the japanese space gravitational wave antenna - decigo
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The Japanese Space Gravitational Wave Antenna - DECIGO. Amaldi7 @Sydney, Australia July 12, 2007 - PowerPoint PPT PresentationTRANSCRIPT

The Japanese Space Gravitational Wave Antenna - DECIGO
Amaldi7 @Sydney, AustraliaJuly 12, 2007
Seiji KAWAMURA, Masaki ANDO, Takashi NAKAMURA, Kimio TSUBONO, Takahiro TANAKA, Ikkoh FUNAKI, Naoki SETO, Kenji NUMATA, Shuichi SATO, Kunihito IOKA, Nobuyuki KANDA, Takeshi TAKASHIMA, Kazuhiro AGATSUMA, Tomomi AKUTSU, Tomotada AKUTSU, Koh-suke AOYANAGI, Koji ARAI, Yuta ARASE, Akito ARAYA, Hideki ASADA, Yoichi ASO, Takeshi CHIBA, Toshikazu EBISUZAKI, Motohiro ENOKI, Yoshiharu ERIGUCHI, Feng-Lei HONG, Masa-Katsu FUJIMOTO, Ryuichi FUJITA, Mitsuhiro FUKUSHIMA, Toshifumi FUTAMASE, Katsuhiko GANZU, Tomohiro HARADA, Tatsuaki HASHIMOTO, Kazuhiro HAYAMA, Wataru HIKIDA, Yoshiaki HIMEMOTO, Hisashi HIRABAYASHI, Takashi HIRAMATSU, Hideyuki HORISAWA, Mizuhiko HOSOKAWA, Kiyotomo ICHIKI, Takeshi IKEGAMI, Kaiki T. INOUE, Koji ISHIDOSHIRO, Takehiko ISHIKAWA, Hideharu ISHIZAKI, Hiroyuki ITO, Yousuke ITOH, Shogo KAMAGASAKO, Nobuki KAWASHIMA, Fumiko KAWAZOE, Hiroyuki KIRIHARA, Naoko KISHIMOTO, Kenta KIUCHI, Werner KLAUS, Shiho KOBAYASHI, Kazunori KOHRI, Hiroyuki KOIZUMI, Yasufumi KOJIMA, Keiko KOKEYAMA, Wataru KOKUYAMA, Kei KOTAKE, Yoshihide KOZAI, Hideaki KUDOH, Hiroo KUNIMORI, Hitoshi KUNINAKA, 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, Yoshinori NAKAYAMA, Erina NISHIDA, Kazutaka NISHIYAMA, Atsushi NISHIZAWA, Yoshito NIWA, Masatake OHASHI, Naoko OHISHI, Masashi OHKAWA, Akira OKUTOMI, Kouji ONOZATO, Kenichi OOHARA, Norichika SAGO, Motoyuki SAIJO, Masaaki SAKAGAMI, Shin-ichiro SAKAI, Shihori SAKATA, Misao SASAKI, Takashi SATO, Masaru SHIBATA, Hisaaki SHINKAI, Kentaro SOMIYA, Hajime SOTANI, Naoshi SUGIYAMA, Yudai SUWA, Hideyuki TAGOSHI, Tadayuki TAKAHASHI, Ryutaro TAKAHASHI, Ryuichi TAKAHASHI, Kakeru TAKAHASHI, Hirotaka TAKAHASHI, Akiteru TAKAMORI, Tadashi TAKANO, Keisuke TANIGUCHI, Atsushi TARUYA, Hiroyuki TASHIRO, Mitsuru TOKUDA, Masao TOKUNARI, Morio TOYOSHIMA, Shinji TSUJIKAWA, Yoshiki TSUNESADA, Ken-ichi UEDA, Masayoshi UTASHIMA, Hiroshi YAMAKAWA, Kazuhiro YAMAMOTO, Toshitaka YAMAZAKI, Jun'ichi YOKOYAMA, Chul-Moon YOO, Shijun YOSHIDA, Taizoh YOSHINO

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

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

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

Drag free and FP cavity: compatible?
Mirror
S/C IS/C II

FP cavity and drag free : compatible?
Local sensor
ThrusterThruster
Mirror
Relative position between mirror
and S/C
S/C II S/C I

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

Orbit and constellation (preliminary)
Sun
Earth
Record disk
Increase angular resolution
Correlation for stochastic background

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

Requirements Acceleration noise should be suppressed below
radiation pressure noise– Force noise: DECIGO = LISA/50
(Acceleration noise in terms of h: 1, Distance: 1/5000, Mass: 100)
– Fluctuation of magnetic field, electric field, gravitational field, temperature, pressure, etc.
Sensor noise should be suppressed below shot noise.– Phase noise: DECIGO = LCGT×10
(Sensor noise in terms of h: 1, storage time: 10)– Frequency noise, intensity noise, beam jitter, etc.
Thruster system should satisfy range, noise, bandwidth, and durability.

Roadmap200
708 09 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26
Missio
nO
bjectives
Test of key technologies Detection of GW w/ minimum spec.Test FP cavity between S/C
Full GW astronomy
Sco
pe
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

Pre-conceptual design and objectives of DPF
ThrusterLocal
Sensor
Floating mirrorRigidCavity
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

Interim organizationPI: Kawamura (NAOJ)Deputy: Ando (Tokyo)
Executive CommitteeKawamura (NAOJ), Ando (Tokyo), Seto (NAOJ), Nakamura (Kyoto), Tsubono (Tokyo), Tanaka (Kyoto), Funaki (ISAS), Numata (Merryland), Sato
(NAOJ), Kanda (Osaka city), Takashima (ISAS), Ioka (Kyoto)
Pre-DECIGO
Sato (NAOJ)
Satellite
Funaki (ISAS)
Science, Data
Tanaka (Kyoto)Seto (NAOJ)
Kanda (Osaka city)
DECIGO pathfinderLeader: Ando (Tokyo)
Deputy: Takashima (ISAS)
Detector
Ando (Tokyo)
Housing
Sato (NAOJ)
Laser
Ueda (ILS)Musya (ILS)
Drag free
Moriwaki (Tokyo)
Sakai (ISAS)
Thruster
Funaki (ISAS)
Bus
Takashima (ISAS)
Data
Kanda (Osaka city)
Detector
Numata (Merryland)
Ando (Tokyo)
Mission phase
Design phase

Current status
• There are now 140 members from 50 institutes in DECIGO working group
• Budget request (DECIGO R&D and fabrication of DPF, $20M) was rejected.
• We will submit budget request (R&D for DECIGO and DP, $10M) this year again.
• DPF working group was formally approved by JAXA/ISAS.
• We will submit budget request (R&D for DPF, $200K) to JAXA/ISAS.

Summary DECIGO can not only bridge the gap
between terrestrial detectors and LISA, but also open a very deep window at 0.1 – 10 Hz.
DECIGO will use FP arm cavity to further improve the sensitivity.
We have been and will be working hard to obtain a budget to initiate R&D for DECIGO and DPF.
We hope that we will obtain a budget for DECIGO R&D, and that DPF mission will be approved soon!

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