clio current status of japanese detectors daisuke tatsumi national astronomical observatory of japan
Post on 16-Dec-2015
220 Views
Preview:
TRANSCRIPT
CLIOCLIO
Current Status ofCurrent Status ofJapanese DetectorsJapanese Detectors
Daisuke TatsumiNational Astronomical Observatory of Japan
2
ContentsContents• 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 give a brief introduction to the current activities of data analysis.
3
The Japanese DetectorsThe Japanese DetectorsTwo prototype detectors for LCGT are being developed in Japan.
•TAMALocation: Suburb of Tokyo, Japan
Baseline length: 300m
•CLIOLocation: Kamioka underground site, Japan
Baseline length: 100mFeature: 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
TAMATAMA
Brief History1995 Construction start
1999 First observation experiment
2000 World best sensitivityat the time
2001 1000 hours Observation2002 Power recycling (PR)2003 Second 1000 hours
observation with PR2004 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 upgradeTAMA upgradeAfter the last observation experiment in 2004, TAMA detector is being upgraded to reduce the low frequency noises.
6
TAMA SAS TAMA SAS (Seismic Attenuation System)(Seismic Attenuation System)
TAMA-SAS(IP + GASF + Payload)
1. Horizontal Inverted Pendulum resonant freq. : 30mHz
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.
2. VerticalDouble MGAS FiltersEach of 0.5Hz resonance
3. PayloadTop mass (Platform) Intermediate massMirror - Recoil mass
7
SAS Installation ScheduleSAS Installation Schedule
12
3
4
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.
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 lockedwith SAS,
Oct: Third and forth SAS were installed to the perpendicular arm cavity (3), (4).
8
Stable lock ofStable lock of SAS Fabry-Perot cavity SAS Fabry-Perot cavity
TIME
Transmitted Power of
SAS FP cavity
Transmitted Power of
old suspension cavity
Locked FP configuration
Feedbacksignal
to Mirror
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
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.
Improvement of Improvement of cavity length fluctuation cavity length fluctuation
10
Improvement of Improvement of angular fluctuationsangular 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 configurationby the end of next July.
11
TAMA SummaryTAMA 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
CLIOCLIO CLIOCLIOCCryogenic ryogenic LLaser aser IInterferometer nterferometer OObservatorybservatory
in Kamioka minein Kamioka mine
13
CLIOCLIO
CLIO & LCGTCLIO & LCGTPurpose 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 Sapphire mirrors 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
CLIOCLIO
ConstructionConstruction
All of vacuum pipes, cryostats and cryocoolers were installed by the June, 2005.
15
CLIOCLIO First operation of First operation of the cryogenic interferometerthe cryogenic interferometer
First operation of the cryogenic interferometerhas been demonstrated on 18 February, 2006 !
This figure shows mirror temperatures as a function of time. During the lock, the mirrors keep its temperature around 20K.
20K
23K
Near Mirror
End Mirror
about 50 min. Lock
Tem
pera
ture
(K
)
16
CLIOCLIO
CLIO sensitivity at 300KCLIO sensitivity at 300K
10010 1k 10k
Frequency (Hz)
Dis
pla
cem
en
t (m
/rtH
z)
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 bestnoise spectrum of CLIO.At all of frequency regions, the differences from the target sensitivity at 300K are about a factor of 4.
Current Best
Target sensitivity at 300K
17
CLIOCLIO Observable ranges forObservable ranges forInspiral GW signalsInspiral GW signals
For neutron star binaries, CLIO and TAMA can observe the event within 49kpc and 73kpc, respectively.
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.
CLIO
TAMA
LISM
1.4Msolar
18
CLIOCLIO
CLIO SummaryCLIO 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 noise reaches at thermal noise level, its improvement by cooling will be demonstrated.
19
DECIGODECIGO DECDECi-hertz i-hertz IInterferometer nterferometer GGravitational Wave ravitational Wave OObservatorybservatory
Pre-conceptual DesignFP Michelson interferometerArm length: 1000 kmOrbit and constellation: TBD Laser: 532 nm, 10 WMirror: 1 m, 100 kgFinesse: 10
NS+NS@z=1
BH+BH(1000Msun )
@z=1
3 year-correlation
merger
merger10210-2 100
10-24
10-22
10-20
10-18
G
W = 2.210 -16
Laser
Drag-freesatellite
Arm cavity
Arm cavity
Drag-free satellite Drag-free satellite
PD
PD
Foreground
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)
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.
20
Activities of Data AnalysisActivities 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.
Period Data length [hours] Analyzed data [hours]
DT4 Sept. ‘00 154.9 147.1
DT5 Mar. ‘01 107.8 95.26
DT6 Aug.-Sept. ‘01 1049 876.6
DT8 Feb.-Apr. ‘03 1163 1100
DT9 Nov.’03-Jan.’04 556.9 486.1
2705
2462.8
Total length of data analyzed (DT 4,5,6,8,9)
Length of data for upper limit (DT 6,8,9)
We derived a 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)
Data length
[hours]
Detection probability of Galactic signals
Threshold of ζ
(false alarm rate = 1 /yr)
Upper limit to the Milky Way Galaxy events [events /yr] (C.L.=90%)
DT6 876.6 0.18 21.8 130
DT8 1100 0.60 13.7 30
DT9 486.1 0.69 17.7 60
0.042 0.031
0.045 0.070
0.056 0.032
0.049 0.073
0.035 0.028
0.029 0.056
8.0
4.6
4.9
4.6
59
29
Upper limit on the Galactic event rate
1 3Msolar
Single upper limit is given by
RNULiTi
i
Ti
R17 1.513.02 [yr -1]
Conservative upper limit
R20 [yr -1]
(gr-qc/0610064, PRD in press)
by using dataof 102.6 days
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
top related