decigo and pathfinder missions
DESCRIPTION
DECIGO and Pathfinder Missions. Masaki Ando (Department of Physics , Kyoto University). Original Picture : Sora. - PowerPoint PPT PresentationTRANSCRIPT
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Seiji Kawamura, Takashi Nakamura, Kimio Tsubono, Takahiro Tanaka, Ikkoh Funaki, Naoki Seto, Kenji Numata, Shuichi Sato, Nobuyuki Kanda, Takeshi Takashima, Kunihito Ioka, Kazuhiro Agatsuma, Tomotada Akutsu, Tomomi Akutsu, Koh-suke Aoyanagi, Koji Arai, Yuta Arase, Akito Araya, Hideki Asada, Yoichi Aso, Takeshi Chiba, Toshikazu Ebisuzaki, Motohiro Enoki, Yoshiharu Eriguchi, 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, 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, Shogo Kamagasako, Nobuki Kawashima, Fumiko Kawazoe, Hiroyuki Kirihara, Naoko Kishimoto, Kenta Kiuchi, 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, 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, Kakeru Takahashi, Keitaro Takahashi, Tadayuki Takahashi, Hirotaka Takahashi, Ryuichi Takahashi, Ryutaro Takahashi, Takamori Akiteru, 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
Masaki Ando (Department of Physics, Kyoto University)
Original Picture : Sora
DECIGO and Pathfinder Missions
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Baseline length: 1000 km3 S/C formation flight 3 FP interferometers Drag-free control
DECIGO
Laser
Photo-detector
1000kmArm cavity
Drag-free S/C
Arm
cavi
tyMirror
DECIGO
Space GW antenna (~2024)Obs. band around 0.1 Hz
(Deci-hertz interferometer Gravitational wave Observatory)
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
1. DECIGO Overview and Science
Pre-conceptual Design
2. DECIGO Pathfinder Overview and Science
Design and Status
3. Summary
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
1. DECIGO Overview and Science
Pre-conceptual Design
2. DECIGO Pathfinder Overview and Science
Design and Status
3. Summary
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Gravitational Waves
"Mass tells space-time how to curve, and space-time tells mass how to move.“ John Archibald Wheeler
From presentation by Laura Cadonati
General Relativity
Einstein equation
Interpret gravity as nature of space-time
Curvature of Space-time
Mass(Energy-Momentum)
Motion of Mass Ripples in gravitational field Propagate as waves
Gravitational Waves
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
EM and GW waves
A. Einstein
Solution of the Einstein equation
Gravitational waveWaves in space-time (gravitational field)
1918: Predicted by Einstein1989: Confirmed by a Binary pulsar observation
Electromagnetic waveWaves in electromagnetic
field
1864 : Predicted by Maxwell1888 : Confirmed by the Hertz’s experiment Radiated by acceleration
of masses High transmittance through matter (Small interactions with
matter)
Radiated by acceleration of charged particlesUtilized in telecommunications and observations
J.C. Maxwell
Solution of the Maxwell equations
‘Gravitational-wave astronomy’
Independent Information Direct probe of dynamic motion of matters Early universe before recombination
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
重力波による天文学
Astronomical Probes
Astronomy
StarsGalaxies
Black HolesMassive BHs
Planets
Gamma-ray burstSupernovae
AstronomicalPhenomenaGamma
X-rayVisible rayInfrared
Microwave
EM waveobservation
CosmologyInflation
Dark matterDark energy
Cosmic Background
Nuclear PhysicsHigh-Density Matter
Cosmic-Rayobservation
NeutrinoHigh-energy CR
Background: NASA/WMAP Science Team
General RelativityRelativity in Strong Gravitational-Field
GWobservation
Low-freq. GWs
High-freq. GWsCompact Inspiral
Supernovae
BackgroundGWs
Pulsar
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
LCGT and DECIGO
LCGT (~2014) Terrestrial Detector High frequency events
Target: GW detection
DECIGO (~2024) Space observatory Low frequency sources
Target: GW astronomy
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
DECIGO
DECIGO
Space GW antenna (~2024)Obs. band around 0.1 Hz
10–4 10–2 100 102 104
10–26
10–24
10–22
10–20
10–18
10–16
Frequency [Hz]
Str
ain
[
1/H
z1/2 ] Terrestrial
Detectors (Ad. LIGO, LCGT, etc)
DECIGO
LISA
(Deci-hertz interferometer Gravitational wave Observatory)
‘Bridge’ the obs.gap between LISA and Terrestrial detectors
Effect of Gravitational waves
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Gravitational WavesChange in proper distanceTidal force for finite-sized matter
x
y
z
GW
Typical amp. h =10-21 distance change by 10-
21m for 1-m separation
GW amplitude h : Strain (dimensionless)
Precise length measurement with long baseline
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
DECIGO Interferometer
Interferometer Unit: Differential FP interferometer
Laser
Photo-detector
1000kmArm cavity
Drag-free S/C
Arm
cavi
tyMirror
Baseline length: 1000 km3 S/C formation flight 3 FP interferometers Drag-free control
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Targets and Science
DECIGO (1 unit)
IMBH inspiral (z~1)
Merger
Frequency [Hz]
GW
am
plitu
de [
Hz-
1/2]
10-4 10-2 100 102 104
10-24
10-22
10-20
10-18
10-16
10-26
DECIGO (Correlation)
Background
GW
(Ωgw
~ 2 x 10 -16)
NS inspiral (z~1)
Merger
3month
IMBH binary inspiralNS binary inspiralStochastic background
Galaxy formation (Massive
BH)
Cosmology (Inflation, Dark energy)
Constraint on dark energy
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
DECIGO will observe 104-5 NS binaries at z~1
Precise ‘clock’ at cosmological distance
Angular resolution ~ 10arcmin ( 1 detector ) ~ 10arcsec ( 3 detectors )
at z=1%1,, wwm
Determine cosmological parameters
Absolute and independent measurement
Information on acceleration of expansion of the universe
chirp waveformDistance:
Redshift: host galaxy
‘Standard Siren’
Relationship between distance and redshift
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)
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Stochastic Background GWs
Stochastic
Background GWs
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
1. DECIGO Overview and Science
Pre-conceptual Design
2. DECIGO Pathfinder Overview and Science
Design and Status
3. Summary
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Pre-Conceptual Design
Interferometer Unit: Differential FP interferometer
Laser
Photo-detector
Arm cavity
Drag-free S/C
Arm
cavi
tyMirror
Arm length: 1000 kmFinesse: 10Mirror diameter: 1 mMirror mass: 100 kgLaser power: 10 WLaser wavelength : 532 nmS/C: drag free
3 interferometers
Interferometer Design
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Transponder type vs Direct-reflection type
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
/Hz
1/2]
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
Compare : Sensitivity curves and Expected Sciences
Cavity and S/C control
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
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
Requirements
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Disp. meas. Noise Shot noise 3 x 10-18 m/Hz1/2 (0.1 Hz)
Acceleration Noise Force noise 4x10-17 N/Hz1/2 (0.1 Hz)
Other noises should be well below the shot noise Laser freq. noise: 1 Hz/Hz1/2 (1Hz)
Stab. Gain 105, CMRR 105
x 10 of LCGT in phase noise
x 1/50 of LISA
External force sources Fluctuation of magnetic field, electric field, gravitational field, temperature, pressure, etc.
Orbit and Constellation
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Record-disk orbit around the SunRelative acc. 4x10-12 m/s2
Halo orbit around L2 (or L1)
Relative acc. 4x10-7 m/s2
(Mirror force ~10-9 N )
(Mirror force ~10-4 N )
Separated unit
Constellation
4 interferometer units
2 overlapped units Cross correlation2 separated units Angular resolution
overlapped units
Separated unit
Candidate of orbit:
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Roadmap
Figure: S.Kawamura
2007
08 09 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26
Mission
Objective
Space test of key tech. GW observation
Detect GW with min. spec FP between S/C
GW astronomy
Design
Single small satellite Short FP interferometer
3 S/C 1 interferometer unit
3 S/C x 3-4 units
DECIGO Pathfinder (DPF)
Pre-DECIGO DECIGO
R&DFabricatio
n
R&DFabricatio
n
R&DFabricatio
n
SDS-1/SWIM
Organization
PI: Kawamura (NAOJ)Deputy: Ando (Kyoto)
Executive CommitteeKawamura (NAOJ), Ando (Kyoto), Seto (Kyoto), Nakamura (Kyoto),
Tsubono (Tokyo), Tanaka (Kyoto), Funaki (ISAS), Numata (Maryland), Sato (Hosei), Kanda (Osaka city), Takashima (ISAS), Ioka (KEK)
Pre-DECIGO
Sato (Hosei)
Satellite
Funaki (ISAS)
Science, Data
Tanaka (Kyoto)Seto (Kyoto)
Kanda (Osaka city)
DECIGO pathfinderLeader: Ando (Kyoto)
Deputy: Takashima (ISAS)
Detector
Ando (Kyoto)
Housing
Sato (Hosei)
LaserUeda (ILS)
Musya (ILS)
Drag freeMoriwaki (Tokyo)Sakai (ISAS)
Thruster
Funaki (ISAS)
Bus
Takashima (ISAS)
Data
Kanda (Osaka
city)
Detector
Numata (Maryland)
Ando (Kyoto)
Mission phase
Design phase
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Collaboration and support
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
・ Supports from LISA Technical advises from LISA/LPF experiences Support Letter for DECIGO/DPF LISA-DECIGO workshop (2008.11)
・ Collab. with Stanford univ. group Drag-free control of DECIGO/DPF UV LED Charge Management System for DPF
・ Collab. with JAXA navigation-control section formation flight of DECIGO, DPF drag-free control
・ Research Center for the Early Universe (RESCEU), Univ. of Tokyo Support DECIGO as one of main projects (2009.4-)
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
1. DECIGO Overview and Science
Pre-conceptual Design
2. DECIGO Pathfinder Overview and Science
Design and Status
3. Summary
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Roadmap
Figure: S.Kawamura
2007
08 09 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26
Mission
Objective
Space test of key tech. GW observation
Detect GW with min. spec FP between S/C
GW astronomy
Design
Single small satellite Short FP interferometer
3 S/C 1 interferometer unit
3 S/C x 3-4 units
DECIGO Pathfinder (DPF)
Pre-DECIGO DECIGO
R&DFabricatio
n
R&DFabricatio
n
R&DFabricatio
n
SDS-1/SWIM
DECIGO-PF
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
DECIGO Pathfinder (DPF)
Single satellite (Payload ~1m3 , 350kg)
Low-earth orbit (Altitude 500km, sun synchronous)
30cm FP cavity with 2 test masses Stabilized laser source Drag-free control
Local Sensor
Actuator
Thruster
First milestone mission for DECIGOShrink arm cavity DECIGO 1000km DPF 30cm
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
DPF satellite
Stabilized. Laser source
Interferometer module
Satellite Bus system
Solar Paddle
MissionThruster head
On-boardComputer
Bus thruster
Mast structure
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 mission payload
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
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 : ~90 x 90 x 90 cm
Laser source Yb:YAG laser (1030nm) Power : 25mW Freq. stab. by Iodine abs. line
DPF Sensitivity
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Satellite mass : 350kg, Area: 2m2
Altitude: 500kmThruster noise: 0.1μN/Hz1/2
Laser source : 1030nm, 25mW IFO length : 30cmFinesse : 100, Mirror mass : 1kgQ-factor : 105, Substrate: TBDTemperature : 293K (Preliminary
parameters)
10–2 10–1 100 101 10210–18
10–17
10–16
10–15
10–14
10–13
10–12
10–11
10–18
10–17
10–16
10–15
10–14
10–13
10–12
No
ise
leve
l
[1/H
z1/2
]
Frequency [Hz]
Shot noise
Mirror thermal
Laser Radiation
Laser: 1030nm, 25mWFinesse: 100Mirror mass: 1kgQ–value of a mirror: 106
Cavity length: 30cm
pressure noiseThruster noise
PM acceleration Noise
Geog
ravity Laser Frequencynoise
Dis
pla
cem
ent
No
ise
[m
/Hz1
/2]
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
DPF sensitivity
10–4 10–2 100 102 104
10–26
10–24
10–22
10–20
10–18
10–16
Frequency [Hz]
Str
ain
[
1/H
z1/2 ]
DECIGO
LCGT
Core-collapseSupernovae
NS binary inspiral
ScoX-1 (1yr)
Pulsar (1yr)
Massive BH inspirals
Galaxybinaries
Gravity-gradient noise (Terrestrial detectors)
DPF limit
Background GWsfrom early universe (Wgw=10-14)
DPF sensitivity h ~ 2x10-15 Hz1/2 (x10 of quantum noises)
Foreground GWs
LISA
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
GW target of DPF
Observable range reaches the Galactic center (SNR~5 )
BH QNM
h ~ 10-15 , f ~ 0.3 Hz Distance 1Mpc, m = 105
Msun
IMBH inspiral and merger
Obs. Duration (~1000sec)
h ~ 10-15 , f ~ 4 Hz Distance 10kpc, m = 103
Msun
KAGAYA
Blackholes events in our galaxy
Hard to access by others Original observation
103 104 105 10610–1
100
101
102
Ob
serv
able
Ran
ge
Mass [Msolar]
[kp
c,
SN
R=
5]
Galactic Center
BH QNMBH Inspiral
(By N.Kanda)
Gravity of the Earth
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Measure gravity field of the Earth for Satellite Orbits
Determine global gravity field Density distributionMonitor of change in time Ground water motion Strains in crusts by earthquakes and volcanoes
GPS satellite
東京大字地震研・新谷氏、京都大学・福田氏の資料 / 情報提供
Observation Gap between GRACE and GRACE-FO (2012-16) DPF contribution in international network
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
1. DECIGO Overview and Science
Pre-conceptual Design
2. DECIGO Pathfinder Overview and Science
Design and Status
3. Summary
R&D for DPF (1)
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Stabilized Laser BBM development Yb:YAG (NPRO) source Saturated absorption by I2
Stability test, Packaging
By M.Musha
By S.Sato
IFO and housing BBM-EM development Test of concepts + Earth gravity sensors
By A.Araya
R&D for DPF (2)
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Attitude control and Drag-free Satellite structure (mass distribution) Passive attitude stabilization by gravity gradient Mission thruster position Control topology
Thruster System design with existing tech. Noise meas. system (thruster stand) Development of Slit FEEP
By I.Funaki
ByS.Moriwaki
SWIM launch and operation
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
Tiny 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
Successful control
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
SWIM In-orbit operation
z control on
yaw control on
Operation: May 12, 2009
Downlink: ~ a week
Test mass controlled
Damped oscillation (in pitch DoF)
Error signal zero
Signal injection OL trans. Fn.
Free oscillation in x and y DoF
By W.Kokuyama
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
DPF mission status
DPF : One of the candidate of JAXA’s small satellite series
At least 3 satellite in 5 years withStandard Bus + M-V follow-on rocket
1st mission (2012): SPRINT-A/EXCEED2nd mission (~2013/14) : ERG3rd mission (~2015/16) : TBD
SPRINT-A /EXCEED
DPF is one of the candidates of 3rd mission
Next-generationSolid rocket booster (M-V FO) Fig. by JAXA
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
1. DECIGO Overview and Science
Pre-conceptual Design
2. DECIGO Pathfinder Overview and Science
Design and Status
3. Summary
Summary
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
DECIGO : Fruitful Sciences
Very beginning of the UniverseDark energyGalaxy formation
DECIGO Pathfinder
Important milestone for DECIGOStrong candidate of JAXA’s satellite seriesSWIM – under operation in orbit first precursor to space!
KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)
End