status of tama
Download
Skip this Video
Download Presentation
Status of TAMA

Loading in 2 Seconds...

play fullscreen
1 / 25

Status of TAMA - PowerPoint PPT Presentation


  • 149 Views
  • Uploaded on

Status of TAMA. Masaki Ando (Department of Physics, University of Tokyo) on behalf of the TAMA Collaboration. TAMA collaborators.

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about 'Status of TAMA' - zeno


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
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)

tama collaborators
TAMA 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)

outline
Outline
  • TAMA300 overview
  • TAMA300 data-taking runs

Data taking 9 (Nov. 2003 – Jan. 2004)

  • Efforts for detector improvement

Noise hunting,

TAMA-SAS

  • TAMA data-analysis review

Chirp, Burst, Ringdown searches,

Detector characterization

  • Summary

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

tama300 1 overview
TAMA300 (1)- Overview -
  • TAMA project (1995-)

TAMA300, an interferometric GW detector in Japan

Baseline length : 300m

Fabry-Perot-Michelson interferometer with power recycling

Placed at National Astronomical Observatory in Japan

First obs. run in 1999 (DT1)

Upgrade and observation runs

Baseline 300m

Sufficient sensitivity for

Galactic binary inspirals

Automated crewless operation

9 observation runs

(Data : ~3000 hours)

National Astronomical

Observatory at Mitaka, Japan

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

tama300 2 detector configuration
TAMA300 (2)- Detector configuration -

Main IFO

10W laser

10m MC

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

tama300 3 data acquisition and distribution
TAMA300 (3)- Data acquisition and distribution -

Data

storage

Data

acquisition

Main IFO

Data

Analysis

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

tama300 4 facilities
TAMA300 (4)- Facilities -

Beam tube

Center Room

NM2

Injection

Bench

BS

300m Tube

MC1

RM

NM1

Output Bench

10W Laser

End Room

EM1

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

tama300 5 components
TAMA300 (5)- Components -

Mirror suspension

10W laser source

Fused silica Mirror

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

data taking run 1 observation runs
Data taking run (1)- Observation runs -
  • TAMA observation runs

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

data taking run 2 data taking 9
Data taking run (2)- Data Taking 9 -
  • TAMA DT9

Data Taking 9

Nov. 28, 2003

– Jan. 10, 2004

558 hours of data

Noise level : 2x10-21 /Hz1/2

In particular …

DT6

Noise floor level drift

DT8

2nd half : 200 hours

(Christmas, new-year

Holiday terms)

Better noise level

Stable environment

DT9

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

data taking run 3 noise level in dt9
Data taking run (3)- Noise level in DT9 -
  • Noise level

Data Taking 9

Noise level : 2x10-21 /Hz1/2

Mostly limited by

shot noise and

photo-detector noise

DT6

DT9

Improvements:

Implementation of

power recycling

(power gain: 4.5)

Better stabilization

for laser-frequency noise

Shot noise

+Detector noise

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

data taking run 4 observable range in dt9
Data taking run (4)- Observable range in DT9 -
  • Observable distance

Detectable distance for binary inspiral

(SNR=10, optimal condition)

DT9

72.8 kpc for

1.4 Mo binary inspirals

DT6

TAMA300 covers

most part of

our Galaxy

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

data taking run 5 automated observation in dt9
Data taking run (5)- Automated observation in DT9 -
  • Crewless observation in DT9

Automated 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)

detector improvement 1 noise hunting
Unidentified noise

Scattered light ?

Beam jitter ?

Laser source ?

RF detection ?

Electronics ?

Noise hunting!

Detector improvement (1)- Noise hunting -
  • Noise investigation

DT9 noise level

Seismic noise

Alignment noise

Shot noise

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

detector improvement 2 noise hunting with rmi
Detector improvement (2)- Noise hunting with RMI -
  • Strategy

Investigate noise behavior

with simplified configuration

Power-recycled Michelson

Remove POs

Single PD at the dark port

… etc

Back to full configuration

checking the noise level

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

detector improvement 3 noise reduction
Detector improvement (3)- Noise reduction -
  • RMI noise reduction

Back to full configuration

step by step

Improved

about 10 times after DT9

Simpler configuration

Scattered noise reduction

Recent result …

Re-installed POs

 keep best noise

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

detector improvement 4 rmi phase noise
Detector improvement (4)- 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)

detector improvement 5 seismic noise reduction
Detector improvement (5)- Seismic noise reduction -
  • TAMA-SAS

Development for better seismic attenuation

Seismic attenuation system (SAS)

For low frequency (0.1~10Hz)

R&D with Caltech and Univ. of Pisa

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 mm/s

Design for TAMA : fixed

Main parts : delivered

Installation in 2005

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

tama data analysis 1 overview
TAMA data analysis (1)- Overview -
  • TAMA data-analysis activities

Compact binary inspirals: chirp

Change in signal frequency (low  high)

Waveforms are well predicted (2.5 PN)

Stellar-core collapses, etc: burst

Short GW signals from violent phenomena

Possible coincidence with

electromagnetic and/or neutrino

New-born black hole: ringdown

Damped sinusoidal waves

from a quasi-normal mode

Waveforms are predicted

Pulsars, Compact binaries: periodic

Continuous GW signals

Gain SNR with long-term observations

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

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

tama data analysis 2 chirp wave analysis
TAMA data analysis (2)- Chirp-wave analysis -
  • Chirp-wave analysis

Target:

Binary inspirals

Waveforms by post-Newtonian approx.

Schemes:

Matched filtering

Fake reduction with a c2-test

Galactic simulation

 Upper limit for event rate

In this workshop …

H. Takahashi, S. Fairhurst (Thu. PM)

TAMA DT8 - LIGO S2

coincidence 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…

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

tama data analysis 3 burst wave analysis
TAMA data analysis (3)- Burst-wave analysis -
  • Burst-wave analysis

Target:

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

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

tama data analysis 4 ringdown wave analysis
TAMA data analysis (4)- Ringdown-wave analysis -
  • Ringdown-wave analysis

Target:

New-born BHs

Damped sinusoidal waveform

 Mass, Kerr parameter of BH

Schemes:

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)

tama data analysis 5 other activities
TAMA data analysis (5)- Other activities -
  • Continuous-wave analysis

K.Soida et al.,

Class. Quantum Grav. 20 (2003) S645

Target:

Possible pulsar at SN1987A remnant

Sinusoidal wave

without precise freq. information

Schemes:

Matched filtering

(Heterodyne detection)

DT8-9 analysis in progress…

Characterization

In this workshop …

S.Telada (Thu. AM): Calibration in time domain

N.Kanda (Thu. AM): Effect of correlation of

two detectors in LCGT

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

summary
Summary

TAMA detector

Data Taking 9

Improve the sensitivity by a factor of 2

observable range 72kpc for 1.4Mo binaries

Automated stable operation

Noise investigation with RMI

Preparation for TAMA-SAS installation

Data analysis

Inspiral, burst, and ringdown searches

results are being obtained

LIGO-TAMA coincidence analyses

Some activities on data analysis:

Continuous wave search

Waveform estimation

Detector correlations

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

slide25
End

The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

ad