decigo and pathfinder missions

41
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

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DECIGO and Pathfinder Missions. Masaki Ando (Department of Physics , Kyoto University). Original Picture : Sora. - PowerPoint PPT Presentation

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Page 1: DECIGO and Pathfinder Missions

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

Page 2: 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

LaserPhoto-detector

1000kmArm cavity

Drag-free S/C

Arm

cav

ityMirror

DECIGO  

Space GW antenna (~2024)Obs. band around 0.1 Hz

(Deci-hertz interferometer Gravitational wave Observatory)

Page 3: DECIGO and Pathfinder Missions

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

Page 4: DECIGO and Pathfinder Missions

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

Page 5: DECIGO and Pathfinder Missions

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

Page 6: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

EM and GW wavesA. 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

Page 7: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

重力波による天文学

Astronomical Probes

AstronomyStarsGalaxies

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

Page 8: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

LCGT and DECIGOLCGT (~2014) Terrestrial Detector High frequency events

Target: GW detection

DECIGO (~2024) Space observatory Low frequency sources

Target: GW astronomy

Page 9: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

DECIGODECIGO  

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]

Stra

in

[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

Page 10: DECIGO and Pathfinder Missions

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

Page 11: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

DECIGO Interferometer

Interferometer Unit: Differential FP interferometer

LaserPhoto-detector

1000kmArm cavity

Drag-free S/C

Arm

cav

ityMirror

Baseline length: 1000 km3 S/C formation flight 3 FP interferometers Drag-free control

Page 12: DECIGO and Pathfinder Missions

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

plit

ude

[H

z-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)

Page 13: DECIGO and Pathfinder Missions

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?

TimeSt

rai

n

Template (No Acceleration)

Real Signal ?

Phase Delay ~ 1sec (10 years) Seto, Kawamura, Nakamura,

PRL 87, 221103 (2001)

Page 14: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

Stochastic Background GWs

Stochastic

Background GWs

Page 15: DECIGO and Pathfinder Missions

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

Page 16: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

Pre-Conceptual Design

Interferometer Unit: Differential FP interferometer

LaserPhoto-detector

Arm cavity

Drag-free S/C

Arm

cav

ityMirror

Arm length: 1000 kmFinesse: 10Mirror diameter: 1 mMirror mass: 100 kgLaser power: 10 WLaser wavelength : 532 nmS/C: drag free

3 interferometers

Page 17: DECIGO and Pathfinder Missions

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]

Stra

in

[1/H

z1/2 ]

LCGT

LISA

DECIGO(LISA type, 5x104km)

DECIGO(FP type, 1000km)

Laser: 10W, 532nmMass: 100kgMirror: 1m dia.

WD-WD confusion

noise

Decisive factor: Binary confusion noise

Compare : Sensitivity curves and Expected Sciences

Page 18: DECIGO and Pathfinder Missions

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

Page 19: DECIGO and Pathfinder Missions

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.

Page 20: DECIGO and Pathfinder Missions

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:

Page 21: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

RoadmapFigure: 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

Page 22: DECIGO and Pathfinder Missions

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)

Page 23: DECIGO and Pathfinder Missions

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-)

Page 24: DECIGO and Pathfinder Missions

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

Page 25: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

RoadmapFigure: 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

Page 26: DECIGO and Pathfinder Missions

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

Page 27: DECIGO and Pathfinder Missions

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

Page 28: DECIGO and Pathfinder Missions

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

Page 29: DECIGO and Pathfinder Missions

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

Noi

se le

vel

[1/H

z1/2 ]

Frequency [Hz]

Shot noiseMirror thermal

Laser Radiation

Laser: 1030nm, 25mWFinesse: 100Mirror mass: 1kgQ–value of a mirror: 106

Cavity length: 30cm

pressure noiseThruster noise

PM acceleration Noise

Geogravity Laser Frequency

noise

Dis

plac

emen

t Noi

se

[m/H

z1/2 ]

Page 30: DECIGO and Pathfinder Missions

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]

Stra

in

[1/H

z1/2 ]

DECIGO LCGT

Core-collapseSupernovae

NS binary inspiral

ScoX-1 (1yr)

Pulsar   (1yr)

Massive BH inspiralsGalaxybinaries

Gravity-gradient noise (Terrestrial detectors)

DPF limit

Background GWsfrom early universe (gw=10-14)

DPF sensitivity h ~ 2x10-15 Hz1/2 (x10 of quantum noises)

Foreground GWs

LISA

Page 31: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

GW target of DPF

Observable range reaches the Galactic center (SNR~5 )

BH QNMh ~ 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

Obs

erva

ble

Ran

ge

Mass [Msolar]

[kpc

, SNR

=5]

Galactic Center

BH QNMBH Inspiral

(By N.Kanda)

Page 32: DECIGO and Pathfinder Missions

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

Page 33: DECIGO and Pathfinder Missions

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

Page 34: DECIGO and Pathfinder Missions

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.SatoIFO and housing

BBM-EM development Test of concepts  + Earth gravity sensors

By A.Araya

Page 35: DECIGO and Pathfinder Missions

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

Page 36: DECIGO and Pathfinder Missions

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

Page 37: DECIGO and Pathfinder Missions

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, 2009Downlink: ~ 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

Page 38: DECIGO and Pathfinder Missions

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

Page 39: DECIGO and Pathfinder Missions

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

Page 40: DECIGO and Pathfinder Missions

Summary

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

DECIGO : Fruitful SciencesVery beginning of the UniverseDark energyGalaxy formation

DECIGO PathfinderImportant milestone for DECIGOStrong candidate of JAXA’s satellite seriesSWIM – under operation in orbit first precursor to space!

Page 41: DECIGO and Pathfinder Missions

KEK Theory Center Cosmophysics Group Workshop (November 11, 2009, Tskuba, Ibaraki)

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