TY - JOUR
T1 - Mirror suspension system for the TAMA SAS
AU - Takamori, Akiteru
AU - Ando, Masaki
AU - Bertolini, Alessandro
AU - Cella, Giancarlo
AU - DeSalvo, Riccardo
AU - Fukushima, Mitsuhiro
AU - Iida, Yukiyoshi
AU - Jacquier, Florian
AU - Kawamura, Seiji
AU - Márka, Szabolcs
AU - Nishi, Yuhiko
AU - Numata, Kenji
AU - Sannibale, Virginio
AU - Somiya, Kentaro
AU - Takahashi, Ryutaro
AU - Tariq, Hareem
AU - Tsubono, Kimio
AU - Ugas, Jose
AU - Viboud, Nicolas
AU - Yamamoto, Hiroaki
AU - Yoda, Tatsuo
AU - Wang, Chenyang
PY - 2002/4/7
Y1 - 2002/4/7
N2 - Several R&D programmes are ongoing to develop the next generation of interferometric gravitational wave detectors providing the superior sensitivity desired for refined astronomical observations. In order to obtain a wide observation band at low frequencies, the optics need to be isolated from the seismic noise. The TAMA SAS (seismic attenuation system) has been developed within an international collaboration between TAMA, LIGO, and some European institutes, with the main objective of achieving sufficient low-frequency seismic attenuation (-180 dB at 10 HZ). The system suppresses seismic noise well below the other noise levels starting at very low frequencies above 10 Hz. It also includes an active inertial damping system to decrease the residual motion of the optics enough to allow a stable operation of the interferometer. The TAMA SAS also comprises a sophisticated mirror suspension subsystem (SUS). The SUS provides support for the optics and vibration isolation complementing the SAS performance. The SUS is equipped with a totally passive magnetic damper to suppress internal resonances without degrading the thermal noise performance. In this paper we discuss the SUS details and present prototype results.
AB - Several R&D programmes are ongoing to develop the next generation of interferometric gravitational wave detectors providing the superior sensitivity desired for refined astronomical observations. In order to obtain a wide observation band at low frequencies, the optics need to be isolated from the seismic noise. The TAMA SAS (seismic attenuation system) has been developed within an international collaboration between TAMA, LIGO, and some European institutes, with the main objective of achieving sufficient low-frequency seismic attenuation (-180 dB at 10 HZ). The system suppresses seismic noise well below the other noise levels starting at very low frequencies above 10 Hz. It also includes an active inertial damping system to decrease the residual motion of the optics enough to allow a stable operation of the interferometer. The TAMA SAS also comprises a sophisticated mirror suspension subsystem (SUS). The SUS provides support for the optics and vibration isolation complementing the SAS performance. The SUS is equipped with a totally passive magnetic damper to suppress internal resonances without degrading the thermal noise performance. In this paper we discuss the SUS details and present prototype results.
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U2 - 10.1088/0264-9381/19/7/352
DO - 10.1088/0264-9381/19/7/352
M3 - Article
AN - SCOPUS:0036269355
SN - 0264-9381
VL - 19
SP - 1615
EP - 1621
JO - Classical and Quantum Gravity
JF - Classical and Quantum Gravity
IS - 7
ER -