Transcript スライド 1 - TAMA 300

Sora
LISA8 @Stanford Univ. USA
June 29, 2010
Seiji Kawamura, Masaki Ando, Naoki Seto, Shuichi Sato, Ikkoh Funaki, Takashi Nakamura, Kimio Tsubono, Jun'ichi Yokoyama, Kenji Numata,
Nobuyuki Kanda, Takeshi Takashima, Takahiro Tanaka, Kunihito Ioka, Kazuhiro Agatsuma, Tomotada Akutsu, Koh-suke Aoyanagi, Koji Arai, Akito
Araya, Hideki Asada, Yoichi Aso, Takeshi Chiba, Toshikazu Ebisuzaki, Yumiko Ejiri, Motohiro Enoki, Yoshiharu Eriguchi, Masa-Katsu Fujimoto,
Ryuichi Fujita, Mitsuhiro Fukushima, Toshifumi Futamase, Tomohiro Harada, Tatsuaki Hashimoto, Kazuhiro Hayama, Wataru Hikida, Yoshiaki
Himemoto, Hisashi Hirabayashi, Takashi Hiramatsu, Feng-Lei Hong, Hideyuki Horisawa, Mizuhiko Hosokawa, Kiyotomo Ichiki, Takeshi Ikegami, Kaiki
T. Inoue, Koji Ishidoshiro, Hideki Ishihara, Takehiko Ishikawa, Hideharu Ishizaki, Hiroyuki Ito, Yousuke Itoh, Kiwamu Izumi, Isao Kawano, Nobuki
Kawashima, Fumiko Kawazoe, Naoko Kishimoto, Kenta Kiuchi, Shiho Kobayashi, Kazunori Kohri, Hiroyuki Koizumi, Yasufumi Kojima, Keiko
Kokeyama, Wataru Kokuyama, Kei Kotake, Yoshihide Kozai, Hiroo Kunimori, Hitoshi Kuninaka, Kazuaki Kuroda, Kei-ichi Maeda, Hideo Matsuhara,
Nobuyuki Matsumoto, Yuta Michimura, Yasushi Mino, Osamu Miyakawa, Umpei Miyamoto, Shinji Miyoki, Mutsuko Y. Morimoto, Toshiyuki Morisawa,
Shigenori Moriwaki, Shinji Mukohyama, Mitsuru Musha, Shigeo Nagano, Isao Naito, Kouji Nakamura, Hiroyuki Nakano, Kenichi Nakao, Shinichi
Nakasuka, Yoshinori Nakayama, Kazuhiro Nakazawa, Erina Nishida, Kazutaka Nishiyama, Atsushi Nishizawa, Yoshito Niwa, Taiga Noumi, Yoshiyuki
Obuchi, Masatake Ohashi, Naoko Ohishi, Masashi Ohkawa, Kenshi Okada, Norio Okada, Kenichi Oohara, Norichika Sago, Motoyuki Saijo, Ryo Saito,
Masaaki Sakagami, Shin-ichiro Sakai, Shihori Sakata, Misao Sasaki, Takashi Sato, Masaru Shibata, Hisaaki Shinkai, Ayaka Shoda, Kentaro Somiya,
Hajime Sotani, Naoshi Sugiyama, Yudai Suwa, Rieko Suzuki, Hideyuki Tagoshi, Fuminobu Takahashi, Kakeru Takahashi, Keitaro Takahashi, Ryutaro
Takahashi, Ryuichi Takahashi, Tadayuki Takahashi, Hirotaka Takahashi, Takamori Akiteru, Tadashi Takano, Nobuyuki Tanaka, Keisuke Taniguchi,
Atsushi Taruya, Hiroyuki Tashiro, Yasuo Torii, Morio Toyoshima, Shinji Tsujikawa, Yoshiki Tsunesada, Akitoshi Ueda, Ken-ichi Ueda, Masayoshi
Utashima, Kent Yagi, Hiroshi Yamakawa, Kazuhiro Yamamoto, Toshitaka Yamazaki, Chul-Moon Yoo, Shijun Yoshida, Taizoh Yoshino, Ke-Xun Sun
Outline
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


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Japanese GW Roadmap
DECIGO
Roadmap to DECIGO
DECIGO Pathfinder, etc.
Organization, Collaboration, etc.
Summary
Japanese Roadmap
to GW Astronomy
DECIGO
LCGT
Detecting GW
(International network)
Opening a new window
(after LISA)
LCGT: $110M for 3 years approved!
(Thanks to support from international GW community)
What is DECIGO?
Deci-hertz Interferometer Gravitational Wave Observatory
 Bridges the gap between LISA and ground-based detectors
 Low confusion noise -> Extremely high sensitivity
Strain [Hz-1/2]
10-18
10-20
LISA
Ground-based
detectors
DECIGO
10-22 Confusion
Noise
10-24
10-4
10-2
100
102
Frequency [Hz]
104
Pre-conceptual design
Differential FP interferometer
Arm length: 1000 km
Mirror diameter: 1 m
Laser wavelength：0.532 m
Finesse: 10
Laser power: 10 W
Mirror mass: 100 kg
S/C: drag free
3 interferometers
Arm cavity
Arm cavity
Laser
Photodetector
Drag-free S/C
Mirror
Transponder type
Why FP cavity?
Shorten
arm length
Implement FP cavity
Strain
Shorten
arm length
Shot noise
Shot noise
Transponder type
More stringent
acceleration noise
requirement
Implement FP cavity
FP cavity type
Frequency
Better shotnoise-limited
sensitivity
Drag free and FP cavity:
compatible?
Solar radiation
pressure, etc
Solar radiation
pressure, etc
S/C II
1,000 km
S/C I
Mirror
Gravity force
Gravity force
Gravity force
Gravity force
FP cavity and drag free :
compatible?
Relative position
between mirror
and S/C
S/C II
Local
sensor
S/C I
Mirror
Thruster
Thruster
Gravity force
Gravity force
Drag free and FP cavity:
compatible?
Relative position
between mirror
and S/C
S/C II
Local
sensor
No signal
mixture
S/C I
Mirror
Thruster
Thruster
Actuator Gravity force
Interferometer
output (GW signal)
Orbit and constellation
(preliminary)
Earth
Correlation
for stochastic
background
Record disk
Sun
Increase angular
resolution
Science by DECIGO
Mini-black
hole

Dark matter
10-19
Formation of 10-20
supermassive BH 10-21
Coalescence
Brans Dicke
parameter
5 years
1 cluster
3 months
10-22
10-23
10-24
10-25
Shot noise
Correlation
(3 years)
Inflation
Coalescence
-16
(GW~2×10 )
Verification
of inflation 10-26
10-3
10-2
10-1
1
10
Frequency [Hz]
102
103
Acceleration
of Universe

Dark energy
Requirements

Force noise of DECIGO should be 50
times more stringent than LISA
– Acceleration noise in terms of h:
comparable
– Distance: 1/5000
– Mass: 100

Sensor noise of DECIGO should be10
times looser than LCGT
– Sensor noise in terms of h: comparable,
– Storage time: 10
Conceptual Design of DECIGO

Optimize the design parameters to
improve the sensitivity for the effective
cleaning of the foreground
– arm length, mirror diameter, mirror mass,
laser power, finesse, etc.
– Lead by Tomotada Akutsu

Establish the design to realize the
required performances
– proof mass, mirror curvature, local
sensor/actuator, frequency stabilization
Roadmap
2009 10
11
12 13
14
15 16
17 18 19 20 21
Mission
R&D
Fabrication
R&D
Fabrication
22 23 24
25
26 27 28 29
R&D
Fabrication
Pre-DECIGO
DICIGO Pathfinder
SWIM
Masaki Ando’s talk on Thursday
 Wataru Kokuyama’s poster
DECIGO
Objectives
Test of key technologies
Detection of GW
w/ minimum spec.
Test FP cavity
between S/C
Full GW
astronomy
Scope
1 S/C
1 arm
3 S/C
1 interferometer
3 S/C,
3 interferometer
3 or 4 units
DECIGO Pathfinder (DPF)
Single satellite
 Earth orbit
 Altitude: 500km
 Sun synchronous

Thruster
Local Sensor
Actuator
Arm length: 1000 km
Arm length: 30 cm
JAXA’s Small Science
Satellite Series

Plan to launch 3 small satellites between
2011 and 2015
– using next-generation solid rocket booster

Reduce time and cost by “Standard bus
system”
– Bus weight : 200kg, Bus power : 800W
– 3-axes attitude control
– SpaceWire-based data processing system
DECIGO Pathfinder
DPF Payload
Size :
950mm cube
Weight : 150kg
Power :
130W
Data Rate: 800kbps
Mission thruster x12
Mission
Thruster head
Stabilized.
Laser source
On-board
Computer
Power Supply
SpW Comm.
Satellite Bus
(‘Standard bus’ system)
Size :
950x950x1100mm
Weight : 200kg
SAP :
960W
Battery: 50AH
Downlink : 2Mpbs
DR:
1GByte
3N Thrusters x 4
Interferometer
module
Satellite
Bus system
Bus thruster
Solar Paddle
DPF Payload
Mission weight : ~150kg
Mission space : ~95 x 95 x 90 cm
Thruster
Laser source
Yb:YAG laser (1030nm)
Power : 25mW
Freq. stab. by Iodine abs. line
Drag-free control
Local sensor signal
 Feedback to thrusters
Fabry-Perot interferometer
Finesse : 100
Length : 30cm
Test mass : ~1kg
Signal extraction by PDH
–13
10
]
1/2
PM
ac
og
Ge
–14
10
–15
ler
–16
10
at
io
n
s
ru
Th
10
ter
–17
no
10
–2
10
–1
10
–13
10
–14
10
6
–15
10
–16
No
Laser
Frequency
10
is
La
se e
noise
–17
r
pr R
10
es ad
Shot noise
su iat
–18
re ion
M
i
r
10
r
o
no
r therm
al
ise
–19
10
0
1
2
10
10
10
ise
–18
10
ce
ity
rav
Noise level [1/Hz
Cavity length: 10cm
Laser: 1064nm, 25mW
Finesse: 100
Mirror mass: 1kg
Q–value of a mirror: 10
–12
10
Frequency [Hz]
1/2
–12
10
Displacement Noise [m/Hz
–11
10
]
Goal sensitivity of DPF
[kpc, SNR=5]
Observable Range
Detection range
2
10
BH QNM
BH Inspiral
1
10
Galactic Center
0
10
–1
10
3
10
4
10
5
10
Mass [M solar]
6
10
Gravity of the Earth
 Ayaka Shoda’s poster
Measure gravity field of the Earth
from Satellite Orbits, and gravity-gradiometer
GPS satellite
Determine global gravity field
 Density distribution
Monitor of change in time
Ground water motion
Strains in crusts by
earthquakes and volcanoes
Observation Gap
between GRACE and GRACE-FO
(2012-16)
 DPF contribution
in international network
By Araya and Fukuda
R&D for Subsystems
 Shuichi Sato’s talk on Thursday, Yuta Michimura’s talk on Thursday
Test mass module
Frequency-stabilized
laser
Electrostatic sensor/
actuator
Drag-free
model
Interferometric sensor
Thruster
Funding Status


Advanced to the final hearing as one of
the two candidates for the 2nd small
science satellite mission, but not
selected.
We will apply for the 3rd mission in
2011 (sometime after April).
SWIM
Tiny GW detector module
Launched in Jan. 23, 2009
In-orbit operation
TAM: Torsion Antenna Module with free-falling test mass
(Size : 80mm cube, Weight : ~500g)
Test mass
~47g Aluminum, Surface polished
Small magnets for position control
Photo：
JAXA
Coil
Photo sensor
Reflective-type optical
displacement sensor
Separation to mass ~1mm
Sensitivity ~ 10-9 m/Hz1/2
6 PSs to monitor mass motion
Pre-DECIGO
PreDECIGO
DECIGO
Arm length
100 km
1000 km
Mirror diameter
30 cm
1m
Laser wavelength
0.532 m
0.532 m
Finesse
30
10
Laser power
1W
10 W
Mirror mass
30 kg
100 kg
# of
1
interferometers in
each cluster
3
# of clusters
4
1
Sensitivity of Pre-DECIGO
S/N~14 for NS-NS@300Mpc, 10-20 events/year
-15
10
Strain sensitivity [1/rHz]
-16
10
DPF
-17
10
-18
10
pre-DECIGO
-19
10
-20
10
NS-NS inspiral (@300Mpc)
-21
10
-22
10
-23
10
DECIGO
-24
10
-3
10
-2
10
-1
10
0
10
1
10
Frequency [Hz]
2
10
3
10
Pre-DECIGO
• Science goal of Pre-DECIGO should
be defined (with peter Bender’s
suggestion: formation of galaxies)
– Lead by Shuichi Sato
• Optimize the design of Pre-DECIGO
both for the science goal and
technology goal
DECIGO Interim Organization
PI: Kawamura (NAOJ)
Deputy: Ando (Kyoto)
Executive Committee
Kawamura (NAOJ), Ando (Kyoto), Seto (kyoto), Nakamura (Kyoto),Tsubono
(Tokyo), Sato (Hosei), Tanaka (Kyoto), Funaki (JAXA/ISAS),Numata (Maryland),
Kanda (Osaka City), Ioka (KEK), Takashima (JAXA/ISAS), Yokoyama (Tokyo)
Pre-DECIGO
Detector
Sato (Hosei)
Akutsu (NAOJ)
Numata (Maryland)
Science & Data
Tanaka (Kyoto)
Seto (Kyoto)
Kanda (Osaka City)
Spacecraft
Funaki (JAXA/ISAS)
Design Phase
DECIGO Pathfinder
Mission Phase
Leader: Ando (Kyoto)
Laser
Detector
A. Ueda (NAOJ)
K. Ueda (E.C.)
Musha (E.C.)
Housing
Sato (Hosei)
Drag-free
Moriwaki
(Tokyo)
Sakai
(JAXA/ISAS)
Thruster
Bus
Data
Funaki
(JAXA/ISAS)
Takashima
(JAXA/ISAS)
Kanda
(Osaka City)
1st International
LISA-DECIGO Workshop
• Nov. 12-13, 2008 @ ISAS, Sagamihara, Japan
• Participants:
– Danzmann, Heinzel, Gianolio, Jennrich, Lobo,
McNamara, Mueller, Prince, Stebbins, Sun, Vitale, …
• Accomplishments:
– Mutual understanding
– Exposure of the missions to people in the
neighboring fields
• We are grateful for the strong support from the
LISA community
Collaboration with Stanford
• MOU for the collaboration
– UV LED discharge for DPF/DECIGO
– Other R&D for DECIGO
• We appreciate the great help from
the Stanford team (Ke-Xun Sun, Bob
Byer, Dan DeBra, …)
Other Collaborations

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
– Discussing the possibility of its becoming the nucleus of DPF

NASA Goddard
– Fiber laser ⇒ started discussion

UNISEC (University Space Engineering Consortium)
– Started discussion
Conclusions


DECIGO will bring us a variety of
fruitful science.
The first step to realize DECIGO is to
have DPF approved!