1 cluster Radiation pressure noise Strain [Hz-1/2] Acceleration of Universe ⇓ Dark energy Shot noise 10-3 10-2 10-1 1 10 102 103 Frequency [Hz]

  22. 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)

  23. Science by DECIGO (3) 10-19 10-20 10-21 10-22 10-23 10-24 10-25 10-26 1 cluster Radiation pressure noise Strain [Hz-1/2] Shot noise Correlation (3 years) Inflation (GW=210-16) Verification of inflation 10-3 10-2 10-1 1 10 102 103 Frequency [Hz]

  24. 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.

  25. Roadmap R&D Fabrication R&D Fabrication R&D Fabrication DICIGO Pathfinder (DPF) Pre-DECIGO DECIGO

  26. DECIGO Pathfinder (DPF) DPF DECIGO Floating Mirrors Laser 1,000 km 30 cm PD Shrink the arm length from 1,000 km to 30 cm Drag-free S/C

  27. Conceptual design and Technologies to demonstrate Stabilization system Floating mirror Thruster Laser Local Sensor Actuator • Drag-free control system • Laser source and stabilization system • Control of Fabry-Perot interferometer • Launch-lock system

  28. Goal sensitivity of DPF

  29. Expected sources

  30. JAXA’s Small science satellite series • Plan to launch 3 small satellites between 2011 and 2015 • using next-generation solid rocket booster • Reduce time and cost by means of ‘Standard bus system’ • Bus weight : ~ 200kg, Bus power : ~ 800W • Downlink ~ 2Mbps, Data storage ~ 1GByte • 3-axes attitude control • SpaceWire-based data processing system • We submitted a proposal for DPF

  31. In June 2007, I attended the LIGO PAC meeting at Caltech, and we were invited to dinner at a Chinese restaurant.

  32. We gained momentum! DPF was selected as one of the 4 important mission candidates for small science satellite series run by JAXA/ISAS.

  33. Stabilized Laser DPF Payload Thruster Control Unit Size : 900mm cube Weight : 100kg Power : 200W Data Rate: 600kbps Mission thruster x16 Central Processing Unit Mission Thrusters Housing Control Unit Interferometer Module Interfererometer Control Unit Bus Thrusters Solar Paddle DPF S/C Power Supply SpW Comm. Satellite Bus (‘Standard bus’ system) Size : 900mm cube Weight : 200kg SAP : 800W Battery: 50AH Downlink : 2Mpbs DR: 1GByte 3N Thrusters x 4

  34. DPF DPF Mission Outline Launch: 2012 (target) Mission Lifetime: 1 year (nominal) Launcher: Single launch by M-V follow-on (solid rocket booster under development) PBS (Post-Boost stage) for fine orbit insertion 500km Orbit: Low-Earth (Altitude 500km), Sun-synchronous orbit (dusk-dawn) Attitude Control: Gravity-gradient stab. Drag-free control with mission thrusters (Safe hold control by bus thrusters)

  35. History and Future 2006 Nov. Submitted a proposal of DPF 2007 Jun. Fortune cookie 2007 Aug. Selected as a Pre-Phase-A mission R&D costs funded 2008 Sep. Submitted Phase-A proposal 2008 Dec. Hearing held for selecting the 2nd mission 2009 Mar. 2nd mission will be selected

  36. Pre-DECIGO

  37. Sensitivity of Pre-DECIGO S/N~14 for NS-NS@300Mpc, 10-20 events/year

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

  39. DECIGO-WG Seiji Kawamura, Masaki Ando, Takashi Nakamura, Kimio Tsubono, Naoki Seto, Shuichi Sato, Kenji Numata, Nobuyuki Kanda, Ikkoh Funaki, Takeshi Takashima, Takahiro Tanaka, Kunihito Ioka, Kazuhiro Agatsuma, Koh-suke Aoyanagi, Koji Arai, Akito Araya, Hideki Asada, Yoichi Aso, Takeshi Chiba, Toshikazu Ebisuzaki, Yumiko Ejiri, 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, Nobuki Kawashima, Fumiko Kawazoe, Naoko Kishimoto, Kenta Kiuchi, Shiho Kobayashi, Kazunori Kohri, Hiroyuki Koizumi, Yasufumi Kojima, Keiko Kokeyama, Wataru Kokuyama, 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, Kouji Nakamura, Hiroyuki Nakano, Kenichi Nakao, Shinichi Nakasuka, Yoshinori Nakayama, Kazuhiro Nakazawa, Erina Nishida, Kazutaka Nishiyama, Atsushi Nishizawa, Yoshito Niwa, Yoshiyuki Obuchi, Masatake Ohashi, Naoko Ohishi, Masashi Ohkawa, Norio Okada, 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, Rieko Suzuki, Hideyuki Tagoshi, Fuminobu Takahashi, Kakeru Takahashi, Keitaro Takahashi, Ryutaro Takahashi, Ryuichi Takahashi, Tadayuki Takahashi, Hirotaka Takahashi, Takamori Akiteru, Tadashi Takano, Keisuke Taniguchi, Atsushi Taruya, Hiroyuki Tashiro, Mitsuru Tokuda, Yasuo Torii, Morio Toyoshima, Shinji Tsujikawa, Yoshiki Tsunesada, Akitoshi Ueda, Ken-ichi Ueda, Masayoshi Utashima, Yaka Wakabayashi, Hiroshi Yamakawa, Kazuhiro Yamamoto, Toshitaka Yamazaki, Jun'ichi Yokoyama, Chul-Moon Yoo, Shijun Yoshida, Taizoh Yoshino

  40. 1st InternationalLISA-DECIGO Workshop • Nov. 12-13, 2008 @ ISAS, Sagamihara, Japan • Participants: • Danzmann, Heinzel, Gianolio, Jennrich, Lobo, McNamara, Mueller, Prince, Stebbins, Sun, Vitale, … • Accomplishments: • Mutual understanding • Kick-off of collaborations • Exposure of the missions to people in the neighboring fields

  41. Collaboration with Stanford • UV LED discharge for DPF • Other R&D for DECIGO

  42. Summary • DECIGO can detect GWs from the inflation as well as can bring us extremely interesting science. • DPF has been selected as one of the important mission candidates for small science satellite series; they plan to launch 3 missions in 5 years starting from 2011.

  43. Let DPF fly!

  44. Possible breakthrough for3rd-generation detectors:Displacement-noise free Interferometer Kawamura and Chen, PRL, 93, (2004) 211103 Chen and Kawamura, PRL, 96 (2006) 231102

  45. Motivation • Displacement noise: seismic Noise, thermal noise, radiation pressure noise • Cancel displacement noise  shot noise limited sensitivity • Increase laser power  sensitivity improved indefinitely Diplacement noise Displacement noise Cancel displacement noise Shot noise Sensitivity Increase laser power PD Laser Frequency

  46. GW and mirror motion interact with light differently Difference outstanding for GW wavelength  distance between masses GW On reflection On propagation Light Mirror motion Mirror motion

  47. Cancel motion of objects Clock • Motion of A, B, and C cancelled • GW signal remains

  48. Why is it possible? # of MQ (4) ＞ # of DOF (3) MQ: Measurable quantity DOF: Degree of freedom Therefore a combination of MQs that is free from DOFs exists!

  49. Clock noise? Clock • Motion: cancelled • Clock noise: not cancelled

  50. Why? # of DOF (Clock): 3 # of DOF (Displacement): 3 # of MQ: 4 Therefore it is not always possible to make a combination of MQs that is free from all the DOFs!

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