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Current Status of Japanese Detectors

Current Status of Japanese Detectors. Daisuke Tatsumi National Astronomical Observatory of Japan. Contents. The Japanese Detectors TAMA CLIO DECIGO Analysis (Brief introduction) Inspiral (Tagoshi) Veto analysis (Ishidoshiro) Noise characterization (Akutsu).

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Current Status of Japanese Detectors

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  1. Current Status ofJapanese Detectors Daisuke Tatsumi National Astronomical Observatory of Japan

  2. Contents • The Japanese Detectors • TAMA • CLIO • DECIGO • Analysis (Brief introduction) • Inspiral (Tagoshi) • Veto analysis (Ishidoshiro) • Noise characterization (Akutsu) This is a content of my talk. First, I would like to talk about the current status of TAMA, CLIO and DECIGO detectors. And then I will givea brief introduction to the current activities of data analysis.

  3. The Japanese Detectors Two prototype detectors for LCGT arebeing developed in Japan. • TAMA Location: Suburb of Tokyo, Japan Baseline length: 300m • CLIO Location: Kamioka underground site, Japan Baseline length: 100m Feature: Cryogenic Sapphire Mirrors One is TAMA detector which is located in west suburb of Tokyo. It has a baseline length of three hundred meters. The another is CLIO detector which is located in Kamioka mine. This mine is about three hundred kilo-meters away from Tokyo. The most important feature of this detector is that it adopts cryogenic sapphire mirrors.

  4. TAMA Brief History 1995 Construction start 1999 First observation experiment 2000 World best sensitivity at the time 2001 1000 hours Observation 2002 Power recycling (PR) 2003 Second 1000 hours observation with PR 2004 The ninth observation experiment TAMA has started observation experiments since 1999. By the beginning of 2004, 3000 hours of data in total was accumulated through the nine observation experiments.

  5. TAMA upgrade After the last observation experiment in 2004, TAMA detector is being upgraded to reduce the low frequency noises.

  6. 1. Horizontal Inverted Pendulum resonant freq. : 30mHz 2. Vertical Double MGAS Filters Each of 0.5Hz resonance 3. Payload Top mass (Platform) Intermediate mass Mirror - Recoil mass TAMA SAS (Seismic Attenuation System) TAMA-SAS (IP + GASF + Payload) To reduce the seismic noise, new isolation system is being installed. This figure shows a schematic view of TAMA SAS. To isolate horizontal motion, an inverted pendulum is implemented. For vertical motion, double stage MGAS filters are used. Finally mirror was suspended by a double pendulum.

  7. SAS Installation Schedule 2005 Sep:First SAS was installed for inline end mirror (1) 2006 Jun:Second SAS was installed for inline near mirror (2) Aug:A Fabry-Perot cavity was locked with SAS, 3 Oct:Third and forth SAS were installed to the perpendicular arm cavity (3), (4). 4 2 1 The SAS installation was started in September, 2005. In this summer, a Fabry-Perot cavity was locked with SAS. Now all of four test mass mirrors are suspended by SAS.

  8. Locked FP configuration Transmitted Power of SAS FP cavity Transmitted Power of old suspension cavity Feedback signal to Mirror TIME Stable lock of SAS Fabry-Perot cavity With the locked Fabry-Perot configuration, we operated the interferometer. In this configuration, one arm was installed SASs but another one was still old suspensions. The cavities were locked for six and a half hours. Even if in the daytime of the working days, stable locks were realized by SAS. This is a important progress for TAMA, because many human activities disturbed our observations.

  9. Improvement of cavity length fluctuation This figure shows the improvement of a cavity length fluctuation by using SAS. Above 2 Hz region, the SAS improved the seismic noise more than 24 dB.

  10. Improvement of angular fluctuations The angular fluctuation of the mirror is also reduced by SAS. Above 3 Hz region, the SAS improved the angular fluctuations more than 25 dB. Actual improvements at 100 Hz region will be confirmed by locked Fabry-Perot configuration. And then, our detector will be tuned for power-recycled Fabry-Perot Michelson configuration by the end of next July.

  11. TAMA Summary - To improve low frequency sensitivity, we are installing SAS for the test masses. - We confirmed * Stable mass lock of a cavity with SAS, * Improvement of length fluctuation and * Improvement of angular fluctuations. We are currently tuning SASs for another cavity. • We plan to take data in the next summer and plan to continue TAMA operations with R&D for LCGT.

  12. CLIOCryogenic Laser Interferometer Observatoryin Kamioka mine

  13. CLIO & LCGT Purpose of CLIO (100m arm length) Technical demonstration of key features of LCGT. LCGT is a future plan of Japanese GW group. LCGT is located at Kamioka underground site for low seismic noise level, adopts Cryogenic Sapphiremirrors for low thermal noise level and has arms of 3km long. Except for the arm length, CLIO has same features of LCGT. Therefore, the detector can demonstrate them as a prototype of LCGT.

  14. Construction All of vacuum pipes, cryostats and cryocoolers were installed by the June, 2005.

  15. First operation of the cryogenic interferometer First operation of the cryogenic interferometer has been demonstrated on 18 February, 2006 ! 23K End Mirror Temperature (K) Lock about 50 min. Near Mirror 20K This figure shows mirror temperatures as a function of time. During the lock, the mirrors keep its temperature around 20K. 20K

  16. Current Best Target sensitivity at 300K CLIO sensitivity at 300K After the several cryogenic operations, CLIO detector has been operated at 300K. To improve the sensitivity, noise hunting is in progress. This figure shows the current best noise spectrum of CLIO. At all of frequency regions, the differences from the target sensitivity at 300K are abouta factor of 4. Displacement (m/rtHz) 10 10k 1k 100 Frequency (Hz)

  17. Observable ranges forInspiral GW signals 1.4Msolar For neutron star binaries, CLIO and TAMA can observe the event within 49kpc and 73kpc, respectively. CLIO TAMA LISM We can say that the two detectors have almost same sensitivity. At over 10 solar mass region, CLIO keeps good sensitivities due to its low seismic noises. It is the greatest benefit of underground site.

  18. CLIO Summary • The first operation of the cryogenic interferometer was successfully demonstrated. • Current sensitivity at 300K is close to the target sensitivity within a factor of 4. • Several observation experiments at 300K are in progress. • (Details of detector characterization will be given • by Akutsu) • -Once the displacement noisereaches at thermal noise level,its improvement by cooling will be demonstrated.

  19. 10-18 10-20 10-22 10-24 10-2 100 102 DECIGODECi-hertz Interferometer Gravitational Wave Observatory The DECIGO project is also in progress. The pre-conceptual design has been finished. Most important feature of this detector is adopting the Fabry-Perot Michelson scheme. Its baseline length is 1000 km. Each of cavities has a finesse of 10. By using this detector, GW signals of deci-hertz region will be detected. Pre-conceptual Design FP Michelson interferometer Arm length: 1000 km Orbit and constellation: TBD Laser: 532 nm, 10 W Mirror: 1 m, 100 kg Finesse: 10 • NS+NS (1.4+1.4Msun) • z<1 (SN>26: 7200/yr) • z<3 (SN>12: 32000/yr) • z<5 (SN>9: 47000/yr) • IMBH (100+100Msun) • z<1 (SN>1000: ?/yr) Drag-free satellite BH+BH(1000Msun) @z=1 Arm cavity merger Foreground GW = 2.210-16 3 year-correlation NS+NS@z=1 PD Laser Arm cavity merger PD Drag-free satellite Drag-free satellite

  20. Activities of Data Analysis • Detector Characterization • Veto analysis by Ishidoshiro • CLIO data by Akutsu • Inspiral • A combined result of DT6, 8 and 9 for galactic events was obtained by Tagoshi Finally I would like to give a brief introduction to the activities of data analysis. In this afternoon session of detector characterization, two talks will be given. One is veto analysis of TAMA data by Ishidoshiro. The other is the evaluation of the first CLIO data by Akutsu. The last topic is the inspiral search of TAMA data by Tagoshi.

  21. TAMA inspiral analysis by H. Tagoshi, et al.

  22. TAMA inspiral analysis (1) Search for inspiraling compact binaries were performed by using TAMA data in 2000-2004. Total length of data analyzed (DT 4,5,6,8,9) Length of data for upper limit (DT 6,8,9) We deriveda single (combined) upper limit from DT6, 8, and 9 data. This enable us to derive a more stringent upper limit than previous works. (DT4 and 5 data were not used for upper limit, since they were shorter and sensitivity was much inferior than later DT6-9 data).

  23. TAMA inspiral analysis (2) Upper limit onthe Galactic event rate Single upper limit is given by by using data of 102.6 days Conservative upper limit (gr-qc/0610064, PRD in press) By using data of a hundred days, we set a combined upper limit to be 20 events per year on galactic events. This result was accepted by PRD.

  24. End

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