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Sora. The Japanese Space Gravitational Wave Antenna: DECIGO. LISA8 @Stanford Univ. USA June 29, 2010 - PowerPoint PPT Presentation
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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 Japanese GW Roadmap DECIGO Roadmap to DECIGO DECIGO Pathfinder, etc. Organization, Collaboration, etc. Summary
Japanese Roadmapto GW Astronomy
Detecting GW(International network)
LCGT
DECIGO
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
10-18
10-24
10-22
10-20
10-4 10410210010-2
Frequency [Hz]
Stra
in [H
z-1/2]
LISA
DECIGO
Ground-based detectors
Confusion Noise
moved above
LISA band To be movedinto GBD 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
LaserPhoto-detector
Arm cavity
Drag-free S/C
Arm cavity
Mirror
Why FP cavity?
Frequency
Stra
in
Radiation pressure
noise f -2
Shot noiseShot n
oise f1
Transponder type
Shot noise
Shortenarm length
Shot noise
f1
Radiation pressure
noise f -2
Transponder typeShortenarm length Implement FP cavity
Implement FP cavity
FP cavity type Better shot-noise-limited
sensitivity
More stringent acceleration noise
requirement
Drag free and FP cavity: compatible?
Mirror
S/C IS/C II
Solar radiationpressure, etc
Solar radiationpressure, etc
Gravity force
Gravity force
Gravity force
Gravity force
1,000 km
FP cavity and drag free : compatible?
Local sensor
ThrusterThruster
Mirror
Relative position between mirror
and S/C
S/C II S/C I
Gravity force Gravity force
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
Gravity force
Orbit and constellation (preliminary)
Sun
Earth
Record disk
Increase angular resolution
Correlation for stochastic background
Formation of super-
massive BH
Verification of inflation
Science by DECIGO
Frequency [Hz]
Correlation(3 years)
Stra
in [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 binaryCoalescence
5 years
NS binary (z=1)
Coalescence
3 months
Acceleration of Universe
Dark energy
Radiation pressure noise
Shot noise
1 cluster
Mini-black hole
Dark matter
Brans Dickeparameter
Inflation(GW~2×10-16)
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
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 technologiesDetection 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 ÞMasaki Ando’s talk on Thursday
Pre-DECIGO
DECIGO
R&DFabrication
R&DFabrication
R&DFabrication
SWIMÞ Wataru Kokuyama’s poster
DECIGO Pathfinder (DPF)
Local Sensor
Actuator
Thruster
Single satellite Earth orbit Altitude: 500km Sun synchronous
Arm length: 1000 kmArm 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
Stabilized. Laser source
Interferometer module
Satellite Bus system
Solar Paddle
MissionThruster head
On-boardComputer
Bus thruster
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
DPF Payload
Fabry-Perot interferometer Finesse : 100 Length : 30cm Test mass : ~1kg Signal extraction by PDH
Drag-free control Local sensor signal Feedback to thrusters
Mission weight : ~150kgMission space : ~95 x 95 x 90 cm
Laser source Yb:YAG laser (1030nm) Power : 25mW Freq. stab. by Iodine abs. line
Thruster
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
Noi
se le
vel
[1/H
z1/2 ]
Frequency [Hz]
Shot noiseMirror 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
plac
emen
t Noi
se
[m/H
z1/2 ]
Detection range
103 104 105 10610–1
100
101
102
Obs
erva
ble
Ran
ge
Mass [Msolar]
[kpc
, SNR
=5]
Galactic Center
BH QNMBH Inspiral
Gravity of the EarthMeasure gravity field of the Earth from Satellite Orbits, and gravity-gradiometer
Determine global gravity field Density distributionMonitor of change in time Ground water motion Strains in crusts by earthquakes and volcanoes
GPS satellite
By Araya and Fukuda
Observation Gap between GRACE and GRACE-FO (2012-16) DPF contribution in international network
Þ Ayaka Shoda’s poster
R&D for SubsystemsÞ Shuichi Sato’s talk on Thursday, Yuta Michimura’s talk on Thursday
Frequency-stabilized laser
ThrusterInterferometric sensor
Drag-freemodel
Electrostatic sensor/actuator
Test mass module
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).
SWIMTiny 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
Pre-DECIGOPre-DECIGO
DECIGO
Arm length 100 km 1000 km
Mirror diameter 30 cm 1 m
Laser wavelength 0.532 m 0.532 m
Finesse 30 10
Laser power 1 W 10 W
Mirror mass 30 kg 100 kg
# of interferometers in each cluster
1 3
# of clusters 1 4
Sensitivity of Pre-DECIGO
10-2410-2310-2210-2110-2010-1910-1810-1710-1610-15
Stra
in s
ensi
tivi
ty [
1/rH
z]
10-3 10-2 10-1 100 101 102 103
Frequency [Hz]
DPFDPFDPFDPF
NS-NS inspiral (@300Mpc)
pre-DECIGO
DECIGO
S/N~14 for NS-NS@300Mpc, 10-20 events/year
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 OrganizationPI: Kawamura (NAOJ)Deputy: Ando (Kyoto)
Pre-DECIGO
Sato (Hosei)
Spacecraft
Funaki (JAXA/ISAS)
Science & DataTanaka (Kyoto)
Seto (Kyoto)Kanda (Osaka City)
DECIGO PathfinderLeader: Ando (Kyoto)
Detector
A. Ueda (NAOJ)
Housing
Sato (Hosei)
Laser
K. Ueda (E.C.)Musha (E.C.)
Drag-free Moriwaki (Tokyo)Sakai
(JAXA/ISAS)
Thruster
Funaki(JAXA/ISAS)
Bus
Takashima(JAXA/ISAS)
Data
Kanda(Osaka City)
DetectorAkutsu (NAOJ)
Numata (Maryland)
Mission Phase
Design Phase
Executive CommitteeKawamura (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)
1st InternationalLISA-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
DECIGO will bring us a variety of fruitful science.
The first step to realize DECIGO is to have DPF approved!
Conclusions