Interplanetary Network of Optical Lattice Clocks
Hisaaki Shinkai (Osaka Inst. Tech.)
真⾙寿明（⼤阪⼯⼤）
http://www.oit.ac.jp/is/shinkai
Proposal of new GW detection method, using the world-recording precise clocks in space,and current-ready techniques.
work with
Toshikazu Ebisuzaki 戎崎俊⼀（RIKEN）
Hidetoshi Katori ⾹取秀俊 (RIKEN, UTokyo)
Jun Makino 牧野淳⼀郎 (Kobe U, RIKEN)
Atsushi Noda 野⽥篤司 (JAXA)
Toru Tamagawa ⽟川徹（RIKEN）「数理科学」2018-12「科学」2017-12
Int. J. Mod. Phys. D 28 (2019) 1940002
https://doi.org/10.1142/S0218271819400029 or arXiv:1809.10317

2019 June 14 @ GW-Research Exchanging MeetingInterplanetary Network of Optical Lattice Clocks
Hisaaki Shinkai (Osaka Inst. Tech.)
真⾙寿明（⼤阪⼯⼤）
http://www.oit.ac.jp/is/shinkai
Proposal of new GW detection method, using the world-recording precise clocks in space,and current-ready techniques.

work with
Toshikazu Ebisuzaki 戎崎俊一（RIKEN）
Hidetoshi Katori 香取秀俊 (RIKEN, UTokyo)
Jun Makino 牧野淳一郎 (Kobe U, RIKEN)
Atsushi Noda 野田篤司 (JAXA)
Toru Tamagawa 玉川徹（RIKEN）「数理科学」2018-12「科学」2017-12
Int. J. Mod. Phys. D 28 (2019) 1940002
https://doi.org/10.1142/S0218271819400029 or arXiv:1809.10317

伊能忠敬
Tadataka Ino (1745-1818)
a Japanese astronomer,
cartographer, and geodesist.

天文学・物理学の受容
中国

日本

春秋戦国時代：置閏法，連大配置法の暦

ヨーロッパ BC45：ユリウス暦，
カエサ ル
1太陽年=365.25日

 862（貞観4）：宣明暦（せんみょうれき）

漢代：蓋天説，渾天説の宇宙論（論天説）

1543：コペルニクス

元：イスラム・アラビアの科学技術が伝わり，天体観測技術の水準が上がる

1619：ケプラー『世界 の調 和』

C.Ferreira （沢野忠庵）・向井元升『乾坤弁説』
アリストテレスの4元素説を中国流の陰陽五行説で批評地が円くて天の中央にあることを肯定★天動説，ティコ・ブラーエの説
1620？『崇禎暦書』すうていれきしょ『暦算全書』

 1645-1911（清）：時憲暦
ドイツの宣教師アダム・シャール
中国最後の太陰暦（いわゆる旧暦）

1723，1738『暦象考成』上下編

W.J.Blaeu著
Tweevoudig onderwijs van de hemelseen adressen globen
1666

1687：ニュ ートン『自然哲 学の数学的諸原理』（プリンキピ ア）

J.Keill 著 J. Lulofs蘭訳
Inleiding tot de ware Natuur en
Sterrenkunde
1741

1733『暦算全書』翻 訳，中根 元圭『五星本天皆以 地為 心』
ティコ・ブラーエの観測値

 1755（宝暦5）：宝暦暦（ほうりゃくれき）
1763年の日食を外す．1771年修正宝暦暦．しかし，閏月計算に不具合発生．

★ケプラー，楕円軌道・不等速運動説（地動説含まず）1792

ニュ ートンの歳実

本木良永 (1735-1794)

天文暦学研究 ，天体観測，消長 法，『時中暦』

1774『天地二球用法』

1786『実験録推歩 法』，89? 奇 法発見 ？
1797?『五星距 地之奇 法』
間 重富 1796？ 天行方数諸曜帰一之理

志筑忠雄 (1760-1806) 1798（寛政10）：寛政暦
西洋天文学を取り入れた暦．

司馬江漢
1793『地球全図略説』

訳語として惑星・視差・
近点・遠点など

訳語として遠心力など

1798，1802『暦象新書』
巻末に『混沌分判図説』独自の太陽系起源説
ラプラス・カントの星雲説(1796)とほぼ同時

B. Martin 著 I.Tirion蘭訳
Natuurkunde
1744
G.Adams 著 J. Ploos蘭訳
Gronden der Starrenkunde
1770

1792『星術本原太陽窮理了解新制天地二球用法記』

高橋至時

1802『新修五星法図説』
1804『ラランデ 暦書管見 』

コペルニクスの太陽系説



三浦梅園

麻田剛立 （1734-1799）

1742『暦象考成後編』宣教師ケーグラー

1太陽年=365.2425日

徳川吉宗 ，禁 書令 の緩 和，西洋天文学を用いた改 暦を指示

1680 日本に輸入さ れ広 まる
1730『天経或問』訓 点本，
西川正休

1675『天経或問てんけいわくもん』

1年=354日

1632：ガ リレイ『天文対話 』地動説擁護 1685（貞享2）：貞享暦（じょうきょうれき），渋川春海

1645『西洋新法暦書』

 1587：グレゴリオ暦，
グレゴ リウ ス13世

1609：ケプラー『新天文学』

1643：宣教師キアラ(G.Chiara) 天文書持ち込む

1太陽年=365.2425日，
1朔望月=29.530593日

 622：ヒジュラ暦『天球の回転について』1639（寛永16）：鎖国

 1281-1644（元・明）：授時暦

中東

Newton力学
Kepler 3法則

J-J. L. de Lalande著 (A.B. Strabbe蘭訳)
Astronomia of Sterrkunde
1773-80

1803

伊能忠敬

ガ リレオ衛 星の食観測

1796「和蘭天説」地動説に触れる
1808『刻白爾天文図解』地動説を紹介

山片蟠桃
1805？『夢 の代』

1822『新修五星法』
渋川景佑
高橋景保 『新巧 暦書』

帆足萬里

1836『窮理通 』

 1844（天保15）：天保暦
日本最後の太陰暦（いわゆる旧暦）
渋川景佑

1846『新法暦書続 編』

 1873（明治6）：太陽暦・グレゴリオ暦

T. INO learned astronomical positioning method.
He observed the eclipse of Io.

⿇⽥剛⽴とケプラーの惑星運動第3法則
真⾙寿明
⼤阪⼯業⼤学紀要61巻 (2016) 2号 27-36

Interplanetary Network of Optical Lattice Clocks
Hisaaki Shinkai (Osaka Inst. Tech.)
真⾙寿明（⼤阪⼯⼤）Int. J. Mod. Phys. D 28 (2019) 1940002

https://doi.org/10.1142/S0218271819400029 or arXiv:1809.10317◆Cassiniʼs Doppler tracking (2001-2002) can be improved 3-order mag.
with current technologies◆“INO-c”, “INO-d” : sensitivity curve，detectable distance D◆ Event rate by hierarchical formation model of SMBH

◆ One satellite costs 50 billion yen (500億円).

5

１. Introduction：Optical Lattice Clock“Optical Lattice Clock”
H. Katori（JPS Journal，2002, p754）
trap atoms at standing laser wave
read frequency of transient phase
Cs atomic clock Δt/t = 5x10-16
Optical Lattice Clock (2015)10-18

magic freq. compensates multi-polarization
OLC targets

Δt/t = 10-19

grav. potential of 15m diﬀerence
relativistically measured
5cm

JPS J，2017，p84（１cｍ on the EarthΔt/t＝ 1.1 x10-18 ）6

１. Introduction

Cassini
INO-a
INO-b
INO-c
INO-d

lambda=1pc

2000AU

20AU

0.2AU

3000km3km

http://rhcole.com/apps/GWplotter/7

１. Introduction：Existing plans for space GW observatories
LISA (ESA/NASA)

B-DECIGO⇒

DECIGO（Japan）

Laser Interferometer Space Anntena

Deci-hertz Interferometer GW Observatory

mHz range

0.1Hz range

0.1 - 100 mHz range

2030 launch

proposed2025­2030

3 satellites at L4 of Sun-Eartharound earth 2000km ３sattelites ⇒ Sun orbit

3 satellites around the Earth

2.50 x 106 km

100 km105 km⇒TianQin 天琴1000 km(China)robust to acceleration noiselight transponder

Fabry-Perot interferometer

Fabry-Perot interferometerrobust to shot-noises
drag-free ﬂight

drag-free ﬂight

drag-free ﬂight

Doppler tracking with Laser beamsame as ground interferometersame as ground interferometer

1702.00786

CQG 28 (2011) 094011

CQG 33 (2016) 035010

8

１. Introduction：Existing plans for space GW observatories
Ni, arXiv:1610.01148

ASTROD=Astrodynamical Space Test of Relativity using Optical Devices

9

2． Doppler tracking of Cassini Saturn Explorer
Cassini 2001-2002 (Armstrong, LRR 2006)
Armstrong et al. ApJ, 599, 806 (2003)

hc(f)G. Cassini (1625-1712)

3x10-15
10-4 Hz
Cassini (1997-2017)atomic clock
troposphere (対流圏)
plasmaradiation pressure of Sun
control technology

10

2． Improvement of Doppler sensitivity（１）Cassini 2001-2002 (Armstrong, LRR 2006)
Armstrong et al. ApJ, 599, 806 (2003)

hc(f)3x10-15
10-4 Hz
Cassini (1997-2017)

troposphere (対流圏)
plasma▼atomic clockin space

radiation pressure of Sun
control technology

11▼

2． Improvement of Doppler sensitivity（2）monitor the time by Opt Lattice Clocks
in 3 satellites
need to make it portable

10-5HzOpt. Lattice Clocktroposphere (対流圏)
plasma▼atomic clock▼

1 AU baseline▼

longer baseline is better to track Doppler shift▶ fuel, power▶ L1, L4, L5 of Sun-Earth orbit
L1=unstable point
L4, L5 = stable pointin space

radiation pressure of Sun
control technology

12

2． Improvement of Doppler sensitivity（3）If light transmission,
no eﬀects from plasma.

need R&D> 107km

10-5Hzatomic clock
troposphereplasmaOpt. Lattice Clock▼▼ ▼1 AU baseline▼▼

If radio transmission,
use two frequency ranges（double tracking）
to check phase diﬀerences due to interplanetary plasmarad. pressure
control technology

in spacelight transmission

13

2． Improvement of Doppler sensitivity（4）required levelh=10-17=0.7mm=2x10-8m/s

Δg/g ≒ 10-12

rad. press. F=P/c
P=1.3 kW/m2
ΔP/P ≒ 1/1000

10-5HzΔa/a ≒ 10-11< 10-121000 kg, 10 m2
10cm 12kW wirelessatomic clock
troposphereplasmaOpt. Lattice Clock▼▼ ▼ ▼

1 AU baseline▼

acceleration
a=5x10-8 m/s2

in spacelight transmission

rad. pressure
solar panel parasol
control technology
no drag-free<latexit sha1_base64="5pN7MY4zB3DFNlfIFPZCHrTwzcc=">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</latexit>phn (f ) = f Sn (f )14

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INO: Interplanetary Network of Optical Lattice Clocks

3. Principle of GW detection
１．Each satellite has Opt Lattice Clock,send out each time to others.
2．Each satellite recognizes
direction・distance・velocity
of others，and we know all of them.

Hisaaki Shinkai (Osaka Inst. Tech.)

GW research exchange meeting, June 14, 201915

INO: Interplanetary Network of Optical Lattice Clocks

3. Principle of GW detection
１．Each satellite has Opt Lattice Clock,send out each time to others.
2．Each satellite recognizes
direction・distance・velocity
of others，and we know all of them.

Hisaaki Shinkai (Osaka Inst. Tech.)

GW research exchange meeting, June 14, 201916

INO: Interplanetary Network of Optical Lattice Clocks

17

3. Principle of GW detection
１．Each satellite has Opt Lattice Clock,send out each time to others.
2．Each satellite recognizes
direction・distance・velocity
of others，and we know all of them(including the potentioal of the Sun.)
Note: eﬀects of planets are O(month).

Hisaaki Shinkai (Osaka Inst. Tech.)

GW research exchange meeting, June 14, 2019

INO: Interplanetary Network of Optical Lattice Clocks

18

3. Principle of GW detection
１．Each satellite has Opt Lattice Clock,send out each time to others.
2．Each satellite recognizes
direction・distance・velocity
of others，and we know all of them(including the potentioal of the Sun.)
Note: eﬀects of planets are O(month).
3．When GW passes, we know its
diﬀerences.
If the events are 〜10s (/yr),then we can calibrate them well.

Hisaaki Shinkai (Osaka Inst. Tech.)

GW research exchange meeting, June 14, 2019<latexit sha1_base64="5pN7MY4zB3DFNlfIFPZCHrTwzcc=">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</latexit>phn (f ) = f Sn (f )19

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22

３．GW obs. using Optical Lattice Clocks：target sources
unequal-mass Binary BH inspiral at 1Gpc
mass ratio q=0.01
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▽
△
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□

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106+104

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▲
▲

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LISA

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10-4
10-1

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frequency [Hz]1 day=8.6x104 s
1 month=2.6x106 s

GW research exchange meeting, June 14, 2019
◆
■

●

INO-c

▲

◆
◆

102+1

■
■

●

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102

INO: Interplanetary Network of Optical Lattice Clocks

23

３．GW obs. using Optical Lattice Clocks：detectable distance
S/N=10z

detectable distance [Mpc]�������� ����� [���] - ����� ���� [������] (���=��)
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104
106
chirp mass M̲c [Msun]

Hisaaki Shinkai (Osaka Inst. Tech.)

GW research exchange meeting, June 14, 2019

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INO: Interplanetary Network of Optical Lattice Clocks

24

３．GW obs. using Optical Lattice Clocks：detectable distance
S/N=100z

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104
106
chirp mass M̲c [Msun]

Hisaaki Shinkai (Osaka Inst. Tech.)

GW research exchange meeting, June 14, 2019

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INO: Interplanetary Network of Optical Lattice Clocks

25

３．GW obs. using Optical Lattice Clocks：detectable distancedetectable distance [Mpc]

LISA

INO-c

mass ratio q=0.2

q=0.2
1702.00786

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INO: Interplanetary Network of Optical Lattice Clocks

26

３．GW obs. using Optical Lattice Clocks：detectable distancedetectable distance [Mpc]mass ratio q=0.2

LISA

INO-c

q=0.2
1702.00786

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GW research exchange meeting, June 14, 2019

27

4．SMBH formation model：IMBHsʼ hierarchical mergers

Halo
Gas Cloud

Massive
Stars

BHs

Globular
Cluster

GalaxyRees, M.J. 1978. Observatory 98: 210

IMBHs

SMBHs

Ebisuzaki +, ApJ, 562, L19 (2001)

28

4．SMBH formation model：IMBHsʼ hierarchical mergers
HS, Kanda, Ebisuzaki, ApJ, 835 (2017) 276 [arXiv:1610.09505]

How many Galaxies in the Universe?

How many BHs in a Galaxy?
n(M)1012 M

10.000

0.001

10 M

0.01

1

M

1.95

10

12

within z=1

10-7

100

M
1

9

10

z<3

within z=5

100

105

104

1000

1 × 1011

5 × 1011

1 × 1012

5 × 1012

BH mass

How many BH mergers in the Universe?

Event Rates at bKAGRA(QNM, S/N=10)zfrequency[Hz]104a = 0.9
a = 0.51000

peak at 60M





100



a = 0.0


10



10

100

1000

104

200 events/yr






MBH /M

range 40M-150M

How many BHs in a Galaxy?
Mass Function of Giant Molecular Clouds
1012
108
104

1

1012 Mgalaxy mass

104

106

109 M

10-4

1

100

GMC mass M

A&A 580, A49 (2015) [arXiv:1505.04696]

29

How many BHs in a Galaxy?
Molecular Clouds
Maximum Core

Building Block BHn(M)Galaxy Mass

105

1012 M
10.000

109 M

0.001

10-7

10

1309.1223v3

100

1000

BH mass

10430

How many BHs in a Galaxy?
Count BHs to form a SMBH

Building Block BHn(M)Galaxy Mass

105

1012 Mn(M)10.000

105

109 M

0.001

100

0.1

10-7

10-4

10

10-7
10

1000

105

107

109

1011

BH mass

100

1000

104

BH mass

31

How many BHs in a Galaxy?
Count BHs to form a SMBH

dynamical friction
n(M)
105
100

0.1

10-4
10-7
10

1000

105

107

109

1011

BH mass

32

How many Galaxies in the Universe?
Count BHs to form a SMBH

(sub-)Galaxy
from Halo modelStar Formation Ratepeak z=3.16

33

How many Galaxies in the Universe?
(1) Halo number density
10-13(3) N of Galaxyz<3within z=5

10

12

M

1

M

1.95

100

10-15

1

10-17

10-19

z=0

10-21

0.01

within z=1

z=5

10-23
1011

1012

1013

1014

1015

1 × 1011

5 × 1011

1 × 1012

5 × 1012(2) N of seeds of Galaxy (subHalo)
1000
500

100
50

10
5

34
1012

1013

1014

1015

http://iopscience.iop.org/article/10.3847/0004-637X/830/2/83
https://www.ras.org.uk/news-and-press/2910-a-universe-of-two-trillion-galaxies

x10 more than before# of galaxy (z<8) : 2x1012# of galaxy 106>Msun
reduces in evolution
35

How many Galaxies in the Universe?
Count BHs to form a SMBH

(sub-)Galaxy
from Halo modelStar Formation Ratepeak z=3.16

36

How many BH mergers in the Universe?
in Standard Cosmology
Nmerger (z)Event Rate R[/yr] =V (D/2.26)

図FStandard Cosmologyzaveraging distances
for all directions

BH massz
BH mass37

38

4．SMBH formation model：IMBHsʼ hierarchical mergers
HS, Kanda, Ebisuzaki, ApJ, 835 (2017) 276 [arXiv:1610.09505]

How many Galaxies in the Universe?

How many BHs in a Galaxy?
n(M)1012 M

10.000

0.001

10 M

0.01

1

M

1.95

10

12

within z=1

10-7

100

M
1

9

10

z<3

within z=5

100

105

104

1000

1 × 1011

5 × 1011

1 × 1012

5 × 1012

BH mass

How many BH mergers in the Universe?

Event Rates at bKAGRA(QNM, S/N=10)zfrequency[Hz]104a = 0.9
a = 0.51000

peak at 60M





100



a = 0.0


10



10

100

1000

104

200 events/yr






MBH /M

range 40M-150M

Event Rates at bKAGRA/aLIGO
Inoue+ MNRAS461(16)4329

Kinugawa+ MNRAS456(15)1093

70-140 /yr

6-400 /Gpc^3/yr

HS+ ApJ 835(17)276
SNR = 10
Event Rate [1/yr]

100
50

10

PRX6(2016)041015

165-210/yr

5

1
0.5

10

LIGO grouppeak at 60M

50

100

500

1000

BH mass (final BH) [M ]

5000

104

39

40

4．SMBH formation model：IMBHsʼ hierarchical mergers
How many BHs in a Galaxy?
n(M)How many Galaxies in the Universe?

1012 M

10.000

0.001

0.01

100

1

M

1.95

10

12

within z=1

10-7

10

M
1

9

10 M

z<3

within z=5

100

105

104

1000

1 × 1011

5 × 1011

1 × 1012

5 × 1012

BH mass

How many BH mergers in the Universe?

Event Rates at B-DECIGO(QNM, S/N=30)
1000

peak at 2800M
1440/yr (spin evol.)1010/yr (spin homo.)

100

10

range 1600M-3x104M

z1

BH mass

100

1000

104

105

106

BH mass [Msun]

銀河中⼼ブラックホールの合体形成モデルと重⼒波観測Summary
4．SMBH formation model：IMBHsʼ hierarchical mergers
SMBH形成をIMBHを経たヒエラルキー合体成⻑モデルと考え，宇宙空間でのイベント数，観測される質量プロファイルを計算した．

Event Rate [/year] (z<5)

eLISA

B-DECIGO

1000

1000

100

100

INO-d

S/N=101

S/N=30
S/N=10101

S/N=1010

0.01

S/N=301

S/N=30

S/N=10010-4

0.10

S/N=100

0.10

103

S/N=100
0.01

104

100

106

108

BH mass [Msun]

0.01

100

104

106

(range: 5.5x103M-3.3x104M)

inspiral+ringdown

inspiral+ringdown

520/year(range: 550M-3.8x105M)
S/N=30

真⾙寿明(⼤阪⼯業⼤学)

100

BH mass [Msun]

S/N=10 18000/year(range: 10M-7.9x104M)
S/N=30 4300/year(range: 10M-3.3x104M)

S/N=10108

6/year2018/09/21 天⽂学会 @ 兵庫県⽴⼤学

104

106

108

BH mass [Msun]

19.2/yr29.8/yr
S/N=10inspiral+ringdown

41

42

4．SMBH formation model：IMBHsʼ hierarchical mergers
Event Rate
INO-c

0.01

S/N=10
10-4

event rate [/yr]event rate [/yr]

1

INO-d

1

S/N=100.01

S/N=100
10-4

S/N=100
100

102

104

106

108

104

106

108

100

102

BH mass [Msun]

19.1/yr

0.35/yrfor S/N=10

inspiral+ringdown

104

106

108

104

106

108

BH mass [Msun]

19.2/yr29.8/yrfor S/N=10

inspiral+ringdown

INO: Interplanetary Network of Optical Lattice Clocks

43

Summary
LISA (ESA/NASA)

B-DECIGO⇒ DECIGO（Japan）

TianQin 天琴

mHz range

0.1Hz range

0.1 - 100 mHz range

0.1 mHz ̶1 Hz

3 satellites around the Earth

Sun-Earth L1-L4-L5

105 km

１ AU

3 satellites at L4 of Sun-Earth around earth 2000km ３sattelites ⇒ Sun orbit
2.50 x 106 km

100 km⇒1000 km(China)INO

light or radio link
light transponder

Fabry-Perot interferometer

Fabry-Perot interferometermonitor time w Opt Lattice
Clocksdrag-free ﬂight

drag-free ﬂight

drag-free ﬂight

no drag-freeDoppler tracking with Laserbeamsame as groundinterferometerrobust to accel. noise

robust to shot-noise

Doppler tracking
available at current tech

⭐Cassiniʼs Doppler tracking (2001-2002) can be improved 3-order mag.
with current technologies
Opt Lattice Clocks，３ satellites in space，Solar panel parasol⭐ ”INO-c”，some range is better than LISA sensitivity⭐ ”INO-c”，stellar-mass BH merger prediction 20 events/yr”INO-d”，+ IMBH inspiral 30 events/yr
Hisaaki Shinkai (Osaka Inst. Tech.)

GW research exchange meeting, June 14, 2019

backup45

3．Previous proposals（Kolkowitz+ 2016）
Kolkowitz +PRD94(2016)124043
3 mHz or 30 mHz‒10 Hz5x107 km or 5x106 km
2 satellites, laser linkcompare freq. w Opt LatticeClockdrag-free ﬂight
Doppler shift with Laser beam
drag-free ﬂight
vs. photoelectric charge bycosmic raysee also
Loeb, Maoz, 1501.00996
Vutha, New J. Phys. 17, 063030

46

3．Previous proposals（Su+ 2018）
DOCS=Double Optical Clocks in SpaceSu, Wang, Wang, Philippe
CQG35 (2018) 05010
0.1 mHz‒10 mHz

Earth-Moon Lagrange its
2 satellites, laser linkcompare freq. w Opt LatticeClockdrag-free ﬂight

at Lagrange points of Earth-Moon orbit, link them with the Earth by radioThe Space-Time Explorer and QUantum Equivalence Principle Space Test (STE-QUEST)
ESA, 2024年打ち上げ予定．地球周回軌道にルビジウム同位体原子干渉計．等価原理検証など．
Primary Atomic Reference Clock in Space (PARCS)
NASAが2008年にセシウム原子時計をISSに搭載しようと計画したものだが，Bushの政策Vision for Space
Exploration (VSE) により中止．
Galileo Global Navigation Satellite System
European GNSS Agency とESAが2019年完成目指して，構築しているヨーロッパ発の非軍事GPS. 各衛星は，水素メーザーとルビジウム原子時計を持つ．
Atomic Clock Ensemble in Space (ACES)ESAによる計画． ISSに，セシウム原子時計(PHARAO)と水素メーザー(SHM) の２つの原子時計を設置するもの．
2020年に打ち上げ予定．
Deep Space Atomic Clock (DSAC)
NASA JPLが計画する，水銀イオン原子時計を用いて，ナビゲーションの精度を高めようとする計画．
2018年，SpaceX Falcon で地球周回軌道に打ち上げ予定．

光格⼦時計を宇宙空間に設置する計画
space optical clock mission (SOC)
ESA. ISSに光格子時計を搭載して，地球重力赤方偏移，太陽重力，等価原理検証を目指そうとするもの．
2010年からスタート．10年後（もうすぐ？）にISS搭載を目指す．
INO-ISS (INO at ISS)
ISSに光格子時計を搭載して，地球重力赤方偏移，等価原理検証を目指そうとするもの．
2018年から検討スタート．2019年JAXA内部検討プログラム．3年後にISS搭載を目指す．