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Current Status and Future Plans of TAMA300 Gravitational Wave Detector at NAOJ (ICRC 2003)

This document presents an overview of the TAMA300 gravitational wave antenna, including its detector site, configuration, and current status. It highlights improvements in sensitivity achieved through power recycling and enhanced control systems. Key findings include noise levels, upgraded incident power enhancements, and analysis of the noise budget. The future plans focus on automating operations and upgrading the vibration isolation system to enhance stability and sensitivity. The paper summarizes the successful operation and ongoing advancements to meet the challenges in gravitational wave detection.

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Current Status and Future Plans of TAMA300 Gravitational Wave Detector at NAOJ (ICRC 2003)

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  1. Current Status of TAMA300 Shuichi Sato National Astronomical Observatory of Japan for The TAMA collaboration ICRC2003 08/06/2003

  2. Contents • Overview of TAMA300 gravitational wave antenna • Detector site • IFO configuration • Current status of the detector • Power recycling • IFO control system • Improved IFO sensitivity ICRC2003 08/06/2003

  3. 300m 300m Site view • Mitaka campus of NAOJ, Tokyo • (E 139.32.21 N 35.40.25) Mitaka,Tokyo (NAOJ) West end room Center room South end room Aerial photograph of the TAMA site (NAOJ, Mitaka, Tokyo, JAPAN) ICRC2003 08/06/2003

  4. IFO Configuration Active air spring ICRC2003 08/06/2003

  5. Principle of Power Recycling ICRC2003 08/06/2003

  6. Control scheme of Power Recycled FPMI ICRC2003 08/06/2003

  7. Control scheme of Power Recycled FPMI ICRC2003 08/06/2003

  8. Improved Sensitivity • Noise level of FPMI (Without power recycling) • dx ~ 1.5 x 10-18 [m/Hz1/2 ] @ 1kHz • Dominant contribution in high frequency region • Detector + Shot noise • Frequency noise ICRC2003 08/06/2003

  9. Improved Sensitivity • Noise level of FPMI (Without power recycling) • dx ~ 1.5 x 10-18 [m/Hz1/2 ] @ 1kHz • Dominant contribution in high frequency region • Detector + Shot noise • Frequency noise • Improvements • Incident power • enhancement by • Power recycling • Highly stabilized • laser frequency ICRC2003 08/06/2003

  10. Improved Sensitivity • Noise level of FPMI (Without power recycling) • dx ~ 1.5 x 10-18 [m/Hz1/2 ] @ 1kHz • Dominant contribution in high frequency region • Detector + Shot noise • Frequency noise • Improvements • Incident power • enhancement by • Power recycling • Highly stabilized • laser frequency • Noise level of PRFPMI • dx ~ 8 x 10-19 [m/Hz1/2 ] • @ 1.5kHz ICRC2003 08/06/2003

  11. Expected Observable Distance for Binary Inspirals • SNR=10, optimal incident angle are assumed ICRC2003 08/06/2003

  12. Noise budget (DT8) ICRC2003 08/06/2003

  13. Sensitivity History ICRC2003 08/06/2003

  14. Summary • Current status of TAMA300 • Power recycling • Operating stably • All mirrors are alignment-controlled • Recycling gain : 4.5 • Detector sensitivity • dx~8 x10-19[m/rHz]@1.5kHz • Reaching practical shot noise limit • Future plan • Investigation of the noise issues • Between 100Hz and 1kHz • Further automation for the observation • To operate the interferometer with less operators • Upgrade of the vibration isolation system • Seismic Attenuation System (SAS) • For better stability and sensitivity ICRC2003 08/06/2003

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