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Japanese Gravitational Wave Detectors: LCGT and DECIGO

Japanese Gravitational Wave Detectors: LCGT and DECIGO. Sora. Frontiers in Optics 2009 Laser Science XXV Oct. 13, 2009 San Jose, USA Seiji Kawamura (NAOJ), LCGT Collaboration, DECIGO Working Group. Outline. Roadmap Ground-based detector TAMA300 CLIO LCGT Space antenna DECIGO

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Japanese Gravitational Wave Detectors: LCGT and DECIGO

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  1. Japanese Gravitational Wave Detectors:LCGT and DECIGO Sora Frontiers in Optics 2009 Laser Science XXV Oct. 13, 2009 San Jose, USA Seiji Kawamura (NAOJ), LCGT Collaboration, DECIGO Working Group

  2. Outline • Roadmap • Ground-based detector • TAMA300 • CLIO • LCGT • Space antenna • DECIGO • DECIGO Pathfinder

  3. Roadmapofthe Japanese GW detection Advanced LCGT TAMA LCGT CLIO R&D Pre-DECIGO DECIGO Pathfinder DECIGO

  4. Ground-based Detector • TAMA300 • CLIO • LCGT

  5. TAMA300 • 300 m power-recycled FP Michelson interferometer • located on the NAOJ campus in Tokyo • Project started 1995 • Best sensitivity in world 2000-2002

  6. NewSeismic Attenuation System Joint development with LIGO (RiccardoDeSalvo et al.) based on earlier Virgo concept Photo: Nikon

  7. CLIO • 100 m cryogenic prototype • Differential FP interferometer • located in the Kamioka mine in Gifu TAMA300

  8. Ground motion inKamioka mine

  9. Sensitivity of CLIO Mirror suspension thermal noise --inversely proportional to f 2.5 Thermal noise limit by eddy current damping between actuator magnets and metal solenoid holder --inversely proportional to f 2 Displacement noise 1/√Hz Mirror thermal noise Frequency

  10. LCGT • 3km • Underground at Kamioka • Cryogenic mirrors

  11. Goal Sensitivity of LCGT

  12. Detection range of LCGT

  13. L/H+L/L+V+LCGT 50% L/H+L/L+V 50% LCGT in network • LIGO(H)+LIGO(L)+Virgo+LCGT • Max sensitivity (M.S.): +13% • Coverage at 0.5 M.S.: 100% • 3 detector duty cycle: 82% • LIGO(H)+LIGO(L)+Virgo • Coverage at 0.5 M.S.: 72% • 3 detector duty cycle: 51% B. F. Schutz

  14. Organization LCGT: hosted by ICRR under MOU with NAOJ and KEK. LCGT collaboration: 118 members (92 domestic, 26 oversea members)

  15. Funding Status • Proposal for the 2010 start did not go through. • We will submit a proposal for the 2011 start. • Application for the stimulus fund was turned down.

  16. 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]

  17. 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

  18. 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

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

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

  21. 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)

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

  23. BH binary (1000 M◎ z=1) Coalescence Inflation Science by DECIGO 10-19 10-20 10-21 10-22 10-23 10-24 10-25 10-26 Mini-black hole  Dark matter Formation of super-massive BH BransDicke parameter 5 years 1 unit Radiation pressure noise 3 months Strain [Hz-1/2] NS binary (z=1) Shot noise Acceleration of Universe  Dark energy Correlation (3 years) Coalescence Verification of inflation 10-3 10-2 10-1 1 10 102 103 Frequency [Hz]

  24. Requirements • Force noise of DECIGO should be 50 times more stringent than LISA • Acceleration noise in terms of h: comparable • Distance: 1/5000 • Mass: 100 • Sensor noise of DECIGO should be10 times looser than LCGT • Sensor noise in terms of h: comparable, • Storage time: 10

  25. Roadmap R&D Fabrication R&D Fabrication R&D Fabrication DICIGOPathfinder (DPF) Pre-DECIGO SWIM DECIGO

  26. DEDCIGO Pathfinder (DPF) • Single satellite • Earth orbit • Altitude:500km • Sun synchronous Thruster Local Sensor Actuator Arm length: 30 cm Arm length: 1000 km

  27. Test of frequency stabilization system in space Test of drag-free system Test of laser in space Test of locking system in space conceptual design and objectives of DPF Iodine cell Floating mirror Laser Thruster Local Sensor Actuator Observation of GW at 0.1 – 1 Hz

  28. Payload and standard bus DPF Payload Mast structure Size : 950mm cube Weight : 150kg Power : 130W Data Rate: 800kbps Mission thruster x12 Mission Thruster head Stabilized. Laser source On-board Computer Power Supply SpW Comm. Satellite Bus (‘Standard bus’ system) Size : 950x950x1100mm Weight : 200kg SAP : 960W Battery: 50AH Downlink : 2Mpbs DR: 1GByte 3N Thrusters x 4 Interferometer module Satellite Bus system Busthruster Solar Paddle

  29. Goal sensitivity of DPF

  30. Detection range

  31. R&D for Subsystems Test mass module Frequency-stabilized laser Electrostatic sensor/ actuator Drag-free model Interferometric sensor Thruster

  32. SWIM launch and operation Tiny GW detector module Launched in Jan. 23, 2009 Photo： JAXA In-orbit operation TAM: Torsion Antenna Module with free-falling test mass (Size : 80mm cube, Weight : ~500g) Test mass ~47g Aluminum, Surface polished Small magnets for position control Coil Photo sensor Reflective-type optical displacement sensor Separation to mass ~1mm Sensitivity ~ 10-9 m/Hz1/2 6 PSs to monitor mass motion

  33. 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 (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 (Tokyo) Deputy: Takashima (ISAS) Mission phase Detector Ueda (NAOJ) Laser Ueda (ILS) Musya (ILS) Housing Sato (Hosei) Drag free Moriwaki (Tokyo) Sakai (ISAS) Thruster Funaki (ISAS) Bus Takashima (ISAS) Data Kanda (Osaka city)

  34. Collaborations • LISA • 1st LISA-DECIGOworkshop held in JAXA/ISAS (Nov. 2008) • Stanford Univ. • Charge control using UV LED, etc. ⇒　MOU • NASA Goddard • Fiber laser　⇒　started discussion • JAXAformation flight group • Formation flight • Big bang center of the Univ. of Tokyo • DECIGOadopted as one of the main themes • Advanced technology center of NAOJ • Will make it a main nucleus of DPF • UNISEC (University Space Engineering Consortium) • Started discussion

  35. Funding Status • Proceeded to the final hearing as one of the two candidates for the 2nd small science satellite run by JAXA/ISAS (launching three missions between 2012 and 2016), but not selected. • We will apply for the 3rd mission. (The selection will take place in 2010.)

  36. Conclusions • We need LCGT and DPF funded as soon as possible to establish the GW astronomy in the future!

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