Origin of SMBH?

(1)

真貝寿明 (大阪工業大)

2017/3/7 東京大理安東研セミナー

1

Gravitational Waves from

Merging Intermediate-Mass Black Holes

Origin of SMBH?

GW event rate?

How many BHs in a galaxy?

How many galaxies in the Universe?

真貝・神田・戎崎, ApJ, 835 (2017) 276 [arXiv:1610.09505]

http://www.oit.ac.jp/is/~shinkai/

(2)

1. Gravitational Wave >> Expected Waveform

!25 !20 !15 !10 !5 0 5

!1.0

!0.5 0.0 0.5 1.0

時間

[

ミリ秒

]

合体の時刻重力波の振幅

連星のインスパイラル運動からの重力波波形

ブラックホール形成の重力波波形

× 10 ⁻ ²²

NS-NS NS-BH BH-BH

h

time

Inspiral Merger Ringdown

(3)

http://www.ligo.org/magazine/LIGO-magazine-issue-8.pdf ³

(4)

!25 !20 !15 !10 !5 0 5

!1.0

!0.5 0.0 0.5 1.0

時間

[

ミリ秒

]

× 10 ⁻ ²²

1. Gravitational Wave >> Expected Amplitude

(5)

KAGRA

Typical frequency of BH-‐‑‒BH binary merger @ 1000Mpc

20170307 　真⾙貝

⁵

1. Gravitational Wave >> Expected Events

10 ^-4 0.01 1 100

10 ^-23 10 ^-21 10 ^-19 10 ^-17

S tr ai n S en si ti v it y p S n ( f )[ Hz 1 / 2 ]

frequency [Hz]

f _QNM f _QNM

f _QNM

5R _g 10R _g

50R _g

2R _g

10 M + 10 M 10 ² M + 10

2 M 10 ³ M + 10

3 M 10 ⁴ M + 10

4 M 10 ⁵ M + 10

5 M

(6)

Typical frequency of BH-‐‑‒BH binary merger @ 100Mpc

10 ^-4 0.01 1 100

10 ^-23 10 ^-21 10 ^-19 10 ^-17

S tr ai n S en si ti v it y p S n ( f )[ Hz 1 / 2 ]

frequency [Hz]

10 M + 10 M 10 ² M + 10

2 M 10 ³ M + 10

3 M 10 ⁴ M + 10

4 M

f _QNM f _QNM

f _QNM

5R _g 10R _g

50R _g

2R _g 10 ⁵ M + 10

5 M

1. Gravitational Wave >> Expected Events

KAGRA

(7)

10 ^-4 0.01 1 100 10 ^-23

10 ^-21 10 ^-19 10 ^-17

S tr ai n S en si ti v it y p S n ( f )[ Hz 1 / 2 ]

frequency [Hz]

Typical merger duration of BH-‐‑‒BH binary merger @ 1000Mpc

10 ³ M + 10 ³ M

10M 2h + 10M 12s 12m 0.76s 1.2s 70ms 21h 2m 7.7s

8.9d 20m 1.25m 89d 3.4h 12m

20170307 　真⾙貝

7 1. Gravitational Wave >> Expected Events

(8)

1. Gravitational Wave >> 2015 Detections

LIGO : Laser Interferometer Gravitational-Wave Observatory

4km

Michelson

(9)

http://gwcenter.icrr.u-tokyo.ac.jp/plan/history

3km Michelson Cryogenic (20K)

in quiet mountain site

Sapphira mirrors KAGRA : Kamioka Gravitational wave detector

(Large-scale Cryogenic Gravitational wave Telescope)

神楽（かぐら）

Sinto Music

S tr ai n n oi se am p li tu d e[ 1 / p Hz ]

frequency[Hz]

1 10 100 1000 10⁴

10^-25 10^-22 10^-19 10^-16

Kagra

TOBA

aLIGO aVIRGO

ET

2016/3/25-31, 4/11-25 initial test run, iKAGRA

9

(10)

https://mediaassets.caltech.edu/gwave

2015/9/16--2016/1/15 Observational run 1 2016/11/30—

Observational run 2 LIGO : Laser Interferometer Gravitational-Wave Observatory

1. Gravitational Wave >> 2015 Detections

(11)

GW150914

observed by LIGO L1, H1 source type black hole (BH) binary

date 14 Sept 2015

time 09:50:45 UTC

likely distance 0.75 to 1.9 Gly 230 to 570 Mpc redshift 0.054 to 0.136 signal-to-noise ratio 24

false alarm prob. < 1 in 5 million false alarm rate < 1 in 200,000 yr

Source Masses M⊙

total mass 60 to 70

primary BH 32 to 41

secondary BH 25 to 33

remnant BH 58 to 67

mass ratio 0.6 to 1

primary BH spin < 0.7 secondary BH spin < 0.9

remnant BH spin 0.57 to 0.72 signal arrival time

delay

arrived in L1 7 ms before H1 likely sky position

Southern Hemisphere

likely orientation face-on/off resolved to ~600 sq. deg.

duration from 30 Hz ~ 200 ms # cycles from 30 Hz ~10

peak GW strain 1 x 10

^-21

peak displacement of

interferometers arms ±0.002 fm

frequency/wavelength

at peak GW strain

150 Hz, 2000 km peak speed of BHs ~ 0.6 c peak GW luminosity 3.6 x 10

⁵⁶

erg s

^-1

radiated GW energy 2.5-3.5 M⊙

remnant ringdown freq. ~ 250 Hz

^.

remnant damping time ~ 4 ms

^.

remnant size, area

180 km, 3.5 x 10⁵ km²

consistent with

general relativity?

passes all tests performed graviton mass bound < 1.2 x 10

^-22

eV

coalescence rate of

binary black holes 2 to 400 Gpc

^-3

yr

^-1 online trigger latency

~ 3 min # offline analysis pipelines 5

CPU hours consumed ~ 50 million (=20,000 PCs run for 100 days) papers on Feb 11, 2016 13

# researchers ~1000, 80 institutions in 15 countries

B A C K G R O U N D I M A G E S : T I M E - F R E Q U E N C Y T R A C E ( T O P ) A N D T I M E - S E R I E S

( B O T T O M ) I N T H E T W O L I G O D E T E C T O R S ; S I M U L A T I O N O F B L A C K H O L E H O R I Z O N S ( M I D D L E - T O P ) , B E S T F I T W A V E F O R M ( M I D D L E - B O T T O M )

G W 1 5 0 9 1 4 : F A C T S H E E T

first direct detection of gravitational waves (GW) and first direct observation of a black hole binary

Detector noise introduces errors in measurement. Parameter ranges correspond to 90% credible bounds.

Acronyms: L1=LIGO Livingston, H1=LIGO Hanford; Gly=giga lightyear=9.46 x 10¹² km; Mpc=mega parsec=3.2 million lightyear, Gpc=10³Mpc, fm=femtometer=10^-15 m, M⊙=1 solar mass=2 x 10³⁰kg

(12)

observed by LIGO L1, H1 source type black hole (BH) binary

date 14 Sept 2015

time 09:50:45 UTC

likely distance 0.75 to 1.9 Gly 230 to 570 Mpc redshift 0.054 to 0.136 signal-to-noise ratio 24

false alarm prob. < 1 in 5 million false alarm rate < 1 in 200,000 yr

Source Masses M⊙

total mass 60 to 70

primary BH 32 to 41

secondary BH 25 to 33

remnant BH 58 to 67

mass ratio 0.6 to 1

primary BH spin < 0.7 secondary BH spin < 0.9

remnant BH spin 0.57 to 0.72 signal arrival time

delay arrived in L1 7 ms before H1 likely sky position Southern Hemisphere

likely orientation face-on/off resolved to ~600 sq. deg.

duration from 30 Hz ~ 200 ms # cycles from 30 Hz ~10

peak GW strain 1 x 10^-21 peak displacement of

interferometers arms ±0.002 fm frequency/wavelength

at peak GW strain 150 Hz, 2000 km peak speed of BHs ~ 0.6 c peak GW luminosity 3.6 x 10⁵⁶ erg s^-1 radiated GW energy 2.5-3.5 M⊙

remnant ringdown freq. ~ 250 Hz ^. remnant damping time ~ 4 ms ^. remnant size, area 180 km, 3.5 x 10⁵ km²

consistent with

general relativity? passes all tests performed graviton mass bound < 1.2 x 10^-22eV

coalescence rate of

binary black holes 2 to 400 Gpc^-3yr^-1 online trigger latency ~ 3 min # offline analysis pipelines 5

CPU hours consumed ~ 50 million (=20,000 PCs run for 100 days) papers on Feb 11, 2016 13

# researchers ~1000, 80 institutions in 15 countries B A C K G R O U N D I M A G E S : T I M E - F R E Q U E N C Y T R A C E ( T O P ) A N D T I M E - S E R I E S

( B O T T O M ) I N T H E T W O L I G O D E T E C T O R S ; S I M U L A T I O N O F B L A C K H O L E H O R I Z O N S ( M I D D L E - T O P ) , B E S T F I T W A V E F O R M ( M I D D L E - B O T T O M )

G W 1 5 0 9 1 4 : F A C T S H E E T

first direct detection of gravitational waves (GW) and first direct observation of a black hole binary

Detector noise introduces errors in measurement. Parameter ranges correspond to 90% credible bounds.

Acronyms: L1=LIGO Livingston, H1=LIGO Hanford; Gly=giga lightyear=9.46 x 10¹² km; Mpc=mega parsec=3.2 million lightyear, Gpc=10³Mpc, fm=femtometer=10^-15 m, M⊙=1 solar mass=2 x 10³⁰kg

13億光年先

（400 170 Mpc）

（z=0.054̶0.136）

36Msun + 29 Msun

のBHが合体して 62 Msun

（3 Msun分の質量が消失）

重力波が検出された！

重力波が検出できた！

BHが存在した！

BH連星が存在した！

相対論が第0近似として正しい！

(13)

https://www.ligo.caltech.edu/system/avm̲image̲sqls/binaries/57/page/Black̲Hole̲Mass̲Chart.jpg?1465864737

BHs!

29M+36M=62M 7M+14M=20M

why not more?

(14)

1. Gravitational Wave >> Expected Waveform

!25 !20 !15 !10 !5 0 5

!1.0

!0.5 0.0 0.5 1.0

時間

[

ミリ秒

]

× 10 ⁻ ²²

NS-NS NS-BH BH-BH

Inspiral Merger Ringdown

h

time

(15)

KAGRA

Typical frequency of BH-‐‑‒BH binary merger @ 1000Mpc

15 1. Gravitational Wave >> Expected Events

10 ^-4 0.01 1 100

10 ^-23 10 ^-21 10 ^-19 10 ^-17

S tr ai n S en si ti v it y p S n ( f )[ Hz 1 / 2 ]

frequency [Hz]

f _QNM f _QNM

f _QNM

5R _g 10R _g

50R _g

2R _g

10 M + 10 M 10 ² M + 10

2 M 10 ³ M + 10

3 M 10 ⁴ M + 10

4 M 10 ⁵ M + 10

5 M

(16)

S tr ai n n oi se am p li tu d e[ 1 / p Hz ]

frequency[Hz]

1 10 100 1000 10⁴

10^-25 10^-22 10^-19 10^-16

Kagra

TOBA

aLIGO aVIRGO

ET

10 100 1000 10 ⁴

a = 0.0

a = 0.5 a = 0.9

M _BH /M

fr eq u en cy [Hz ]

地上での重力波干渉計感度

BH quasi-normal freq.

(ringdown freq.)

BH < 2000Msun can be a target

IMBH ringdown freq. is detectable at LIGO/KAGRA

10Hz 1000Hz

1000M 100M

10 100 f _qnm = c ³

2⇡ GM _T 1 0.63(1 a) ^0.3

(17)

Rees, M.J. 1978. Observatory 98: 210 17

2. Model of SMBH

(18)

Volonteri, Science 337 (2012) 544

2. Model of SMBH

(19)

2. Model of SMBH

Greene, Nature Comm 3 (2012) [arXiv:1211.7082]

19

(20)

Gas Cloud

BHs

IMBHs

SMBHs

Halo

Galaxy Globular

Cluster Massive

Stars

2. Model of SMBH

(21)

21 Yagi, CQG 29 075005 (2012) [arXiv:1202.3512]

HLX-1 has 20,000M BH!

http://hubblesite.org/newscenter/archive/releases/2012/2012/11/full/

Starburst galaxy M82 has 1000M BH

BHs

IMBHs

SMBHs

Matsushita+, ApJ, 545, L107 (2000) Matsumoto+, ApJ, 547, L25 (2001)

Ebisuzaki +, ApJ, 562, L19 (2001)

(22)

0.15pc from SgrA*

1-2 x 10 ⁴ Msun

1602.05325

(23)

PortegiesZwart+, ApJ 641(2006)319

23

(24)

BHs

IMBHs

SMBHs

'Missing link' founded

Ebisuzaki +, ApJ, 562, L19 (2001)  

(1)formation of IMBHs by runaway mergers of massive stars in dense star clusters,

(2) accumulations of IMBHs at the center region of a galaxy due to sinkages of clusters by dynamical friction

(3) mergings of IMBHs by multi-body interactions and gravitational radiation.

Marchant & Shapiro 1980; Portegies Zwart et al. 1999;

Portegies Zwart & McMillan 2002;

Portegies Zwart et al. 2004;

Holger & Makino 2003

Matsubayashi et al. 2007

Iwasawa et. al. 2010

雰囲気（巡り逢い）＋仲良し成長モデル

(25)

(26)

(27)

Matsubayashi, HS, Ebisuzaki, ApJ 614 (2004) 864

IMBH-IMBH mergers produce low freq. GW

27

(28)

(29)

Matsubayashi, HS, Ebisuzaki, ApJ 614 (2004) 864

29

(30)

How many BH mergers in the Universe?

How many BH mergers we observe in a year?

How many BHs in a galaxy?

How many galaxies in the Universe?

Detectable Distance ? KAGRA/aLIGO/aVIRGO Cosmological model?

BH spin? Signal-to-Noise?

(31)

31 Mass Function of Giant Molecular Clouds

1 100 10 ⁴ 10 ⁶

10 ^-4 1 10 ⁴ 10 ⁸ 10 ¹²

M 10 ¹² M

10 ⁹ M

galaxy mass

GMC mass

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

How many BHs in a Galaxy?

(32)

10 100 1000 10 ⁴ 10 ^-7

0.001 10.000 10 ⁵

1309.1223v3

10 ¹² M

10 ⁹ M

Galaxy Mass n(M)

BH mass

Molecular Clouds

Maximum Core

Building Block BH

How many BHs in a Galaxy?

(33)

33 Count BHs to form a SMBH

10 1000 10⁵ 10⁷ 10⁹ 10¹¹

10^-7 10^-4 0.1 100 10⁵

10 100 1000 10 ⁴

10 ^-7 0.001 10.000 10 ⁵

10 ¹² M

10 ⁹ M

Galaxy Mass n(M)

BH mass

Building Block BH

BH mass n(M)

How many BHs in a Galaxy?

(34)

Count BHs to form a SMBH

10 1000 10⁵ 10⁷ 10⁹ 10¹¹

10^-7 10^-4 0.1 100 10⁵

dynamical friction

n(M)

How many BHs in a Galaxy?

(35)

35 (sub-)Galaxy

from Halo model

Star Formation Rate

peak z=3.16

Count BHs to form a SMBH

How many Galaxies in the Universe?

(36)

36

10¹¹ 10¹² 10¹³ 10¹⁴ 10¹⁵

10^-23 10^-21 10^-19 10^-17 10^-15 10^-13

z = 0 z = 5

5 10 50 100 500 1000

(1) Halo number density

(2) N of seeds of Galaxy (subHalo)

(3) N of Galaxy

within z=1 within z=5

M ¹

1×10¹¹ 5×10¹¹ 1×10¹² 5×10¹²

0.01 1 100

M ^1.95

How many Galaxies in the Universe?

z<3

10 ¹²

(37)

37 https://www.ras.org.uk/news-and-press/2910-a-universe-of-two-trillion-galaxies

http://iopscience.iop.org/article/10.3847/0004-637X/830/2/83

x10 more than before

# of galaxy (z<8) : 2x10 ¹²

# of galaxy 10 ⁶ >Msun  

reduces in evolution

(38)

(sub-)Galaxy

from Halo model

Star Formation Rate

peak z=3.16

Count BHs to form a SMBH

How many Galaxies in the Universe?

(39)

McConnell-Ma

ApJ 764(2013)184

39

(40)

図F

BH mass

z z

in Standard Cosmology

How many BH mergers in the Universe?

Event Rate R[/yr] = N _merger (z) V (D/2.26)

Standard Cosmology

averaging distances

for all directions

(41)

Signal-to-Noise Ratio (SNR)

S tr a in n o is e am p li tu d e[ 1 / √ Hz]

frequency[Hz]

Kagra

TOBA

aLIGO aVIRGO

ET

41

(42)

Detectable Distances at bKAGRA

Hierarchical Growth

⇢ ² = 8 5

✏ _r (a) f _R ²

(1 + z)M S _h (f _R /(1 + z))

✓ (1 + z)M d _L (z )

◆ 2 ✓ 4µ M

◆ 2

SNR

Energy emission=4% of total M，1% at ringdown Flanagan&Hughes, PRD57(198)4535

Standard Cosmology

a = 0.9

KAGRA KAGRA

(43)

Slide copy from Hiroyuki Nakano

43 GW150914

4.7% of mass emitted

in total 2.8% of mass

emitted by ISCO

1% of mass

emitted

in ringdown?

(44)

図F

BH mass

z z

in Standard Cosmology

How many BH mergers in the Universe?

Event Rate R[/yr] = N _merger (z) V (D/2.26)

Standard Cosmology

averaging distances

for all directions

(45)

Event Rates at bKAGRA

BH spin=0.9,0.5,0.0

peak at 60M

range 40M-150M

7 events/yr

210 events/yr

45

(46)

Event Rates at bKAGRA/aLIGO

7 events/yr

peak at 60M

BH mass (final BH) [M ] BH mass (final BH) [M ]

E ve n t R at e [1 / yr]

(a1) SNR=10, KAGRA (a2) SNR=10, KAGRA

10 50 100 500 1000 5000 10⁴

0.5 1 5 10 50 100

N merger

10 50 100 500 1000 5000 10⁴

10⁷ 10⁸ 10⁹ 10¹⁰ 10¹¹ 10¹²

range 40M-150M

210 events/yr

LIGO group [1602.03842]

Inoue+ MNRAS461(16)4329

6-400 /Gpc^3/yr

Kinugawa+ MNRAS456(15)1093

70-140 /yr

(47)

Event Rates at bKAGRA/aLIGO

7 events/yr

peak at 60M

BH mass (final BH) [M ] BH mass (final BH) [M ]

E ve n t R at e [1 / yr]

(a1) SNR=10, KAGRA (a2) SNR=10, KAGRA

10 50 100 500 1000 5000 10⁴

0.5 1 5 10 50 100

N merger

10 50 100 500 1000 5000 10⁴

10⁷ 10⁸ 10⁹ 10¹⁰ 10¹¹ 10¹²

range 40M-150M

210 events/yr

LIGO group PRX6(2016)041015

Inoue+ MNRAS461(16)4329

6-400 /Gpc^3/yr

Kinugawa+ MNRAS456(15)1093

70-140 /yr

47

(48)

10 ^-4 0.01 1 100 10 ^-23

10 ^-21 10 ^-19 10 ^-17

S tr ai n S en si ti v it y p S n ( f )[ Hz 1 / 2 ]

frequency [Hz]

Sensitivity of Space GW Interferometers

10 ³ M + 10

3 M

10 ² M + 10

2 M 10 ⁴ M + 10

4 M

(49)

10 ^-4 0.01 1 100 10 ^-23

10 ^-21 10 ^-19 10 ^-17

10 ³ M + 10

3 M

10 ² M + 10

2 M 10 ⁴ M + 10

4 M

S tr ai n S en si ti v it y p S n ( f )[ Hz 1 / 2 ]

frequency [Hz]

Sensitivity of Space GW Interferometers

49

(50)

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

これは遊べる GWplotter

(51)

10⁵ 10⁶ 10⁷ 10⁸ 10⁷

10⁸ 10⁹ 10¹⁰ 10¹¹ 10¹²

観測できるBH数分布 1年間で観測できるBH数分布

(S/N=10)

spin 0.9

spin 0

BH質量[Msun]

年55個

10⁴ 10⁵ 10⁶ 10⁷ 10⁸

0.10 1 10 100

10⁴ 10⁵ 10⁶ 10⁷ 10⁸ 10⁹

10 100 1000 10⁴

観測できるBH合体距離 (S/N=10)

BH質量[Msun]

[Mpc]

10^-4 0.01 1 100

10^-23 10^-21 10^-19 10^-17

eLISA N2A5

51 Event Rates at eLISA

(52)

観測できるBH数分布 1年間で観測できるBH数分布

(S/N=10)

spin 0.9

spin 0

BH質量[Msun]

観測できるBH合体距離 (S/N=10)

BH質量[Msun]

[Mpc]

10^-4 0.01 1 100

10^-23 10^-21 10^-19 10^-17

PreDECIGO

100 1000 10⁴ 10⁵ 10⁶ 10⁷

0.10 1 10 100 1000

100 1000 10⁴ 10⁵ 10⁶ 10⁷

10⁷ 10⁹ 10¹¹ 10¹³

1 10 100 1000 10⁴ 10⁵ 10⁶

1 10 100 1000 10⁴ 10⁵

Event Rates at PreDECIGO

(53)

100 1000 10⁴ 10⁵ 10⁶ 10⁷ 10⁷

10⁹ 10¹¹ 10¹³

観測できるBH数分布 1年間で観測できるBH数分布

(S/N=30)

spin 0.9

spin 0

BH質量[Msun]

観測できるBH合体距離 (S/N=30)

BH質量[Msun]

[Mpc]

10^-4 0.01 1 100

10^-23 10^-21 10^-19 10^-17

PreDECIGO

1 10 100 1000 10⁴ 10⁵ 10⁶

10 100 1000 10⁴

100 1000 10⁴ 10⁵ 10⁶ 10⁷

0.10 1 10 100

1000 年4850個

53 Event Rates at PreDECIGO

(54)

BH spin=0.9,0.5,0.0

まとめ

重力波検出のデータを蓄積することによって，銀河分布やSMBH形成シナリオを特定したり，宇宙膨張モデルの検証や，重力理論の検証が可能になる．

Origin of SMBH?

1

Gravitational Waves from

Merging Intermediate-Mass Black Holes

Origin of SMBH?

GW event rate?

How many BHs in a galaxy?

How many galaxies in the Universe?

http://www.oit.ac.jp/is/~shinkai/

1. Gravitational Wave >> Expected Waveform

[

]

× 10 − 22

NS-NS NS-BH BH-BH

h

time

Inspiral Merger Ringdown

http://www.ligo.org/magazine/LIGO-magazine-issue-8.pdf 3

[

]

× 10 − 22

1. Gravitational Wave >> Expected Amplitude

KAGRA

Typical frequency of BH-‐‑‒BH binary merger @ 1000Mpc

5

1. Gravitational Wave >> Expected Events

10 -4 0.01 1 100

10 -23 10 -21 10 -19 10 -17

S tr ai n S en si ti v it y p S n ( f )[ Hz 1 / 2 ]

frequency [Hz]

f QNM f QNM

f QNM

5R g 10R g

50R g

2R g

10 M + 10 M 10 2 M + 10

2 M 10 3 M + 10

3 M 10 4 M + 10

4 M 10 5 M + 10

5 M

Typical frequency of BH-‐‑‒BH binary merger @ 100Mpc

10 -4 0.01 1 100

10 -23 10 -21 10 -19 10 -17

S tr ai n S en si ti v it y p S n ( f )[ Hz 1 / 2 ]

frequency [Hz]

10 M + 10 M 10 2 M + 10

2 M 10 3 M + 10

3 M 10 4 M + 10

4 M

f QNM f QNM

f QNM

5R g 10R g

50R g

2R g 10 5 M + 10

5 M

1. Gravitational Wave >> Expected Events

KAGRA

10 -4 0.01 1 100 10 -23

10 -21 10 -19 10 -17

S tr ai n S en si ti v it y p S n ( f )[ Hz 1 / 2 ]

frequency [Hz]

Typical merger duration of BH-‐‑‒BH binary merger @ 1000Mpc

10 3 M + 10 3 M

10M 2h + 10M 12s 12m 0.76s 1.2s 70ms 21h 2m 7.7s

8.9d 20m 1.25m 89d 3.4h 12m

7

1. Gravitational Wave >> Expected Events

1. Gravitational Wave >> 2015 Detections

LIGO : Laser Interferometer Gravitational-Wave Observatory

4km

Michelson

http://gwcenter.icrr.u-tokyo.ac.jp/plan/history

3km Michelson Cryogenic (20K)

in quiet mountain site

Sapphira mirrors KAGRA : Kamioka Gravitational wave detector

(Large-scale Cryogenic Gravitational wave Telescope)

神楽（かぐら）

Sinto Music

S tr ai n n oi se am p li tu d e[ 1 / p Hz ]

frequency[Hz]

× 10 ⁻ ²²

http://www.ligo.org/magazine/LIGO-magazine-issue-8.pdf ³

× 10 ⁻ ²²

⁵

10 ^-4 0.01 1 100

10 ^-23 10 ^-21 10 ^-19 10 ^-17

f _QNM f _QNM

f _QNM

5R _g 10R _g

50R _g

2R _g

10 M + 10 M 10 ² M + 10

2 M 10 ³ M + 10

3 M 10 ⁴ M + 10

4 M 10 ⁵ M + 10

10 ^-4 0.01 1 100

10 ^-23 10 ^-21 10 ^-19 10 ^-17

10 M + 10 M 10 ² M + 10

2 M 10 ³ M + 10

3 M 10 ⁴ M + 10

f _QNM f _QNM

f _QNM

5R _g 10R _g

50R _g

2R _g 10 ⁵ M + 10

10 ^-4 0.01 1 100 10 ^-23

10 ^-21 10 ^-19 10 ^-17

10 ³ M + 10 ³ M

× 10 ⁻ ²²

10 ^-4 0.01 1 100

10 ^-23 10 ^-21 10 ^-19 10 ^-17

f _QNM f _QNM

f _QNM

5R _g 10R _g

50R _g