the japanese space gravitational wave antenna - decigo
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The Japanese Space Gravitational Wave Antenna - DECIGO. Amaldi6 @Okinawa June 22, 2005 - PowerPoint PPT PresentationTRANSCRIPT
The Japanese Space Gravitational Wave Antenna - DECIGO
Amaldi6 @OkinawaJune 22, 2005
Seiji Kawamura, Takashi Nakamura, Masaki Ando, Kimio Tsubono, Naoki Seto, Shigeo Nagano, Takahiro Tanaka, Takehiko Ishikawa, Ken-ichi Ueda, Mitsuru Musha, Takashi Sato, Mizuhiko Hosokawa, Kenji Numata, Hisashi Hirabayashi, Tadashi Takano, Masa-Katsu Fujimoto, Atsushi Taruya, Yoshiaki Himemoto, Chul-Moon Yoo, Kenichi Nakao, Tomohiro Harada, Kunihito Ioka, Norichika Sago, Wataru Hikida, Shuichi Sato, Keiko Kokeyama, Mitsuhiro Fukushima, Hiroo Kunimori, Toshitaka Yamazaki, Masashi Ohkawa, Tatsuaki Hashimoto, Koh-suke Aoyanagi, Kazuhiro Agatsuma, Tomotada Akutsu, Hideki Asada, Yoichi Aso, Koji Arai, Akito Araya, Takeshi Ikegami, Koji Ishidoshiro, Kiyotomo Ichiki, Yousuke Itoh, Kaiki T. Inoue, Yoshiharu Eriguchi, Naoko Ohishi, Masatake Ohashi, Kenichi Oohara, Akira Okutomi, Shogo Kamagasako, Nobuki Kawashima, Mari Kawamura, Nobuyuki Kanda, Katsuhiko Ganzu, Kenta Kiuchi, Hideaki Kudoh, Kazuaki Kuroda, Kazunori Kohri, Yoshihide Kozai, Yasufumi Kojima, Shiho Kobayashi, Motoyuki Saijo, Masaaki Sakagami, Shihori Sakata, Misao Sasaki, Masaru Shibata, Hisaaki Shinkai, Naoshi Sugiyama, Hajime Sotani, Hirotaka Takahashi, Ryuichi Takahashi, Ryutaro Takahashi, Hideyuki Tagoshi, Hiroyuki Tashiro, Keisuke Taniguchi, Takeshi Chiba, Shinji Tsujikawa, Yoshiki Tsunesada, Masao Tokunari, Isao Naito, Hiroyuki Nakano, Kouji Nakamura, Atsushi Nishizawa, Yoshito Niwa, Choetsu Nozawa, Kazuhiro Hayama, Takashi Hiramatsu, Toshifumi Futamase, Kei-ichi Maeda, Hideo Matsuhara, Hiromi Mizusawa, Yasushi Mino, Osamu Miyakawa, Shinji Miyoki, Shinji Mukohyama, Toshiyuki Morisawa, Kazuhiro Yamamoto, Jun'ichi Yokoyama, Shijun Yoshida, and Taizoh Yoshino
Contents
1. What is DECIGO?2. Current Status3. Budget Situation4. Preliminary Experiment5. Summary
Gap between TerrestrialDetectors and LISA
10-
18
10-
24
10-
22
10-
20
10-
4
104
102
100
10-
2Frequency [Hz]
Str
ain
[H
z-1
/2]
LISA Terrestrial Detectors (e.g. LCGT)
Gap
DECIGO Bridges the Gap
10-
18
10-
24
10-
22
10-
20
10-
4
104
102
100
10-
2Frequency [Hz]
Str
ain
[H
z-1
/2]
LISA
DECIGO
Terrestrial Detectors (e.g. LCGT)
The Japanese Space Gravitational Wave Antenna - DECIGODeci-hertz Interferometer Gravitational Wave Observatory
Importance of Bridgingthe Gap
New window brings new science! Observe inspiral sources that have moved a
bove the LISA band Observe inspiral sources that have not yet
moved into the ground-based detector band Especially inspiral of IMBH Completely new sources could be detected Completely new science could be obtained
Acceleration of Expansion of the Universe
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)
DECIGO as a Future Gravitational Wave
Detection Project in Japan
TAMA
Near Future
NowPast
DECIGO
LCGT
Far Future
1st Priority
History of DECIGO1999 the LISA study group convened by Tsubono2000 Short-arm space antenna suggested by Kawam
ura2001 Space GW antenna WG convened as one of the
possible future projects in NAOJ2001 Named as DECIGO in the PRL paper by Seto,
Kawamura, Nakamura (DECIDE and GO)2002 1st DECIGO-WG meeting2003 2nd DECIGO-WG meeting
(FP-type DECIGO suggested by Ando)2005 3rd DECIGO-WG meeting
Roadmap for DECIGO06 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
Pre-Conceptual Designfor DECIGO
LISA-type DECIGO- Shorter arm length
Fabry-Perot-Cavity-type DECIGO- Even shorter arm length- Resonance of light in the cavity
For both types- Better shot noise (higher power, shorter wavelength, larger mirror)- Better force noise (heavier mass)
Fabry-Perot Type DECIGO
Drag-Free Satellite
Around Lagrange Point Fabry-Perot
cavity
Actuating Force in FP-DECIGO
Anti-Drag + Anti-Gravity +Anti-GW
Anti-Gravity +Anti-GW
Proof Mass
Outer Satellite
The distance should
be kept constant
Sensitivity of DECIGO
Force noise= 1/100 of LISA’s
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.
Preliminary Simulatorfor LISA-type DECIGO
Built a preliminary simulator for DECIGO as a simulator for detecting the Earth’s gravity field around the Earth
地球
Distance: 50 km
vMAX: 1 cm/s( Doppler Shift: 20 kH
z
Satellite 2Satellite 1
Schematic Diagram ofthe Preliminary Simulator
Simulate Doppler shift by AOD
Simulate distance by optical fiber
Lock to mid-fringe by AOD
Monitor FB to DDS
Stabilized Frequency using 5 layer shielded cavity (like LISA)
Sensitivity ofthe Preliminary Simulator
Budget Situation for DECIGO
and other GW Projects in JapanBudget request for “Frontier of
All Wavelength Gravitational Wave Astronomy” to be submitted this fall- TAMA and CLIO- R&D for DECIGO- Pulsar Timing- Super-high frequency G.W. detection
(Budget request for LCGT submitted this year from ICRR)
R&D for DECIGO
Overall Tests
Key Technologies
Ground-based DECIGO
Simulator(S. Kawamura, NAOJ)
DECIGO-Pathfinder (M. Ando, Univ. of Tokyo)
Measurement System
(K. Tsubono,Univ. of Tokyo)
Drag-freeSystem
(T. Ishikawa,
JAXA-ISAS)
Light Source
(K. Ueda, ILS)
Frequency Stabilizati
on(T. Sato,Niigata Univ.)
Evaluation of Light Source
(M. Hosokawa,
NICT)
Satellite Technologie
s(?, JAXA-
ISAS)
Objectives of the R&D
R&D of subsystemsOverall tests by ground-based
simulator and DECIGO-Pathfinder1R&D for optional technologiesDefining the objectives and
conceptual design of DECIGO-PF2Establishing the conceptual
design of DECIGO
Ground-Based Simulater
Laser
LF Pendulum
Seismic Isolation System Seismic Isolation System
Test the system on earth as much as possible Investigate the system at low frequencies Observe GW at low frequenciesLF Pendulum
Pathfinder Test the system which can be tested only in space (Drag-f
ree system) Check if the measurement system works in space Observe GW at low frequencies This effort couples with the JAXA-ISAS’s new satellite plan
Laser
Drag Free System
Measurement System
One Small Satellite
Resonated
Summary It is important to bridge the gap
between terrestrial detectors and LISA.
The Japanese space antenna DECIGO can bridge the gap.
We have started serious investigation of DECIGO.
We will submit a budget request for DECOGO R&D this fall.
We hope that we will be able to start the R&D for DECIGO soon.