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Status of TAMA. Masaki Ando (Department of Physics, University of Tokyo) on behalf of the TAMA Collaboration. TAMA collaborators. - PowerPoint PPT Presentation
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The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)
Status of TAMA Status of TAMA
Masaki Ando (Department of Physics, University of Tokyo)
on behalf of the TAMA Collaboration
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 2
TAMA collaboratorsTAMA collaborators
Tomomi Akutsu, Tomotada Akutsu, Masaki Ando, Koji Arai, Akito Araya, Hideki Asada, Youichi Aso, Mark A. Barton, Peter Beyersdorf, Youhei Fujiki, Masa-Katsu Fujimoto, Ryuichi Fujita, Mitsuhiro Fukushima, Toshifumi Futamase, Yusaku Hamuro, Tomiyoshi Haruyama, Hideaki Hayakawa, Kazuhiro Hayama,Gerhard Heinzel, Gen'ichi Horikoshi, Hideo Iguchi, Yukiyoshi Iida, Kunihito Ioka, Hideki Ishitsuka, Norihiko Kamikubota, Nobuyuki Kanda, Takaharu Kaneyama, Yoshikazu Karasawa, Kunihiko Kasahara, Taketoshi Kasai, Mayu Katsuki, Keita Kawabe, Mari Kawamura, Seiji Kawamura, Nobuki Kawashima, Fumiko Kawazoe, Yasufumi Kojima, Keiko Kokeyama, Kazuhiro Kondo, Yoshihide Kozai, Hideaki Kudo, Kazuaki Kuroda, Takashi Kuwabara, Namio Matsuda, Norikatsu Mio, Kazuyuki Miura, Osamu Miyakawa, Shoken Miyama, Shinji Miyoki, Hiromi Mizusawa, Shigenori Moriwaki, Mitsuru Musha, Shigeo Nagano, Yoshitaka Nagayama, Ken'ichi Nakagawa, Takashi Nakamura, Hiroyuki Nakano, Ken-ichi Nakao, Yuhiko Nishi, Kenji Numata, Yujiro Ogawa, Masatake Ohashi, Naoko Ohishi, Akira Okutomi, Ken-ichi Oohara, Shigemi Otsuka, Yoshio Saito, Shihori Sakata, Misao Sasaki, Kouichi Sato, Nobuaki Sato, Shuichi Sato, Youhei Sato, Hidetsugu Seki, Aya Sekido, Naoki Seto, Masaru Shibata, Hisaaki Shinkai, Takakazu Shintomi, Kenji Soida, Kentaro Somiya, Toshikazu Suzuki, Hideyuki Tagoshi, Hirotaka Takahashi, Ryutaro Takahashi, Akiteru Takamori, Shuzo Takemoto, Kohei Takeno, Takahiro Tanaka, Keisuke Taniguchi, Shinsuke Taniguchi, Toru Tanji, Daisuke Tatsumi, C.T. Taylor, Souichi Telada, Kuniharu Tochikubo, Masao Tokunari, Takayuki Tomaru, Kimio Tsubono, Nobuhiro Tsuda, Yoshiki Tsunesada, Takashi Uchiyama, Akitoshi Ueda, Ken-ichi Ueda, Fumihiko Usui, Koichi Waseda, Yuko Watanabe, Hiromi Yakura, Akira Yamamoto, Kazuhiro Yamamoto, Toshitaka Yamazaki, Yuriko Yanagi, Tatsuo Yoda, Jun'ichi Yokoyama, Tatsuru Yoshida, Zong-Hong Zhu
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 3
OutlineOutline
TAMA300 overview
TAMA300 data-taking runs Data taking 9 (Nov. 2003 – Jan. 2004)
Efforts for detector improvement Noise hunting,
TAMA-SAS
TAMA data-analysis reviewChirp, Burst, Ringdown searches,
Detector characterization
Summary
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 4
TAMA300 (1)TAMA300 (1)- Overview -- Overview -
TAMA project (1995-)
National AstronomicalObservatory at Mitaka, Japan
Baseline 300m
Sufficient sensitivity for Galactic binary inspiralsAutomated crewless operation9 observation runs (Data : ~3000 hours)
First obs. run in 1999 (DT1)
Upgrade and observation runs
TAMA300, an interferometric GW detector in Japan Baseline length : 300m Fabry-Perot-Michelson interferometer with power recycling Placed at National Astronomical Observatory in Japan
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 5
TAMA300 (2)TAMA300 (2)- Detector configuration -- Detector configuration -
10W laser
10m MC
Main IFO
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 6
TAMA300 (3)TAMA300 (3)- Data acquisition and distribution -- Data acquisition and distribution -
Main IFO
Dataacquisition
Data storage
DataAnalysis
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 7
TAMA300 (4)TAMA300 (4)- Facilities -- Facilities -
Center Room Beam tube
End Room
InjectionBench
BSRM NM1
NM2
MC1
10W LaserOutput Bench
300m Tube
EM1
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 8
TAMA300 (5)TAMA300 (5) - Components -- Components -
Mirror suspension
Fused silica Mirror
10W laser source
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 9
TAMA observation runs
Data taking run (1)Data taking run (1)- Observation runs -- Observation runs -
Data Taking ObjectiveObservation
timeTypical strain noise level
Total data(Longest lock)
DT1 August, 1999 Calibration test 1 night 3x10-19 /Hz 1/210 hours
(7.7 hours)
DT2 September, 1999 First Observation run 3 nights 3x10-20 /Hz 1/2 31 hours
DT3 April, 2000Observation with
improved sensitivity3 nights 1x10-20 /Hz 1/2 13 hours
DT4Aug.-Sept.,
2000100 hours'
observation data2 weeks
(night-time operation)1x10-20 /Hz 1/2
(typical)167 hours
(12.8 hours)
DT5 March, 2001100 hours' observation with high duty cycle
1 week(whole-day operation)
1.7x10-20 /Hz 1/2
(LF improvement)111 hours
DT6Aug.-Sept.,
20011000 hours' observatio
n data 50 days 5x10-21 /Hz 1/21038 hours(22.0 hours)
DT7Aug.-Sept.,
2002Full operation with
Power recycling2 days 25 hours
DT8Feb.-April.,
20031000 hours
Coincidence2 months 3x10-21 /Hz 1/2
1157 hours(20.5 hours)
DT9Nov. 2003 -Jan., 2004
Automatic operation
6 weeks 1.5x10-21 /Hz 1/2 558 hours(27 hours)
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 10
Data taking run (2)Data taking run (2)- Data Taking 9 -- Data Taking 9 -
TAMA DT9
0 200 400 600 800 1000 120010
–21
10–20
10–19
No
ise
Le
ve
l [1
/Hz1/
2 ]
Time [hour]
DT9
DT8DT6Noise floor level drift
Thu SunTueMon Fri SatWed
Observation (continuous over 10min)
Date and Time in JST (UTC +9 hours) 29
6
17
24
313029
22
15
11
Nov. 28, 2003
54
12
16
23 25
18
7
30
Dec. 1
8
19
26 27
20
139
2 3
10 14
21
28
Jan. 1 32 4
8 95 106 7 11
Data Taking 9 Nov. 28, 2003 – Jan. 10, 2004 558 hours of data Noise level : 2x10-21 /Hz1/2
2nd half : 200 hours (Christmas, new-year Holiday terms) Better noise level Stable environment
In particular …
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 11
Data taking run (3)Data taking run (3)- Noise level in DT9 -- Noise level in DT9 -
Noise level
Data Taking 9 Noise level : 2x10-21 /Hz1/2 Mostly limited by shot noise and photo-detector noise
DT9
Shot noise+Detector noise
DT6
Improvements:
Implementation of power recycling (power gain: 4.5) Better stabilization for laser-frequency noise
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 12
Data taking run (4)Data taking run (4)- Observable range in DT9 -- Observable range in DT9 -
Observable distanceDetectable distance for binary inspiral (SNR=10, optimal condition)
DT9
DT6
72.8 kpc for 1.4 Mo binary inspirals
TAMA300 covers most part of our Galaxy
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 13
Data taking run (5)Data taking run (5)- Automated observation in DT9 -- Automated observation in DT9 -
Crewless observation in DT9Automated detector operation Master-system (intelligent switching) PC + PCI boards + LabVIEW 64ch digital I/O 16ch A/D + 24ch D/A Lock acquisition Auto adjustment Interface with external system
Self-switching sub-system Logic circuit + Embedded micro processor Laser source control MC control Laser intensity stabilization Beam axes control
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 14
Detector improvement (1)Detector improvement (1)- Noise hunting -- Noise hunting -
Noise investigation
DT9 noise level Seismic noise Alignment noise Shot noise
Unidentified noise Scattered light ? Beam jitter ? Laser source ? RF detection ? Electronics ?
Noise hunting!
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 15
Detector improvement (2)Detector improvement (2)- Noise hunting with RMI -- Noise hunting with RMI -
Strategy
Back to full configuration checking the noise level
Investigate noise behavior with simplified configuration
Power-recycled MichelsonRemove POsSingle PD at the dark port … etc
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 16
Detector improvement (3)Detector improvement (3)- Noise reduction -- Noise reduction -
RMI noise reductionImproved about 10 times after DT9
Simpler configurationScattered noise reduction
Back to full configuration step by step
Recent result … Re-installed POs keep best noise
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 17
Detector improvement (4)Detector improvement (4)- RMI phase noise -- RMI phase noise -
RMI noise
Contribution of RMI phase noise
Promising result
RMI phase noise
Alignment noise (can be improved)
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 18
Detector improvement (5)Detector improvement (5)- Seismic noise reduction -- Seismic noise reduction -
TAMA-SAS
Prototype test with a 3-m Fabry-Perot cavity
Expected Isolation @4Hz 10-8 ➞ 10-11 m/Hz1/2
Expected RMS velocity 3.7 ➞ 0.3 m/s
Installation in 2005
Design for TAMA : fixedMain parts : delivered
Development for better seismic attenuation
Seismic attenuation system (SAS) For low frequency (0.1 ~ 10Hz) R&D with Caltech and Univ. of Pisa
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 19
TAMA data analysis (1)TAMA data analysis (1)- Overview -- Overview -
TAMA data-analysis activities
Detector characterization Calibration, data conditioning, Noise behavior, Correlation between detectors
Coincidence analysis Chirp: LIGO-TAMA Burst: LIGO-TAMA Un-triggered search Triggered search for GRB ROG- TAMA
Compact binary inspirals: chirpChange in signal frequency (low high) Waveforms are well predicted (2.5 PN)
Stellar-core collapses, etc: burst Short GW signals from violent phenomenaPossible coincidence with electromagnetic and/or neutrino
New-born black hole: ringdown Damped sinusoidal waves from a quasi-normal modeWaveforms are predicted
Pulsars, Compact binaries:
periodic Continuous GW signalsGain SNR with long-term observations
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 20
TAMA data analysis (2)TAMA data analysis (2)- Chirp-wave analysis -- Chirp-wave analysis -
Chirp-wave analysis
Upper limit for Galactic event rate
DT6: 50-day observation (2001) Range : 33.1kpc 83 events /yr (1-2Msol)
DT8: 60-day observation (2003) Range : 42.2kpc 29 events /yr (1-3Msol)
DT9: 50-day observation (2003-
2004) Range : 72.8kpc Search in progress…
Target: Binary inspirals Waveforms by post-Newtonian approx.Schemes: Matched filtering Fake reduction with a 2-test Galactic simulation Upper limit for event rate
2 3 4 5 6 7 8 90
10
20
30
40
50
60
70
101
102
103
Det
acta
ble
ran
ge
Data–taking runs
Up
per
lim
it f
or
even
t ra
tes
[eve
nts
/yr]
(C
.L.=
90%
)
[kp
c] (
SN
R=
10)
Detactable
Event upper limit
upper limitGalactic–event
range
In this workshop … H. Takahashi, S. Fairhurst (Thu. PM)
TAMA DT8 - LIGO S2 coincidence analysis
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 21
TAMA data analysis (3)TAMA data analysis (3)- Burst-wave analysis -- Burst-wave analysis -
Burst-wave analysisTarget: Unmodelled: Stellar-core collapse, etc Ref. waveforms by numerical sim.Schemes: Matched filtering Excess-power filter, Linear-fit filter Wavelet-based filter Fake reduction: Veto with auxiliary channel Time-scale selection Galactic simulation Upper limit for event rate
In this workshop … M.Ando (Fri. PM): DT9 results with an excess-pow. filter T.Akutsu (Fri. PM): DT9 results with an ALF filter K.Hayama (Poster): Development of a wavelet-based filter P.Sutton (Fri. PM): LIGO-TAMA coincidence analysis
102 10310–24
10–22
10–20
10–18
De
tec
tor
No
ise
Le
ve
l [
1/H
z1/2 ]
Frequency [Hz]
TAMA
LCGT design sensitivity
noise level(DT9)
GW
RS
S A
mp
litu
de
an
d
10kpc events
100pc events
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 22
TAMA data analysis (4)TAMA data analysis (4)- Ringdown-wave analysis -- Ringdown-wave analysis -
Ringdown-wave analysis
Target: New-born BHs Damped sinusoidal waveform Mass, Kerr parameter of BHSchemes: Matched filtering Fake reduction: Selection of events with realistic freq. and Q-value Behavior in template space
In this workshop … Y.Tsunesada (Thu. PM): DT6-9 event search D.Tatsumi (Poster): Fake-reduction method
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 23
TAMA data analysis (5)TAMA data analysis (5)- Other activities -- Other activities -
Continuous-wave analysis
Target: Possible pulsar at SN1987A remnant Sinusoidal wave without precise freq. informationSchemes: Matched filtering (Heterodyne detection) DT8-9 analysis in progress…
In this workshop … S.Telada (Thu. AM): Calibration in time domain N.Kanda (Thu. AM): Effect of correlation of two detectors in LCGT
Characterization
K.Soida et al., Class. Quantum Grav. 20 (2003) S645
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 24
SummarySummary
TAMA detectorTAMA detector Data Taking 9Data Taking 9 Improve the sensitivity by a factor of 2Improve the sensitivity by a factor of 2 observable range 72kpc for 1.4observable range 72kpc for 1.4MMoo binaries binaries
Automated stable operationAutomated stable operation
Noise investigation with RMINoise investigation with RMI Preparation for TAMA-SAS installationPreparation for TAMA-SAS installation
Data analysisData analysis Inspiral, burst, and ringdownInspiral, burst, and ringdown searchessearches
results are being obtainedresults are being obtained
LIGO-TAMA coincidence analysesLIGO-TAMA coincidence analyses Some activities on data analysis:Some activities on data analysis:
Continuous waveContinuous wave search search Waveform estimationWaveform estimation Detector correlationsDetector correlations
The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France) 25
End