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ICRC2003 08/06/2003

Current Status of TAMA300. Shuichi Sato National Astronomical Observatory of Japan for The TAMA collaboration. ICRC2003 08/06/2003. Contents. Overview of TAMA300 gravitational wave antenna Detector site IFO configuration Current status of the detector Power recycling

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ICRC2003 08/06/2003

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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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