japanese gravitational wave detectors: lcgt and decigo frontiers in optics 2009 laser science xxv...
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![Page 1: Japanese Gravitational Wave Detectors: LCGT and DECIGO Frontiers in Optics 2009 Laser Science XXV Oct. 13, 2009 San Jose, USA Seiji Kawamura (NAOJ), LCGT](https://reader035.vdocuments.mx/reader035/viewer/2022062221/56649e265503460f94b16479/html5/thumbnails/1.jpg)
Japanese Gravitational Wave Detectors:
LCGT and DECIGO
Frontiers in Optics 2009Laser Science XXV
Oct. 13, 2009San Jose, USA
Seiji Kawamura (NAOJ),LCGT Collaboration, DECIGO Working Group
Sora
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Outline
Roadmap Ground-based detector
TAMA300CLIOLCGT
Space antennaDECIGODECIGO Pathfinder
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Roadmap ofthe Japanese GW detection
2000
01 02 03 04 05 06 07 08 09 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28
Ground-
based
▲ ▲ ▲
Space
▲ ▲ ▲
TAMA
CLIOLCGT
DECIGO Pathfinder Pre-DECIGO DECIGO
R&D
Advanced LCGT
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Ground-based Detector
TAMA300 CLIO LCGT
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5
TAMA300 300 m power-recycled FP
Michelson interferometer located on the NAOJ
campus in Tokyo Project started 1995 Best sensitivity in world
2000-2002
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6
New Seismic Attenuation System
Joint development with LIGO (Riccardo DeSalvo et al.) based on earlier Virgo concept
Photo: Nikon
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100 m cryogenic prototype
Differential FP interferometer
located in the Kamioka mine in Gifu
TAMA300
CLIO
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Ground motion in Kamioka mine
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Sensitivity of CLIO
Frequency
Dis
plac
emen
t no
ise
1/√
Hz
Mirror suspension thermal noise--inversely proportional to f 2.5
Mirror thermal noise
Thermal noise limit by eddy current damping between actuator magnets and metal solenoid holder--inversely proportional to f 2
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3km Underground at Kamioka Cryogenic mirrors
LCGT
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Goal Sensitivity of LCGT
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Detection range of LCGT
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LCGT in network
L/H+L/L+V 50% L/H+L/L+V+LCGT 50%
B. F. Schutz
LIGO(H)+LIGO(L)+Virgo
Coverage at 0.5 M.S.: 72% 3 detector duty cycle: 51%
LIGO(H)+LIGO(L)+Virgo+LCGT Max sensitivity (M.S.): +13% Coverage at 0.5 M.S.: 100% 3 detector duty cycle: 82%
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OrganizationLCGT: hosted by ICRR under MOU with NAOJ and KEK. LCGT collaboration: 118 members (92 domestic, 26 oversea members)
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Funding Status
Proposal for the 2010 start did not go through.
We will submit a proposal for the 2011 start.
Application for the stimulus fund was turned down.
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What is DECIGO?Deci-hertz Interferometer Gravitational Wave Observatory
(Kawamura, et al., CQG 23 (2006) S125-S131) Bridges the gap between LISA and terrestrial detectors Low confusion noise -> Extremely high sensitivity
10-18
10-24
10-22
10-20
10-4 10410210010-2
Frequency [Hz]
Str
ain
[H
z-1/2]
LISA
DECIGO
Terrestrial detectors (e.g. LCGT)
Confusion Noise
moved above
LISA band To be moved
into TD band
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Pre-conceptual designDifferential FP interferometer
Arm length: 1000 kmMirror diameter: 1 mLaser wavelength : 0.532 mFinesse: 10Laser power: 10 WMirror mass: 100 kgS/C: drag free3 interferometers
Laser
Photo-detector
Arm cavity
Drag-free S/C
Arm cavity
Mirror
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Why FP cavity?
Frequency
Str
ain
Radiation pressure
noise f -2
Shot noiseShot n
oise
f1Transponder type(e.g. LISA)
Shot noise
Shortenarm length
Shot nois
e f1
Radiation pressure
noise f -2
Transponder type(e.g. LISA) Shorten
arm length Implement FP cavity
Implement FP cavity
FP cavity type Better best- sensitivity
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Drag free and FP cavity: compatible?
Mirror
S/C IS/C II
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FP cavity and drag free : compatible?
Local sensor
ThrusterThruster
Mirror
Relative position between mirror
and S/C
S/C II S/C I
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Drag free and FP cavity: compatible?
Local sensor
ThrusterThruster
Mirror
Relative position between mirror
and S/C
Actuator
Interferometer output (GW signal)
S/C II S/C I
No signalmixture
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Orbit and constellation (preliminary)
Sun
Earth
Record disk
Increase angular resolution
Correlation for stochastic background
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Inflation
Formation of super-
massive BH
Verification of inflation
Science by DECIGO
Frequency [Hz]
Correlation(3 years)
Str
ain
[H
z-1/ 2]
10-3 10-2 10-1 1 10 102 103
10-19
10-20
10-21
10-22
10-23
10-24
10-25
10-26
(1000 M◎ z=1)
BH binary
Coalescence
5 years
NS binary (z=1)
Coalescence
3 months
Acceleration of Universe
Dark energy
Radiation pressure noise
Shot noise
1 unit
Mini-black hole
Dark matter
Brans Dickeparameter
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Requirements
Force noise of DECIGO should be 50 times more stringent than LISAAcceleration noise in terms of h: comparableDistance: 1/5000Mass: 100
Sensor noise of DECIGO should be10 times looser than LCGTSensor noise in terms of h: comparable,Storage time: 10
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Roadmap2009 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29
Mission
Objectives
Test of key technologies
Detection of GW w/ minimum spec.Test FP cavity between S/C
Full GW astronomy
Scope
1 S/C1 arm
3 S/C1 interferometer
3 S/C,3 interferometer3 or 4 units
DICIGO Pathfinder (DPF)
Pre-DECIGODECIGO
R&DFabrication
R&DFabrication
R&DFabrication
SWIM
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DEDCIGO Pathfinder (DPF)
Local Sensor
Actuator
Thruster
Single satellite Earth orbit Altitude: 500km Sun synchronous
Arm length: 1000 kmArm length: 30 cm
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conceptual design and objectives of DPF
ThrusterLocal
Sensor
Floating mirrorIodine cell
Laser
Actuator
Test of drag-free system
Test of locking system in space
Test of laser in space
Test of frequency stabilization
system in space
Observation of GW at 0.1 – 1 Hz
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Payload and standard bus
Stabilized. Laser source
Interferometer module
Satellite Bus system
Solar Paddle
MissionThruster head
On-boardComputer
Bus thruster
Mast structure
Satellite Bus (‘Standard bus’ system)
DPF PayloadSize : 950mm cubeWeight : 150kgPower : 130WData Rate: 800kbpsMission thruster x12
Power SupplySpW Comm.
Size : 950x950x1100mmWeight : 200kgSAP : 960W Battery: 50AHDownlink : 2MpbsDR: 1GByte3N Thrusters x 4
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Goal sensitivity of DPF
10–2 10–1 100 101 10210–18
10–17
10–16
10–15
10–14
10–13
10–12
10–11
10–19
10–18
10–17
10–16
10–15
10–14
10–13
10–12
No
ise
leve
l
[1/H
z1/2 ]
Frequency [Hz]
Shot noise
Mirror thermal
Laser Radiation
Laser: 1064nm, 25mWFinesse: 100Mirror mass: 1kgQ–value of a mirror: 106
Cavity length: 10cm
pressure noise
Thruster noise
PM acceleration Noise
Geogravity
Laser Frequencynoise
Dis
pla
cem
ent
No
ise
[m
/Hz1/
2 ]
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Detection range
103 104 105 10610–1
100
101
102
Ob
serv
able
Ran
ge
Mass [Msolar]
[kp
c,
SN
R=
5]
Galactic Center
BH QNM
BH Inspiral
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R&D for Subsystems
Frequency-stabilized laser
ThrusterInterferometric sensor
Drag-freemodel
Electrostatic sensor/actuator
Test mass module
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SWIM launch and operationTiny GW detector module Launched in Jan. 23, 2009
Test mass
Photo sensor
Coil
TAM: Torsion Antenna Module with free-falling test mass (Size : 80mm cube, Weight : ~500g)
Reflective-type optical displacement sensorSeparation to mass ~1mmSensitivity ~ 10-9 m/Hz1/2
6 PSs to monitor mass motion
~47g Aluminum, Surface polishedSmall magnets for position control
Photo: JAXA
In-orbit operation
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Interim organizationPI: Kawamura (NAOJ)Deputy: Ando (Tokyo)
Executive CommitteeKawamura (NAOJ), Ando (Tokyo), Seto (NAOJ), Nakamura (Kyoto),
Tsubono (Tokyo), Tanaka (Kyoto), Funaki (ISAS), Numata (Maryland), Sato (Hosei), Kanda (Osaka city), Takashima (ISAS), Ioka (Kyoto)
Pre-DECIGO
Sato (Hosei)
Satellite
Funaki (ISAS)
Science, Data
Tanaka (Kyoto)Seto (NAOJ)
Kanda (Osaka city)
DECIGO pathfinderLeader: Ando (Tokyo)
Deputy: Takashima (ISAS)
Detector
Ueda (NAOJ)
Housing
Sato (Hosei)
Laser
Ueda (ILS)Musya (ILS)
Drag free
Moriwaki (Tokyo)Sakai (ISAS)
Thruster
Funaki (ISAS)
Bus
Takashima (ISAS)
Data
Kanda (Osaka
city)
Detector
Numata (Maryland)
Ando (Tokyo)
Mission phase
Design phase
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Collaborations LISA
1st LISA-DECIGO workshop held in JAXA/ISAS (Nov. 2008)
Stanford Univ. Charge control using UV LED, etc. ⇒ MOU
NASA Goddard Fiber laser ⇒ started discussion
JAXA formation flight group Formation flight
Big bang center of the Univ. of Tokyo DECIGO adopted as one of the main themes
Advanced technology center of NAOJ Will make it a main nucleus of DPF
UNISEC (University Space Engineering Consortium) Started discussion
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Funding Status
Proceeded to the final hearing as one of the two candidates for the 2nd small science satellite run by JAXA/ISAS (launching three missions between 2012 and 2016), but not selected.
We will apply for the 3rd mission. (The selection will take place in 2010.)
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Conclusions
We need LCGT and DPF funded as soon as possible to establish the GW astronomy in the future!