Current Status of TAMA300 Shuichi Sato

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Presentation transcript:

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 IFO control system Improved IFO sensitivity ICRC2003 08/06/2003

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

IFO Configuration Active air spring ICRC2003 08/06/2003

Principle of Power Recycling ICRC2003 08/06/2003

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

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

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

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

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

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

Noise budget (DT8) ICRC2003 08/06/2003

Sensitivity History ICRC2003 08/06/2003

Summary Current status of TAMA300 Power recycling Detector sensitivity 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