decigo : the japanese space gravitational wave antenna
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DECIGO : the Japanese Space Gravitational Wave Antenna. Illustration/ KAGAYA. - PowerPoint PPT PresentationTRANSCRIPT
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
DECIGO :DECIGO : the Japanese Space Gravitational Wave the Japanese Space Gravitational Wave AntennaAntenna
Seiji Kawamura, Takashi Nakamura, Masaki Ando, Kimio Tsubono, Naoki Seto, Kenji Numata, Takahiro Tanaka, Kazuhiro Agatsuma, Tomotada Akutsu, Koh-suke Aoyanagi, Koji Arai, Akito Araya, Hideki Asada, Yoichi Aso, Takeshi Chiba, Toshikazu Ebisuzaki, Motohiro Enoki, Yoshiharu Eriguchi, Masa-Katsu Fujimoto, Mitsuhiro Fukushima, Toshifumi Futamase, Katsuhiko Ganzu, Tomohiro Harada, Tomohiro Harada, Tatsuaki Hashimoto, Kazuhiro Hayama, Wataru Hikida, Yoshiaki Himemoto, Hisashi Hirabayashi, Takashi Hiramatsu, Mizuhiko Hosokawa, Kiyotomo Ichiki, Takeshi Ikegami, Kaiki T. Inoue, Kunihito Ioka, Koji Ishidoshiro, Takehiko Ishikawa, Hiroyuki Ito, Yousuke Itoh, Shogo Kamagasako, Nobuyuki Kanda, Nobuki Kawashima, Hiroyuki Kirihara, Kenta Kiuchi, Werner Klaus, Shiho Kobayashi, Kazunori Kohri, Yasufumi Kojima, Keiko Kokeyama, Yoshihide Kozai, Hideaki Kudoh, Hiroo Kunimori, Kazuaki Kuroda, Kei-ichi Maeda, Hideo Matsuhara, Yasushi Mino, Jun-ichi Miura, Osamu Miyakawa, Shinji Miyoki, Mutsuko Y. Morimoto, Tomoko Morioka, Toshiyuki Morisawa, Shigenori Moriwaki, Shinji Mukohyama, Mitsuru Musha, Shigeo Nagano, Isao Naito, Noriyasu Nakagawa, Kouji Nakamura, Hiroyuki Nakano, Kenichi Nakao, Shinichi Nakasuka, Erina Nishida, Atsushi Nishizawa, Yoshito Niwa, Masatake Ohashi, Naoko Ohishi, Masashi Ohkawa, Akira Okutomi, Kenichi Oohara, Norichika Sago, Motoyuki Saijo, Masaaki Sakagami, Shin-ichiro Sakai, Shihori Sakata, Misao Sasaki, Shuichi Sato, Takashi Sato, Masaru Shibata, Hisaaki Shinkai, Kentaro Somiya, Hajime Sotani, Naoshi Sugiyama, Hideyuki Tagoshi, Tadayuki Takahashi, Ryutaro Takahashi, Ryuichi Takahashi, Hirotaka Takahashi, Takamori Akiteru, Tadashi Takano, Keisuke Taniguchi, Atsushi Taruya, Hiroyuki Tashiro, Masao Tokunari, Morio Toyoshima, Shinji Tsujikawa, Yoshiki Tsunesada, Ken-ichi Ueda, Kazuhiro Yamamoto, Toshitaka Yamazaki, Jun'ichi Yokoyama, Chul-Moon Yoo, Shijun Yoshida, Taizoh Yoshino
Illustration/ KAGAYA
Masaki AndoMasaki Ando(Department of Physics,
the University of Tokyo)
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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ContentsContents
Introduction
Pre-conceptual Design
Science
Roadmap and R&D
Summary
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Gravity Gradient noise (Terrestrial Detectors)
Confusion noise by Galactic binaries
10–4 10–2 100 102 104
10–26
10–24
10–22
10–20
10–18
10–16
Frequency [Hz]
Str
ain
[1
/Hz1
/2]
IntroductionIntroduction
DECIGO Deci-hertz Interferometer Gravitational Wave Observatorybridges the gap between LISA and terrestrial detectors
LCGT, Ad-LIGO
Primordial Background GW (gw=10-14)
MBH Coalescence
Resolved Galactic binary
LISA
LIGO
Stellar-core Collapse
NS-NS binary Inspiral
ScoX-1 (1yr)
Pulsar (1yr)
DECIGO
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Pre-conceptual Design (1)Pre-conceptual Design (1)
Pre-conceptual Design FP-Michelson interferometer
Arm length: 1000 km Finesse: 10
Laser Power: 10 W Wavelength: 532 nm
Mirror (Test mass) Diameter: 1 m Mass: 100 kg Shielded by S/C
Orbit and constellation: TBD
Laser
Drag-free satellite
Arm cavity
Arm cavity
Drag-free satellite Drag-free satellite
PD
PD
S. Kawamura, et al., CQG 23 (2006) S125-S131
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Pre-conceptual Design (2)Pre-conceptual Design (2)
SensitivityFloor level : 2x10-24 /Hz1/2 (0.1 - 10Hz)
10–4 10–3 10–2 10–1 100 101 102 10310–25
10–24
10–23
10–22
10–21
10–20
10–19
10–18
Frequency [Hz]
Str
ain
[
1/H
z1/2]
LCGT
LISA
DECIGO(FP type, 1000km)
Laser: 10W, 532nmMass: 100kgMirror: 1m dia.
Noise sources Low freq.: Acceleration noise, Radiation pressure noise High freq.: Shot noise (7.5Hz cut-off freq. )
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Pre-conceptual Design (3)Pre-conceptual Design (3)
Interferometer DesignTransponder type vs Direct-reflection type Compare: Sensitivity curve and Expected Science Same detector parameters (Mirror, Laser, etc.)
10–4 10–3 10–2 10–1 100 101 102 10310–25
10–24
10–23
10–22
10–21
10–20
10–19
10–18
Frequency [Hz]
Str
ain
[
1/H
z1/2]
LCGT
LISA
DECIGO(LISA type, 5x104km)
DECIGO(FP type, 1000km)
Laser: 10W, 532nmMass: 100kgMirror: 1m dia.
WD-W
D
confusion
noise
Decisive factor: Binary confusion noise
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Pre-conceptual Design (4)Pre-conceptual Design (4)
Arm lengthCavity arm length : Limited by diffraction loss
Calculate Effective reflectivity (TEM00 TEM00)
Laser wavelength : 532nm, Mirror diameter: 1m Optimal beam size
101 102 103 104 105 106 107 108 109 101010–4
10–3
10–2
10–1
100
Arm Length [m]
Ra
tio
of
av
aila
ble
po
we
r
LISALCGTTAMA DECIGO Dif
fra
cti
on
Lo
ss
(5x109m)(3x103m)(300 m)
Mirror diameter : 1mOptimal beam profile
(1x106m)
Nd:YAG laser : 532nm
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Pre-conceptual Design (5)Pre-conceptual Design (5)
Requirements
Practical force noise: 4x10-17 N/Hz1/2 per mirror (Mirror mass: 100kg)
Frequency Noise (at 1 Hz) First-stage stabilization : 1 Hz/Hz1/2
Stabilization gain by common-mode arm length : 105
Common-mode rejection ratio : 105
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Pre-conceptual Design (6)Pre-conceptual Design (6)
Cavity and S/C control
Local Sensor
Actuator
Displacement signal between the two Mirrors
Thruster Thruster
Displacement Signal between S/C and Mirror
Mirror
S/C 1 S/C 2
Fig: S. Kawamura
Cavity length change PDH error signal Mirror position (and Laser frequency)Relative motion between mirror and S/C Local sensor S/C thruster
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Pre-conceptual Design (7)Pre-conceptual Design (7)
S/C thruster force
0 12 24 36 48 60–40
–30
–20
–10
0
10
20
30
40
Le
ng
th C
ha
ng
e [
km
]
Time [month]
S/C orbit : TBD
(ex) Similar orbit as that of LISA Numerical simulation of multi-bode system Include gravity of planets Arm length: 1000km Earth-like orbit, 20deg. Behind the earth
Length control is indispensableAcceleration to be controlled: ~4x10-12 m/s2
0 5 10 15 20 25 30–15
–10
–5
0
5
10
15
Le
ng
th C
ha
ng
e [
m]
Time [day]
Black curve: parabolic fitting
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Science by DECIGO (1)Science by DECIGO (1)
NS+NS@z=1
BH+BH(1000Msun)
@z=1
Correlationfor 3 years
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 (1000+1000Msun) z<1 (SN>6000)
Binary Inspiral
Fig: N. Seto
Extremely high rate for NS-NS inspirals
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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NS-NS (z ~1)
GW
DECIGO
Output
Expansion +Acceleration?
Time
Str
ai
n
Template (No Acceleration)
Real Signal ? Phase Delay ~ 1sec (10
years)Seto, Kawamura, Nakamura, PRL 87, 221103 (2001)
Acceleration of Expansion of the Universe
Science by DECIGO (2)Science by DECIGO (2)
Distant binary is a precise clock Monitor Doppler shift
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Distance – Red shift relationship for NS-NS binaries Constraint to dark energy
Distance: determined directly by GW observation
Red shift: determined by identifying the host galaxies (10 arcsec at z=1 for two far-separate DECIGOs)
Constraint to Dark Energy
Science by DECIGO (3)Science by DECIGO (3)
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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06 07 08 09 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24
06 07 08 09 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24
Design & Fabrication
Observation
R&D
Advanced R&D
PF1
DECIGO
Design & Fabrication
Observation
PF2
Roadmap to DECIGO
Roadmap and R&D (1)Roadmap and R&D (1)
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Local Sensor
ActuatorThruster
Single S/C with Test mass Laser interferometer Drag-free system
Objectives Drag-free system Cavity locking in space Modest sensitivity at 0.1 – 1
Hz GW observation
Details: TBD
DECIGO Pathfinder1
Roadmap and R&D (2)Roadmap and R&D (2)
Fig: S. Kawamura
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Laser
Drag-free satellite
Arm cavity
Arm cavity
Drag-free satellite
Drag-free satellite
PD
PD
DECIGO with modest specification
Objectives Cavity locking between two S/C Meaningful sensitivity GW observation
Details: TBD
DECIGO Pathfinder2
Roadmap and R&D (3)Roadmap and R&D (3)
Fig: S. Kawamura
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Clamp
TimeV
ert
ical
Posit
ion2
m
1 sec
Release Hold
Release Hold
Release Hold
Objectives
Continual free-fall environment
Clamp release
Modest sensitivity down to 0.1Hz
Possibility of long arm
DECIGO Simulator
Roadmap and R&D (4)Roadmap and R&D (4)
Fig: S. Kawamura
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Satellite A
Satellite B
Thruster Thruster
Actuator
Air-hockey table
Mirror A
Mirror B
Local sensor
Local sensor
Objectives
Lock acquisition
Drag-free control demonstration
DECIGO Demonstrator
Roadmap and R&D (5)Roadmap and R&D (5)
Fig: S. Kawamura
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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Budget request for “Frontier of All Wavelength Gravitational Wave Astronomy” submitted in 2005
- TAMA and CLIO- R&D for DECIGO- Pulsar Timing- Super-high frequency G.W. detection
Not approved to our surpriseTry again?
Budget
Roadmap and R&D (6)Roadmap and R&D (6)
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
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DECIGO will have an extremely good sensitivity
and open the GW window widely.
DECIGO requires
extremely challenging technology development.
We hope that we will be able to
start the R&D for DECIGO very soon.
SummarySummary
11th Marcel Grossmann Meeting on General Relativity (July 23 - 29, 2006, Freie Universität Berlin)
EndEnd