decigo decigo - Gravitational Wave Project Office

Transcription

Prospects and progress of
DECIGO / DECIGO Path Finder
Nobuyuki Kanda
DECIGO collaboration
drawn by Sora.K
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, MasaKatsu 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
1
2009年7月10日金曜日
DECIGO
Bridge between mHz and 10Hz
Ω
2
DECIGO
Ω
2
DECIGO
Ω
2
DECIGO
DECIGO
Deci-hertz Interferometer Gravitational Wave Observatory
3
DECIGO
DECIGO
Deci-hertz Interferometer Gravitational Wave Observatory
3
DECIGO
Plan of the Talk
1. DECIGO’s Seinece
2. Conceptual Design
3. DECIGO Path Finder
Thanks to S.Kawamura, M.Ando, N.Seto, S.Sato, M.Tokuda
and DECIGO collaborators
for figures, photograph and many suggestions.
4
DECIGO
Science of DECIGO
Stochastic Background GW :
Hearing a call of the early universe
Huge number of binary systems :
Foreground (cleaning) problem
Probing dark energy
NS formation
Black Hole related GW
IMBH
BH+NS
Others...
5
DECIGO
Science of DECIGO
Stochastic Background GW :
Hearing a call of the early universe
Huge number of binary systems :
Foreground (cleaning) problem
Probing dark energy
NS formation
Black Hole related GW
IMBH
BH+NS
cosmological
interests !
Others...
5
DECIGO
Deci-Hz band has fruitful info.
Compact Binaries (NS, stellar mass BH, IMBH)
"
#1/2
!
ρ
f ∼ Gρ ∼
[Hz]
106 [g/cm3 ]
frequency [Hz]
1 ~ several years before coalescence of NS-NS
10
1.4-1.4 Msolar
10-10 Msolar
1
TGW ∼
0.1
0.01
0.0
0.5
1.0
1.5
2.0
time [sec]
!
f
0.2[Hz]
"−8/3 !
M
1.2M"
"−5/3
8
2.5 3.0x10
Escape from WD-WD confusion noise around mHz
6
[yrs]
Stochastic Background GW
from early universe
DECIGO
Ω
Two (or more) set of
DECIGO/BBO make
possible to reach the
sensitivity of stochastic
GW from early
universe.
Ω
Ω
7
DECIGO
Foreground GW from NS-NS binaries
Many neutron star binaries are exist.
Roughly ~105 NS-NS binary mergers will appear on
DECIGO for year(s) of observation.
These signals called
DECIGO instrumental noise spectrum
10
simulated signal : noise + 10 NS-NS binaries*
as NS-NS ‘foreground’.
*
It appear as ‘confusion
10
noise’ around 0.1Hz.
-21
5
0-10 years before merge
-22
-23
10
How to remove is a problem.
(In another words, we will use
many NS’s GWs !)
-24
10
0.01
8
2
3
4
5 6 7 89
0.1
Hz
2
3
4
5 6 789
1
Cleaning requires ...
DECIGO
Quite huge number of templates will be needed.
(Culter & Harms, Phys.Rev. D73 042001, for BBO)
Very acculate waveform parameters must be
determined. → Δm/m < ~10-7 %
(in our estimation)
However, in
principle, the
cleaning will be
possible !
!"
#$$
!"
#$'
!"
#$&
(total fitting parameters)/(data amount)
~(R x Tobs x n) / (f x Tobs)
!"
#$%
/
/012345/67896:8/;<8=>9?@
/;AB;/CB8DA98/=E86FGF:H
/
;=E86F//<AI89/;<8=>9?@
#%
//!@J@/K/!" /L
#(
//!@J@/K/!" /L
#)
//!@J@/K/!" /L
$
'
9
&
%
(
) * +
",!
-.
$
'
&
%
(
) * +
!
DECIGO
NS-NS probe for ...
NS formation
DECIGO might see z~5 NS binaries.
S/N ~ (1+z)1/6
Good angular resolution
~ λ/D ~ 109 m / 1AU ~ 10-2 rad
❨Diffraction limit. It will be slightly better with mode analysis.❩
Dark energy, or Weak lensing
geometrical test of
high-redshift universe
dL-z relation
Cutler&Holz, arxiv0906.3752
10
Acceleration of Expansion of the
Universe
Expansion ＋Acceleration?
DECIGO
DECIGO
GW
NS-NS (z∼1)
Output
Strain
Template (No Acceleration)
Real Signal ?
Phase Delay∼1sec (10 years)
Time
Seto, Kawamura, Nakamura, PRL 87, 221103 (2001)
DECIGO
More Massive Objects
IMBH (Intermidiate Mass Black Hole)
Enough high S/N
1000Msolar-1000Msolar @ z=1 --> S/N ~ 103
BH + NS
Also enough S/N, better than NS-NS.
12
Let’s focus on experimental apparatus.
DECIGO
DECIGO conceptual design
ca
vit
Ar
m
Conceptual design :
Space-based, drag free
Fabry=Perot IF, Finesse:10, 10W 532nm
laser,
3 interferometers
1000 km base line
mirror diameter : 1m, weight 100 kg
y
Deci-hertz Interferometer
Gravitational Wave Observatory
1000km
Arm cavity
Laser
Mirror
Photodetector
Drag-free S/C
13
DECIGO
Why FP cavity?
Transponder type
(e.g. LISA)
Implement FP cavity
Shot noise
Transponder type
(e.g. LISA)
e
Implement FP cavity
FP cavity type
Frequency
Sh
ot
no
is
Shorten
arm length
f1
e
is
no
ot
Sh
ure
Shot noise
f1
s
res
n p -2
tio e f
dia nois
Ra
ure
s
res
n p -2
tio e f
dia nois
Ra
Strain
Shorten
arm length
Better bestsensitivity
DECIGO
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.
DECIGO
Cavity and S/C control
Cavity length change
PDH error signal 
Mirror position (and Laser frequency)
Relative motion between mirror and S/C
Local sensor

S/C thruster
Displacement Signal between S/C and Mirror
S/C
1
Local
Sensor
S/C
2
Mirror
Thruster
Actuator
Displacement signal between the two Mirrors
Thruster
Fig: S. Kawamura
Orbit and Constellation
Candidate of orbit:
Record-disk orbit around the Sun
Relative acc.
4x10-12 m/s2
(Mirror force ~10-9 N )
Halo orbit around L2 (or L1)
Relative acc.
4x10-7 m/s2
DECIGO
DECIGO
Orbit and Constellation
Candidate of orbit:
Record-disk orbit around the Sun
Relative acc.
4x10-12
Separated
unit
m/s2
Halo orbit around L2 (or L1)
Relative acc.
4x10-7 m/s2
Constellation
4 interferometer units
Separated
unit
2 overlapped units 
Cross correlation
2 separated units
Angular resolution

overlapped
units
DECIGO
DECIGO-PF
DECIGO Pathfinder (DPF)
First milestone mission for DECIGO
Shrink arm cavity
DECIGO 1000km  DPF 30cm
Single satellite
Local Sensor
(Payload ~1m3 , 350kg)
Low-earth orbit
(Altitude 500km, sun synchronous)
30cm FP cavity with 2 test masses
Stabilized laser source
Drag-free control
Actuator
Thruster
DECIGO
DPF satellite
Mast
structure
DPF Payload
Size :
950mm cube
Weight : 150kg
Power :
130W
Data Rate: 800kbps
Mission thruster x12
Mission
Thruster head
Stabilized.
Laser source
On-board
Computer
Power Supply
SpW Comm.
Satellite Bus
(‘Standard bus’ system)
Size :
950x950x1100mm
Weight : 200kg
SAP :
960W
Battery: 50AH
Downlink : 2Mpbs
DR:
1GByte
3N Thrusters x 4
Interferometer
module
Satellite
Bus system
Bus thruster
Solar Paddle
DPF mission payload
Mission weight : ~150kg
Mission space : ~90 x 90 x 90 cm
Laser source
Yb:YAG laser (1030nm)
Power : 25mW
Freq. stab. by Iodine abs. line
DECIGO
Drag-free control
Local sensor signal
 Feedback to thrusters
Fabry-Perot interferometer
Finesse : 100
Length : 30cm
Test mass : 1kg
Signal extraction by PDH
DECIGO
DPF Sensitivity
Laser source : 1030nm, 25mW
IFO length : 30cm
Finesse : 100, Mirror mass : 1kg
Q-factor : 105, Substrate: TBD
Temperature : 293K
Satellite mass : 350kg, Area: 2m2
Altitude: 500km
Thruster noise: 0.1μN/Hz1/2
(Preliminary parameters)
Possible GW target of DPF
DECIGO
Blackholes events
in our galaxy
IMBH inspiral and merger
h ~ 10-15 , f ~ 4 Hz
Distance 10kpc, m = 103 Msun
Obs. Duration (~1000sec)
KAGAYA
BH QNM
h ~ 10-15 , f ~ 0.3 Hz
Distance 1Mpc, m = 105 Msun
Possible GW target of DPF
DECIGO
Blackholes events
in our galaxy
IMBH inspiral and merger
h ~ 10-15 , f ~ 4 Hz
Distance 10kpc, m = 103 Msun
Obs. Duration (~1000sec)
KAGAYA
BH QNM
h ~ 10-15 , f ~ 0.3 Hz
Distance 1Mpc, m = 105 Msun
Observable range reaches
the Galactic center (SNR~5 )
Hard to access by others
 Original observation
DECIGO
Gravity of the Earth
Measure gravity field of the Earth for Satellite Orbits
GPS satellite
Determine global gravity field
 Density distribution
Monitor of change in time
Ground water motion
Strains in crusts by
earthquakes and volcanoes
東京大字地震研・新谷氏、
京都大学・福田氏の資料/情報提供
DECIGO
Gravity of the Earth
Measure gravity field of the Earth for Satellite Orbits
GPS satellite
Determine global gravity field
 Density distribution
Monitor of change in time
Ground water motion
Strains in crusts by
earthquakes and volcanoes
Observation Gap
between GRACE and GRACE-FO
(2012-16)
 DPF contribution
東京大字地震研・新谷氏、
京都大学・福田氏の資料/情報提供
in international network
DECIGO
R&D for DPF (1)
By M.Musha
Stabilized Laser
BBM development
Yb:YAG (NPRO) source
Saturated absorption by I2
 Stability test, Packaging
IFO and housing
BBM-EM development
 Test of concepts
+ Earth gravity sensors
S.Sato’s talk
(P. Session #2, Today)
Y.Wakabayashi’s poster
By S.Sato
By
A.Araya
R&D for DPF (2)
Attitude control and Drag-free
Satellite structure (mass distribution)
Passive attitude stabilization
by gravity gradient
Mission thruster position
Control topology
DECIGO
By
S.Moriwaki
R&D for DPF (2)
Attitude control and Drag-free
Satellite structure (mass distribution)
Passive attitude stabilization
DECIGO
By
S.Moriwaki
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
DECIGO
Roadmap of DECIGO/DPF
2007 08
09
10
11
12
13
14
R&D
Fabrication
15
16
17
18
19
20
R&D
Fabrication
21
22
23
24
25
R&D
Fabrication
Mission
DECIGO
Pathfinder
(DPF)
Pre-DECIGO
DECIGO
SDS-1/SWIM
Objective
GW astronomy
GW observation
Detect GW
with min. spec
FP between S/C
Single small satellite
Short FP interferometer
3 S/C
1 interferometer unit
3 S/C
x 3-4 units
Space test of key tech. Design
26
26
DECIGO
Organization
PI: Kawamura (NAOJ)
Deputy: Ando (Kyoto)
Executive Committee
Kawamura (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)
Detector
Numata
(Maryland)
Ando (Kyoto)
Satellite
Funaki (ISAS)
Design phase
DECIGO pathfinder
Leader: Ando (Kyoto)
Deputy: Takashima (ISAS)
Mission phase
Detector
Laser
Housing
Ando
(Kyoto)
Ueda (ILS)
Musya (ILS)
Sato
(Hosei)
Drag free
Moriwaki
(Tokyo)
Sakai (ISAS)
27
Science, Data
Tanaka (Kyoto)
Seto (Kyoto)
Kanda (Osaka city)
Thruster
Bus
Data
Funaki
(ISAS)
Takashima
(ISAS)
Kanda
(Osaka city)
Collaboration and support
DECIGO
・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 ones of main projects (2009.4-)
・Collab. with UNISEC (University Space Engineering Consortium)
Call for active young engineers
DECIGO
Summary
DECIGO is a future space-based GW detector
project :
Fabry-Perot IF, 1000km baseline,
constellation flight
Deci-Hz band is a focus of DECIGO! (same to BBO)
Fruitful frequency band for not only astronomical
sources but also cosmological studies.
DECIGO Path Finder is going now.
29

decigo decigo - Gravitational Wave Project Office

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