Gravitational Wave Physics & Astronomy, Status of KAGRA
Underground and Cryogenic interferometric 3 km gravitational-wave detector at Kamioka, Japan
Contents
1. Gravitational Wave Overview
2. LIGO-Virgo-KAGRA Observational Results
3. The KAGRA interferometer
4. Outlook of GW Astronomy(c) KAGRA Collaboration / Rey.Hori

Hisaaki Shinkai (Osaka Inst. Tech.)
真貝寿明（大阪工業大学）
KAGRA Scientiﬁc Congress, board chair
JGW-G2113045

on behalf of KAGRA collaboration

Cosmology from Home 2021 July

Gravitational Wave Physics & Astronomy, Status of KAGRA

Contents
1. Gravitational Wave Overview
2. LIGO-Virgo-KAGRA Observational Results
3. The KAGRA interferometer
4. Outlook of GW Astronomy(c) KAGRA Collaboration / Rey.Hori

Hisaaki Shinkai (Osaka Inst. Tech.)
真貝寿明（大阪工業大学）
KAGRA Scientiﬁc Congress, board chair
on behalf of KAGRA collaboration

Cosmology from Home 2021 July

1. Gravitational Waves

First Detection (2015 Sep 14)

2017 Nobel PrizeFeb 2016, LIGO announced the ﬁrst detectionof GW (GW150914). The source was Binary BHs.

Oct 2017，LIGO/Virgo announced
the ﬁrst GW detection from Binary NSs (GW170817).

Oct 2017，Royal Swedish academy of scienceannounced the physics prize goes to GW
project.

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

3

Gravitational Wave
from binary BH-BH, NS-NS, BH-NS

typical amplitude 10-22

1. Gravitational Waves

Sources of Gravitational Waves
supernovae

pulsars

black holebinary neutron stars
binary black holes

hard to predict

too small
amplitude

too small
amplitude

The Target

signal = noise + gw
[dimensionless]

GW151226

standard way is to use matched ﬁltering techniquenecessary for GW templates in hand
http://gwcenter.icrr.u-tokyo.ac.jp

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

5

1. Gravitational Waves

What we can learn from GW (from a binary merger) ?
merger phase
振幅
amplitude



1.0

0.5

  
 inspiral


phase


ringdown
phase

0.0

-0.5

合体後の質量・角運動量mass, spin

http://ligo.org/detections/GW170104.php

重力理論の検証
test of GR-1.0

質量・スピン・軌道パラメータ・距離・潮汐力・偏光
mass,spin, orbital parameters, tidal, distance, polarization<latexit sha1_base64="Mh04teE7hG94yDnvEuA6v6XDv3E=">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</latexit>(m1 , m2 , s1 , s2 , ◆, n,
tc , 'c , , r)連星形成シナリオ
原子核状態方程式

-25

-20

-15

-10

-5

nuclear matter EOS
統計

宇宙論パラメータ
銀河形成シナリオ
binary formation
scenario

statistics

galaxy formation scenario

0

時間

5

究極理論の構築
uniﬁedtheorycosmological parameters
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

6

1. Gravitational Waves

Sensitivity requirements for the detectors
vibration control(thermal noise)

power spectral density(seismic noise)

thermal control

initial LIGO
(̶2010)advanced LIGO
(2015‒-)(shot noise)high-power
laser control

Science 256 (1992) 325
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

7

1. Gravitational Waves

Sensitivity requirements for the detectors
GW151226

characteristic strain[dimensionless]
spectral density [sec]power spectral density

signal = noise + gw
[dimensionless]power spectral density[1/ Hz]Science 256 (1992) 325
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

8

1. Gravitational Waves

Sensitivity requirements for the detectors

characteristic strain

http://gwplotter.com

Science 256 (1992) 325
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

9

1. Gravitational Waves

What kind of technology we need?

power spectral density

http://gwplotter.com

Science 256 (1992) 325
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

10

Gravitational Wave Projects

We need more
detectors
forbetterlocalization!
GW International Network

4 km

4 km

600 m
3 km

3 km
7
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

11

Gravitational Wave Projects

LIGO, Virgo and KAGRA

North [deg]LIGO-Livingston
50

LHO

Virgo

Virgo

LLO

KAGRA

South [deg]LIGO-Hanford

KAGRA

0

KAGRA

KAGRA
-50

LIGO-Hanford
-150

-100

-50

West [deg]

0

50

100

150

East [deg]more precise GW source localization
more certain GW source parameters
more chances to hunt GW events
more information of GW polarization
more ideas for GW researches

LIGO-Livingstone

Virgo

Virgo

more man power
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

12

Gravitational Wave Projects

Sensitivity Curve

Binary NS range

LVK collaboration, Living Rev Relativ (2020) 23:3
https://link.springer.com/article/10.1007/s41114-020-00026-9

Science 256 (1992) 325[1304.0670ver2020Jan]

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

13

Gravitational Wave Projects

Observation Period

1h(t) /
r

O1<latexit sha1_base64="Nqkk9BXaevHaLwHVW6nLBLByEfk=">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</latexit>

amplitude of GW

1/ distance

if we improve one-order of magnitude of the sensitivity,

80
Mpc

LIGO

then the observational volume of the Universe
become 103 times larger.

O3

O2
100
Mpc

O5

110-130
Mpc

160-190
Mpc

Target
330 Mpc

50
Mpc

90-120Mpc

150-260
Mpc

25-130
Mpc

130+
Mpc

30
Mpc

Virgo

O4

1
Mpc

KAGRA

Target
330 Mpc

LIGO-India
2015

2016

2017

2018

2019

2020

2021 2022

2023

2024

2025

2026

LIGO-G2002127-v4

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

14

Gravitational Wave Physics & Astronomy, Status of KAGRA
Contents
1. Gravitational Wave Overview
2. LIGO-Virgo-KAGRA Observational Results
3. The KAGRA interferometer
4. Outlook of GW Astronomy

https://antimatterwebcomics.com/comic/physics-nobel-prize-2017/https://antimatterwebcomics.com/comic/gw170817/

Cosmology from Home 2021 July

２. LV & LVK Observational Results

In 5 years, …
Six years ago, GW physics was a “future story”. We did not know the existence of BBH, BH over 10 solar mass (except SMBH).
Now LIGO/Virgo announced 50 events in October 2020 as GWTC-2 up to their O3a.

➡ 3BHBH➡ +4BHBH➡ +1NSNS2015 Sep 14
Editor was suspicious
to put GW in the title.

➡ +39BHBH➡ +1NSNS➡ +2BH+?

▲Today“GW will be detected
within a couple of years. ”

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

16

２. LV & LVK Observational Results

GW150914

The First Detection of GW 36M+29M=62M
GW150914:FACTSHEETBACKGROUND IMAGES: TIME-FREQUENCY TRACE (TOP) AND TIME-SERIES( 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 AT I O N O F B L A C K H O L E
HORIZONS (MIDDLE-TOP), BEST FIT WAVEFORM (MIDDLE-BOTTOM)

first direct detection of gravitational waves (GW) and first direct observationof a black hole binary
observed by

LIGO L1, H1

duration from 30 Hz~ 200 mssource typeblack hole (BH) binary# cycles from 30 Hz

~10

date

14 Sept 2015

peak GW strain

1 x 10-21

time

09:50:45 UTC±0.002 fm

likely distance

0.75 to 1.9 Gly
230 to 570 Mpc

peak displacement ofinterferometers arms

150 Hz, 2000 km

redshift

0.054 to 0.136

frequency/wavelength
at peak GW strain

signal-to-noise ratio

24

peak speed of BHs~ 0.6 cpeak GW luminosity

3.6 x 1056 erg s-1

false alarm prob.

< 1 in 5 million

radiated GW energy

2.5-3.5 M⊙

false alarm rate

< 1 in 200,000 yr

remnant ringdown freq.

~ 250 Hzremnant damping time

~ 4 ms

Source Masses＊The First Detection of GW＊Existence of Binary BH＊Existence of BH at 30MM⊙

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 timedelay

arrived in L1 7 ms
before H1

likely sky position

Southern Hemispherelikely orientation
resolved toface-on/off~600 sq. deg.

.

.

remnant size, area

180 km, 3.5 x 105 km2

consistent withgeneral relativity?

passes all tests
performed

graviton mass bound< 1.2 x 10-22 eV

coalescence rate ofbinary black holes

2 to 400 Gpc-3 yr-1

online trigger latency~ 3 min# offline analysis pipelines5

CPU hours consumed~ 50 million (=20,000
PCs run for 100 days)

papers on Feb 11, 201613

# researchers~1000, 80 institutionsin 15 countries

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 10 12 km; Mpc=megaparsec=3.2 million lightyear, Gpc=10 3 Mpc, fm=femtometer=10 -15 m, M⊙=1 solar mass=2 x 10 30 kg

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

17

２. LV & LVK Observational Results

GW150914

The First Detection of GW 36M+29M=62M★ Distance was determined（400±170 Mpc，z=0.054̶0.136）
but not a particular direction★Comparing with various simulations,binary parameters were determined.
arXiv:1606.01262

Localization and broadband follow-up of thegravitational-wave transient GW150914
This article is under preparation by the LIGO Scientific Collaboration, the Virgo collaboration,and partner observing facilities. The full version will be posted on or after February 15, 2016. It
will describe the rapid detection and position reconstruction of the gravitational-wave signal andthe broadband follow-up campaign by 21 teams of observers, spanning radio, optical, nearinfrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities.

LALInference sky map (GCN 18858) Mollweide projection plot

600 squared degree

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

18

２. LV & LVK Observational Results

GW170817

First Binary Neutron Stars & Follow-up Observations
GW170817 FACTSHEET＊First detection from binary NSs
LIGO Hanford＋Livingston + Virgo
Inspiral period 60 sec，150 cycles．

observed by

H, L, Vsource typebinary neutron star (NS)datelocalization 30 sq. degtime of merger
signal-to-noise ratio
false alarm rate

17 August 201712:41:04 UTC
32.4< 1 in 80 000 years

27 min: Alert for astronomers

distance

85 to 160 million
light-years

5h14m: location information sent out

total mass2.73 to 3.29 M⦿

primary NS mass

1.36 to 2.26 M⦿

secondary NS mass

0.86 to 1.36 M⦿

1.74 sec: GRB was detected.

mass ratio

0.4 to 1.0

inferred duration from 30
Hz to 2048 Hz**~ 60 sinferred # of GW cycles
from 30 Hz to 2048 Hz**~ 3000initial astronomer alert
latency*

27 min

HLV sky map alert latency*
HLV sky area†# of EM observatories that
followed the trigger
also observed inhost galaxy

radiated GW energy> 0.025 M⦿c2

source RA, Dec

radii of NSs

likely ≲ 15 km

sky location

Multi-Messenger Astronomy was establishedeffective spinparameter-0.01 to 0.17

Opt, IR, X-ray, gamma-ray, ….

effective precession
spin parameter

unconstrained

viewing angle(without and with hostgalaxy identification)

GW speed deviationfrom speed of light< few parts in 1015

Hubble constant inferredfrom host galaxy
identification

5 hrs 14 min
28 deg2~ 70
gamma-ray, X-ray,ultraviolet, optical,
infrared, radio

NGC 4993
13h09m48s, -23°22’53"

in Hydra constellation≤ 56° and ≤ 28°

62 to 107 km s-1 Mpc-1

Announced October 2017.
62 papers and preprints appeared on the
day of press release.

Fermi & INTEGRAL detected GRB
1.7 sec later the merger.

Images: time frequency traces (top), GW sky map(left, HL = light blue, HLV = dark blue,
improved HLV = green,
optical source location = cross-hair)

PRL 119 (2017) 161101

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

GW=gravitational wave, EM = electromagnetic,M⊙=1 solar mass=2x1030 kg,
H/L=LIGO Hanford/Livingston, V=Virgo
Parameter ranges are 90% credible intervals.
*referenced to the time of merger**maximum likelihood estimate†90% credible region19

２. LV & LVK Observational Results

GW170817

First Binary Neutron Stars & Follow-up Observations＊First detection from binary NSs
LIGO Hanford＋Livingston + Virgo
Inspiral period 60 sec，150 cycles．
localization 30 sq. deg
27 min: Alert for astronomers
5h14m: location information sent out
1.74 sec: GRB was detected.
Multi-Messenger Astronomy was establishedOpt, IR, X-ray, gamma-ray, ….
Announced October 2017.
62 papers and preprints appeared on the
day of press release.

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

20

２. LV & LVK Observational Results

GW170817

First Binary Neutron Stars & Follow-up Observations
The Astrophysical Journal Letters, 848:L12 (59pp), 2017 October 20

Abbott et al.

★ Sky localization < 30 sq. degree; amplitude and Mc predict distance 40+8-14 Mpc★ Follow-up obs identiﬁed the source．Lens Galaxy NGC4993 at 40 Mpc

Figure 2. Timeline of the discovery of GW170817, GRB 170817A, SSS17a/AT 2017gfo, and the follow-up observations are shown by messenger and wavelength
relative to the time tc of the gravitational-wave event. Two types of information are shown for each band/messenger. First, the shaded dashes represent the times when
information was reported in a GCN Circular. The names of the relevant instruments, facilities, or observing teams are collected at the beginning of the row. Second,
representative observations (see Table 1) in each band are shown as solid circles with their areas approximately scaled by brightness; the solid lines indicate when the21

２. LV & LVK Observational Results

GW170817

First Binary Neutron Stars & Follow-up Observations

Model NSNS merger explodes a lot of matters

Observation▶ heavy nuclear matters via r-process▶ heat up by β-decay & nuclear ﬁssion, photons are trapped▶ expanded and cooled，a lot of photons are emitted (Kilonova）★ bright in visible band（blue kilonova）▶ few Lanthanoids
strong in IR later（red kilonova）▶ much Lanthanoids

Period★ heavy elements 0.03 Msun were emitted at 10-20% of the light speed
1
IA
1

1

18
VIII A
±1

H

1s

2

+1 4

2s

Li

Be
w K~
beryllium

6.941

3

3s

4s

K

Ca
O[K~
calcium

7s

4
IV B

Sr

]gbK~
strontium+3 22850'
90' 5/C%



5
VB

6
VI B

7
VII B

8
VIII B

9
VIII B

10
VIII B

12
II B

3p

+4,3,2 23+5,2,3,4 24+3,2,6 25+2,3,4,6,7 26+3,2 27+2,3 28+2,3 29+2,1 30

Sc

Ti

V

Cr

Mn

Fe

Co

Ni

Cu

Zn

b`
titaniumni\K~vanadiumS~chromium|Pmanganese

1
iron

Wng
cobaltjcU
nickel4copper

2
zinc

44.96

47.87

50.94

52.00

54.94

55.85

58.93

58.69

63.55

+3 40

+4 41

+5,3 42+6,3,5 43+7,4,6 44+4,3,6,8 45+3,4,6 46

C

N

O

F

Ne

&'
nitrogen.'oxygensc'
fluorine

kN
neon

12.01

Y

Zr

Nb

Mo

Tc

Ru

Rh

Pd

Ag

Cd

\WjK~
zirconium

jNt
niobium

 tf
molybdenum

eSkbK~
technetium

ejK~
ruthenium\K~rhodiumo\K~palladium3
silverOh}K~cadmium

91.22

92.91

95.94

98

101.1

102.9

106.4

107.9

14.01

16.00

4 15

19.00

3 16

2 17

87.62

+1 56

88.91

+2

Cs

Ba

_[K~
cesiumn K~barium72

57 71

† 5d

Fr

Ra

s[K~
francium\K~radium

223

226

† 4f

+4,6,8 77+4,3,6 78+4,2 79

Si

P

S

Cl

Ar

UJ'
silicon
phosphorus$6
sulfur'
chlorine

IX
argon

26.98

28.09

30.97

32.07

+3 32

+4,2 33

35.45

3 34

2 35

Ga

Ge

As

Se

Br

Kr

V|jK~
germaniump'arsenic_selenium('bromineS ug
krypton

72.64

74.92

+3 50

78.96

+4,2 5179.90+3,5 52

2 53

W

Re

Os

Ir

Pt

Au

Hg

lanthanides`T]e
tungstenjK~rheniumN]}K~
osmium

J \K~iridium#0
platinum

0
gold

3
mercury

180.9

183.8

105

186.2

106

190.2

107

192.2

108

195.1

109

197.0

110

6p

In

Sn

Sb

Te

I

Xe

]^
tin

Ib
antimonyetelluriumK'
iodine

Q_l
xenon

114.8

118.7

121.8

127.6

126.9

Rf

Db

Sg

Bh

Hs

Mt

Ds

Rg

Cn

actinides

htjK~
dubnium[zRK~
seaborgiumz K~
bohrium

mc[K~hassium|Jgk K~
meitneriuma~]`bK~
darmstadtium

gVjK~
roentgentium

Wxj[K~
copernicum

261

262

266

264

277

268

281

272

285

+3,4 59+3,4 60

+3 61

+3 62

+3,2 63+3,2 64+3 65+3,4 66

7p+3 67+3,5 84+4,2 85

131.3

86

Tl

Pb

Bi

Po

At

Rn

2
lead

q]|]
bismuth{jK~poloniumI]`bastatine

h
radon

207.2

113

Zy\K~
rutherfordium+2,4 83` K~
thallium

204.4

112

ISblJh+3 58+1,3 82

200.6

111

83.80
1 54

J\K~
indium

81

+2,1

Ta

104

5p

39.95
1 36

P K~
gallium

112.4+3,1 80``tantalum57

lanthanides+7,4,6 76

Hf

89 103‡ 6d+6,4 75

msjK~
hafnium

178.5

+2

+5 74

`lJh

137.3

+1 88

+4 73

20.18
1 18

Al

The Universe started from light elements.
Hydrogen was ﬁrst produced. Star formed.
Star makes nuclear fusion, but it ends at Iron.
4d

1 10

!'
carbon69.72

Jcg K~
yttrium

2 9

B

49

+2

3 8

I}jK~
aluminum

4p

+1 48

v K~
helium

yK'
boron
+3 14

65.41

+2,4 47

He

17
VII A

4.003

31

+2

16
VI A

4 7

10.81

11
IB

15
VA

+3 6

BD;FAG']O\K~
scandium

39

+2

Rb

132.9

7

21

3d

q\K~
rubidium

87

3
III B

40.08
+1 38

14
IV A

13

+2

O K~
potassium

6s

13
III A

24.31
+1 20

85.47

6

>H?'

C

@

Mg

55

)BEBC

+2|Tk[K~
magnesium

39.10

5s



<

2p

Na

37

5

@

ig K~
sodium22.99

4

4copper

63.55

9.012
+1 12

19

' ,:' *,: '++2 90'bK~
lithium11

Cu750'

1.008

2+2,1  -@=GJNB

:

'+

2
II A

'
hydrogen

3

 29

"

209.0

114

209

115

116

210

117

222

118

Uut

Fl

Uup

Lv

Uus

Uuo

ununtriumsqK~
flerovium

ununpentiumn K~
livermorium

ununseptium

ununoctium

284

289

288

292

293

294

+3 68

+3 69

+3,2 70+3,2 71750'
90'

+3

La

Ce

Pr

Nd

Pm

Sm

Eu

Gd

Tb

Dy

Ho

Er

Tm

Yb

Lu

`
lanthanum_ K~
ceriumu_N\~
praseodymiumkN\~
neodymiumubK~
promethium

Y| K~
samarium

KrK~
europium

Ph jK~
gadoliniumeqK~
terbium\]u[K~
dysprosiumy}K~holmiumMqK~
erbiumd K~thulium

JceqK~ytterbiumebK~
lutetium

140.9

144.2

145

150.4

152.0

157.3

158.9

162.5

164.9

168.9

173.0

175.0

Why the periodic table has elements heavier than Fe?

(rare earth metals)

138.9

89

actinides

Kawaguchi-Shibata-Tanaka, ApJ 865 (2018) L21★light curves by numerical simulation (lines) andobservations (dots) ﬁt well.

‡ 5f

140.1

+3 90

+4 91

+5,4 92+6,3,4,5 93+5,3,4,6 94+4,3,5,6 95+3,4,5,6 96+3 97+3,4 98

Ac

Th

Pa

U

Np

Pu

Am

Cm

Bk

ISbjK~
actiniumg K~
thoriumugISbjK~
protactiniumK
uranium

kudjK~
neptuniumugjK~
plutoniumI [K~
americiumQ K~
curiumnS K~
berkelium

227

232.0

231.0

238.0

237

239

243

247

247

+3 99

Cf

167.3

+3 100Es

O yjK~ IJ]`JjK~
californium
einsteinium

251

252

+3 101+3,2 102+2,3 103

+3

Fm

Md

No

Lr

sL}K~
fermiumfqK~
mendeleviumlw K~
nobelium[K~
lawrencium

257

258

259

262

by Supernovae！
by NSNS mergers！

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

22

２. LV & LVK Observational Results

GW170817 constraints to EOS
LIGO/Virgo, PRL 119 (2017) 161101

Tidal deformability Λ, quadrupole moment Qij. tidal ﬁeld Eij

Initial result preferred soft EOS, but now changed
LIGO/Virgo, PRL 121 (2018) 161101

Capono+, Nat. Astro. 4 (2020) 625 (arXiv: 1908.10352)

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

23

O1 (2015/9/12 - 2016/1/19)

3 BHBH

GW150914: the first ever detection of gravitational waves from the merger of two black holes more than a billion light years away

https://media.ligo.northwestern.edu/gallery/mass-plot

O2 (2016/11/30 - 2017/8/25)

After O2：GWTC1 (2018/12/3 released)

10 BHBH
1 NSNS• GW170814: the first GW signal measured by the three-detector network, also from a binary black hole (BBH) merger;• GW170817: the first GW signal measured from a binary neutron star (BNS) merger — and also the first event observed in light,
by dozens of telescopes across the entire electromagnetic spectrum.

https://media.ligo.northwestern.edu/gallery/mass-plot

O3a (2019/4/1 - 2019/9/30)

After O3a：GWTC2 (2020/10/28 released)

46 BHBH
2 NSNS
2 BH+?

•
•
•
•
•
•
•
•

GW190412: the first BBH with definitively asymmetric component masses, which also shows evidence for higher harmonics
GW190425: the second gravitational-wave event consistent with a BNS, following GW170817
GW190426_152155: a low-mass event consistent with either an NSBH or BBH
GW190514_065416: a BBH with the smallest effective aligned spin of all O3a events
GW190517_055101: a BBH with the largest effective aligned spin of all O3a events
GW190521: a BBH with total mass over 150 times the mass of the Sun
GW190814: a highly asymmetric system of ambiguous nature, corresponding to the merger of a 23 solar mass black hole with a 2.6 solar masscompact object, making the latter either the lightest black hole or heaviest neutron star observed in a compact binary
GW190924_021846: likely the lowest-mass BBH, with both black holes exceeding 3 solar masses

２. LV & LVK Observational Results

GWTC-2
Gravitational Wave Transient Catalog 2
arXiv:2010.14527

39 events in O3a36BHBH, 1 NSNS, 2 BH+unknown
GWyymmdd̲hhmmss for new events
False-Alarm Rate < 2/1yr• GW190412: the first BBH with definitively asymmetric component masses, which also
•
•
•
•
•
•

•

shows evidence for higher harmonics
GW190425: the second gravitational-wave event consistent with a BNS, following
GW170817
GW190426_152155: a low-mass event consistent with either an NSBH or BBH
GW190514_065416: a BBH with the smallest effective aligned spin of all O3a events
GW190517_055101: a BBH with the largest effective aligned spin of all O3a events
GW190521: a BBH with total mass over 150 times the mass of the Sun
GW190814: a highly asymmetric system of ambiguous nature, corresponding to themerger of a 23 solar mass black hole with a 2.6 solar mass compact object, making
the latter either the lightest black hole or heaviest neutron star observed in a compact
binaryGW190924_021846: likely the lowest-mass BBH, with both black holes exceeding 3
solar masses

arXiv:2010.14529
arXiv:2010.14533

Test of GR
Population properties27

２. LV & LVK Observational Results

LIGO/Virgofrom GWTC-2, we knew …

arXiv:2010.14533★ minimum mass of BH 6 Msun or 2.6 Msun
GW190814（23 Msun + 2.6 Msun）BHBH or BHNS
★ maximum mass of BH 150 Msun
GW190521（85 Msun + 66 Msun）

2.6 Msun object is a BH or NS？

★ Large mass ratio of BBH
GW190412（30 Msun + 8.3 Msun）&

GW190814★ Non-zero Eﬀective Spin Binaries
Evidence of dynamical formation of binary?

★ BH mass distribution
power law with 2.00 ~ 2.73
★ Event Rates of Binaries＋Normal Dist. with a peak at 40 Msun
Origin of a peak?

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

28

２. LV & LVK Observational Results

GW190521

LIGO/Virgo

Discovery of IMBH（１）

PRL 125 (2020) 101102

Mass

85 +21-14 Msun + 66 +17-18 Msun -> 142 +28-16 Msun

Distance

5.3 +2.4-2.6 Gpc, z= 0.82 +0.28-0.34

100
Stellar-mass BH

105

Intermediate-massBH

Msun
Super-massive BH

Existence of BH over 100 Msun！

No formation scenario for BH over
65 Msun in the standard model.

M87 by EHT
mass

6.5 109Msun

distance
55 Mly16.9 Mpc
PRL 125 (2020) 101102

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

29

２. LV & LVK Observational Results

LIGO/Virgo

GW190521

Discovery of IMBH（2）Mass

PRL 125 (2020) 101102

85 +21-14 Msun + 66 +17-18 Msun -> 142 +28-16 Msun

Distance 5.3 +2.4-2.6 Gpc, z= 0.82 +0.28-0.34

100
Stellar-mass BH

105

Intermediate-massBH

Msun
Super-massive BH

Existence of BH over 100 Msun！

No formation scenario for BH over
65 Msun in the standard model.

M87 by EHT
mass

Second generation of mergers

6.5 109Msun

distance
55 Mly16.9 Mpc

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

30

２. LV Observational ResultsO3a (2019/4/1 - 2019/9/30)

GWTC2(PRX 11, 021053 (2021) )Existence of IMBH over 150 Msun！

A peak at 40 Msun in BH mass distribution？

Compact objects
in 2‒5 Msun mass gap ?

BH＋NSLess BNS than expected？

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

31

２. LV Observational ResultsO3a (2019/4/1 - 2019/9/30)

GWTC2(PRX 11, 021053 (2021) )Existence of IMBH over 150 Msun！

A peak at 40 Msun in BH mass distribution？
Origin of BH？

Compact objects
in 2‒5 Msun mass gap ?

Origin of BBH？

BH＋NS
Less BNS than expected？

Max Mass of NS?

Origin of BNS?

EOS of NS?

Hyper-massive NS ? Ultra-light BH? Exotic Object?
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

32

２. LV & LVK Observational Results

LIGO/Virgo

GWTC-2: Test of General Relativity by LIGO-Virgo

PRD 103 (2021) 122002
arXiv:2010.14529

1. Residuals test
2. Inspiral‒merger‒ringdown consistency test
3. Hierarchical analysis
4. Parametrized test
5. Spin-induced quadrupole moment
6. Ringdown
7. Echoes
8. Dispersion

Subtract the best ﬁt template for the event from the strain data andcompute the 90% upper limit on residual SNR.

9. Polarizations
Check whether the residual SNR is consistent with SNR from noise:measure SNR from noise-only times around the event times,
yielding a p-value
All p-values consistent with residual SNR produced by noise

No statistically signiﬁcant deviations from GR
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

33

２. LV & LVK Observational Results

LIGO/Virgo

GWTC-2: Test of General Relativity by LIGO-Virgo

PRD 103 (2021) 122002
arXiv:2010.14529

1. Residuals test
2. Inspiral‒merger‒ringdown consistency test
3. Hierarchical analysis
4. Parametrized test
5. Spin-induced quadrupole moment
6. Ringdown

Waveform models
IMRPhenom - phenomenological PN-based models, calibrated to NR

7. Echoes

SEOB - aligned-spin eﬀective-one-body models, calibrated to NR

8. Dispersion(note: only includes quadrupole)

9. Polarizations

GW190814◀ IMRPhenom waveform test
mostly consistent, but …

GW170823
GW190408 181802

GW170823
GW190408 181802
GW190814◀ 39.5M+29.5M, SNR@ inspiral < 8◀ 24.5M+18.3M, with multimodal posterior◀ 23M+2.6M, large mass ratio everNo statistically signiﬁcant deviations from GR
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

34

２. LV & LVK Observational Results

LIGO/Virgo

GWTC-2: Test of General Relativity by LIGO-Virgo

PRD 103 (2021) 122002
arXiv:2010.14529

1. Residuals test
2. IMR consistency test
3. Hierarchical analysis
4. Parametrized test
5. Spin-induced quadrupole moment
6. Ringdown
7. Echoes
8. Dispersion
9. Polarizations

No statistically signiﬁcant deviations from GR
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

35

２. LV & LVK Observational Results

LIGO/Virgo

GWTC-2: Test of General Relativity by LIGO-Virgo

PRD 103 (2021) 122002
arXiv:2010.14529

1. Residuals test
2. IMR consistency test
3. Hierarchical analysis
4. Parametrized test
5. Spin-induced quadrupole moment
6. Ringdown
7. Echoes
8. Dispersion
9. Polarizations

No signiﬁcant evidence for higher-mode in ringdown part

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

36

２. LV & LVK Observational Results

LIGO/Virgo

No Mountains in 5 milli-sec pulsars

ApJL 902 (2020) L21( arXiv:2007.14251 )O1+O2+O3a data，GW search from 5 pulsars
PSR J0437-4715

がか座

PSR J0711-6830

510光年

5.75 ms 最も精度よく位置が判明している天体

3400光年

5.5 ms22.7 ms NS+NS, ダブル・パルサーのA，8500万年後に合体

PSR J0737-3039A

とも座

1600光年PSR J0534+2200

Crab pulsar (かに星雲)

6300光年PSR J0835-4510

Vela pulsar (ほ座)800光年

33 ms NS，SN1054
89.3 ms NS，３番目に明るい天体

重力波未検出no detectionof GW
If we model NS with a mountain on eq. plane, peak < 10-8.
GW from J0711-6830 is less than spin-down ratio.
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

37

２. LV & LVK Observational Results

LIGO/Virgo

No Lensed GWs in O3a

Freq-dep. beating pattern

Ranking

Similar pairs in M, χ( arXiv:2105.06384 )Detections of lensed events will improvecompact objects merger rate
Consistency

no detection of lensed signature
No magniﬁcation, multiple-image, nor microlensing signatures
on O3a data

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

38

２. LV & LVK Observational Results

LIGO/Virgo/KAGRA

Discovery of NS-BH binaries

ApJL (2021)( arXiv:2106.xxxxx )Detections of lensed events will improvecompact objects merger rate

https://www.ligo.org/science/outreach.php
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

39

Gravitational Wave Physics & Astronomy, Status of KAGRA
Contents
1. Gravitational Wave Overview
2. LIGO-Virgo-KAGRA Observational Results
3. The KAGRA interferometer
4. Outlook of GW Astronomy(c) KAGRA Collaboration / Rey.Hori

Hisaaki Shinkai (Osaka Inst. Tech.)
真貝寿明（大阪工業大学）
KAGRA Scientiﬁc Congress, board chair
Nature Astronomy 3, 35 (2019)https://www.nature.com/articles/s41550-018-0658-y

on behalf of KAGRA collaboration

Cosmology from Home 2021 July

Status of KAGRA

KAGRA (Kamioka Gravitational-Wave Observatory)
1000m under thesummit of the Mt.

Mozumicontrol office.
(15 min)Toyama City
(60 min)

358m above thesea level.

http://gwcenter.icrr.u-tokyo.ac.jp/en/（大型低温重力波望遠鏡）
former name LCGT = large cryogenic gravitational telescope
named by public naming contest, 神楽（かぐら）dance music in front of Gods
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

41

Status of KAGRA

KAGRA (Kamioka Gravitational-Wave Observatory)
TAMA 300 m (NAOJ, Tokyo area, 2008)

CLIO 20 m (Kamioka, 2010)https://doi.org/10.1093/ptep/ptaa125

arXiv: 2005.05574

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

42

Status of KAGRA

Brief History of KAGRA
today

calendar
year

2010

2011

2012

2013

2014

2015

Project
Start
Tunnel Excavation

2016

2017

2018

2019

2020

2021

adv vibration isolation, optics, cryo.…

installation

operationiKAGRA = initial KAGRAbKAGRA = baseline KAGRA
iKAGRA[arXiv:1712.00148]

bKAGRAphase-1

bKAGRAphase-2

O3[arXiv:1901.03569]

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

43

Status of KAGRA

Basic Idea of the Interferometer
Longer arm-length makes better sensitivity“Michelson” interferometerL
Laser Source

Beam Splitter

L

MirrorSensitivity (Lower the better)

MirrorPhoton Detector
Frequency

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

44

Status of KAGRA

Basic Idea of the Interferometer“Michelson” interferometer

Longer arm-length makes better sensitivity

Longer arm-length makes better sensitivity
Laser Source

Sensitivity (Lower the better)

Best sensitivity for 100 Hz is L= 750 km

Photon Detector
Frequency

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

45

Status of KAGRA

Basic Idea of the Interferometer
Longer arm-length makes better sensitivity
Best sensitivity for 100 Hz is L= 750 km

end mirror

input mirrors
Laser Sourceend mirror

Sensitivity (Lower the better)“Fabry-Pérot Michelson” interferometer

Not so good for high freq.
due to GW cancellation.

Photon Detector
Frequency

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

46

Status of KAGRA

Basic Idea of the Interferometer
Longer arm-length makes better sensitivity“Fabry-Pérot Michelson” interferometer

resonanceend mirror

input mirrors

end mirror

Laser Source

resonance

Photon Detector

Finesse F ~ 1000
(effective reflections F/π)

Sensitivity (Lower the better)

Best sensitivity for 100 Hz is L= 750 km

Not so good for high freq.
due to GW cancellation.
High finesse introduces
optical losses at mirrors

Frequency

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

47

Status of KAGRA

Basic Idea of the Interferometer

Laser Source

resonance
Power-Recycling
mirrorPhotonget more effective
laserDetector
power(TAMA300, initial LIGO, Virgo)

Sensitivity (Lower the better)“Power-Recycled” Fabry-Pérot Michelson interferometer

Reduce shot-noiseof laser

Frequency

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

48

Status of KAGRA

Basic Idea of the Interferometer“Signal-Recycled” Fabry-Pérot Michelson interferometer

resonance

Signal-Recycling
mirrorgetmore Detector
effective GW signals
Photonget more effective GW signals
resonance (N+1/2) wavelength between SR & IM

Sensitivity (Lower the better)

Laser Source(GEO600)

get more finesse
with SR mirror

Frequency

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

49

Status of KAGRA

Basic Idea of the Interferometer

input mirrors
Laser Source

Power-Recycling
mirrorSignal-Recycling
mirrorgetPhoton
more effective
Detector GW signals
resonance (N+1/2) wavelength between SR & IM

Sensitivity (Lower the better)“Dual-Recycled” Michelson interferometer

get more finesse
with SR mirror

Frequency

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

50

Status of KAGRA

Basic Idea of the Interferometer

Laser Source

Signal-Extraction
mirrorgetPhoton
more effective
DetectorGW signals
resonance N wavelength(KAGRA, Advanced LIGO, Advanced Virgo)

Sensitivity (Lower the better)“Resonant Side-band Extraction” interferometer

keep at relative low finesse
with SE mirror

Frequency

for optical losses
for GW cancellation

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

51

Status of KAGRA

Basic Idea of the Interferometer

400mW Nd:YAG laser
amplified to 40W
finesse 540
Laser Sourcefinesse 800-1530

Photon Detector(KAGRA, Advanced LIGO, Advanced Virgo)

Sensitivity (Lower the better)“Resonant Side-band Extraction” interferometermore laser power

Frequency

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

52

Status of KAGRA

Basic Idea of the Interferometer“Resonant Side-band Extraction” interferometer

400mW Nd:YAG laser
amplified to 40W
finesse 540
Laser Sourcefinesse 800-1530

Photon Detector

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

53

Status of KAGRA

Basic Idea of Suspension System
x0<latexit sha1_base64="0q2r0nZH242eTp0Bf9v9gSkCLf4=">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</latexit>`x<latexit sha1_base64="sn15ZQE08dd7qSQV4xcUZ3Fc5es=">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</latexit>

Relative Movement<latexit sha1_base64="j4L7qP1Ylz8giwBeM5fCMDQzNsA=">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</latexit>

f-2

Frequency [Hz]Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

54

Status of KAGRA

Relative Movement

Basic Idea of Suspension System

f-2
f-4

Frequency [Hz]Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

55

Status of KAGRA

Relative Movement

Basic Idea of Suspension System

f-2
f-4
f-6

Frequency [Hz]Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

56

Status of KAGRA

Relative Movement

Basic Idea of Suspension System

Frequency [Hz]Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

57

Status of KAGRA

Basic Idea of Suspension System
Type-AbKAGRA configuration

BRT- Cryogenic test masses- 3 km arm cavities- RSE with power recycling

ETM

Type-A system

Y-arm- Cryogenic test mass
Sapphire, 23kg, 20K- Tall seismic isolator
IP + GASF + Payload
ITM

MC

PRM

PR3 PR2

Type-C system- Mode cleaner
Silica, 0.5kg, 290K
- Stack + Payload

BS

BRT

IO

ITM

Test mass and Core optics (BS, FM,..)
Silica, 10kg, 290K
- Seismic isolator
Table + GASF + Type-B Payload-

ETM

Type-B system
SRM

Type-Bp payload

X-arm

OMMT
OMC

- Core optics (BS, SRM,…)
Silica, 10kg, 290K
- IP + GASF + Payload- Stack for aux. optics

as the conﬁguration of April 2020 (O3GK)
Class. Quantum Grav. 36 (2019) 165008

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

58

Status of KAGRA

Cryogenic System<latexit sha1_base64="QLLJPypWxpFYAZ8BuEgH0hqQLN8=">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</latexit>

Thermal Noise /

s

4kB T
m!02 !Q

low temperaturelarge mass

sapphire mirror
22.8 kgdiameter 22cm
thickness 15cm

20 K
in 4 weeks
Class. Quantum Grav. 36 (2019) 165008
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

59

Status of KAGRA

KAGRA (Kamioka Gravitational-Wave Observatory)
2018年8月

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

60

Status of KAGRA

KAGRA (Kamioka Gravitational-Wave Observatory)

90cm snow in one night, Dec 17 2020
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

61

Status of KAGRA

Joint Research MoA signed LIGO-Virgo-KAGRA＊ 1 Mpc (BNS) is required to join the observation.

Aug 24, 2019

Dec 19, 2019

October 4, 2019 @ Ceremony of MoA signing

March 26, 2020

main part (10 pages)
Concept, Deﬁnitions,Purposes

Appendix A (17 pages)
Organizations, Procedures

Letter of Intent (3 pages)
KAGRAʼs Join to O3＊ Finally, over 1 Mpc in the end of March 26, 2020.

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

62

Status of KAGRA

O3b,

O3GK,

and after that2019 | 2020
12

1

2

3

4

5

6

7

8

9

O3b (planned)
O3b (LV)
GEO600 Astrowatch ~ 1.2 Mpc
Feb25-Mar10

Dec 17-25

KAGRA

ER

Obs.

Apr 7-21

Obs.
O3GK

* O3GK observation paper plan

1,000
970

March 29, 2020

(LVK paper)

883

655
600

594

500

COVID-19 infected # in Japan / day

500
442
382

278

250

165

pr
.7
A

9
ar
.2

5
M

ar
.2

8
M

ar
.1
M

ar
.9
M

ar
.5
M

ar
.3
M

20
Fe
b.

14
Fe
b.

11
Fe
b.

5

66

Fe
b.

ec
.
D

ec
.

6

0

40

11

10

D

Sensitivity Record in kpc

750

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

63

Status of KAGRAO3GK (April 7-21, 2020)
Oﬃcial start and end time
Start :April 7 8:00 2020 UTC, GPS Time : 1270281618
End : April 21 0:00 2020 UTC, GPS Time 1271462418
KAGRA Duty Cycle : Locked 69%, Observing 58%
Longest lock 8h05m
bad weather
ocean tide

Sensitivity : 500-700 kpc

GRB200415A

Takahiro Yamamoto, JGW-P2011980

GRB200415A

6.4 days

NGC 235 (Sculptor galaxy)

7.3 days

3.5 Mpc, one of the brightest galaxies
https://gcn.gsfc.nasa.gov/fermi̲grbs.html

Jim Lough, LIGO-G2001554

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

64

Status of KAGRA

Overview of KAGRA: reviews in PTEP 2020-2021
published PTEP 2020
KAGRA history
https://doi.org/10.1093/ptep/ptaa125

arXiv: 2005.05574

published PTEP 2020
KAGRA Science
https://doi.org/10.1093/ptep/ptaa120

published PTEP 2021
KAGRA Calibration, Detector characerization,
physical environment monitors
https://doi.org/10.1093/ptep/ptab018

arXiv: 2008.02921

arXiv: 2009.09305

in preparation* Overview of KAGRA : Noise Budget* Overview of KAGRA : Data transfer and management* Overview of KAGRA : Data analysis methods

https://iopscience.iop.org/article/10.1088/1361-6382/abd922
Class. Quant. Grav. 38 (2020) 065011

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

65

Status of KAGRA

KAGRA collaboration
114 groups, 14 countries/regions
460+ active members
Default-author list 2019+2020
has 200 names.

Organize International Workshop
KIW8 July 7-9 2021 @ Daejeon, Korea
200+ participants
KIW9 May 2022 @ Beijing China

http://gwwiki.icrr.u-tokyo.ac.jp/JGWwiki/KAGRA
Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

66

Status of KAGRA

Toward O4
2015* Target Sensitivity 25 - 130 Mpc* Recent estimate: less than 25 Mpc
due to heat absorption of sapphire mirrors
by reducing laser noise, low-f noise,

LIGO

2016

2017

2018

2019

2020

2021

2022

60-80Mpc

60-100Mpc

120-130 Mpc

160-190 Mpc

O1

O2

O3a O3bO490-120Mpc

50 MpcVirgoless than 100Kx20 sensitivity at mid-freq.
dual recycling
lock trials by the end of September 2020
suspension noise control for low freq.
one-order reduced in Julyde-frosting mirrors
de-frosting windows for oplev light

O2

KAGRA

iKAGRA

2015

2016

30
Mpc

bKAGRAphase1
2017

2018

O4

O3a O3b1Mpc

25-70Mpc

bKAGRAphase2

O3

O4

2019

2020

2021

2022

commissioning
Summer 2022
O4 starts
today

Summer 2021

repair & installation

Cryo-Payload repairing

DGS/AEL upgrade (DGS/AEL)ETMY tower repairing

Stray light around IOO (AOS)

install laser beam baﬄes

Suspension frame modiﬁcation (AOS, VIS)

Cryocoolers replacement (CRY)

Temperature monitors (VIS)

Intensity noise reduction system (IOO)

and more

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

67

Gravitational Wave Physics & Astronomy : Outlook (1)Last 5 years★ The ﬁrst detection of GW was 5 years ago. Since then we detected over 50 events.
Most of them are binary BHs, and 2 binary NSs, and two unknown ones.
Recent GW studies cover the constraints to the lensed events, stochastic backgrounds, spinning NSs,
and also to cosmic stringʼs model, dark matter candidates.

https://antimatterwebcomics.com/comic/physics-nobel-prize-2017/https://antimatterwebcomics.com/comic/gw170817/

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

68

Gravitational Wave Physics & Astronomy : Outlook (2)Next 5 years★ A+, AdV+, and KAGRA projects involve signiﬁcant upgrades in O5. The sensitivity of LIGO-Virgo-KAGRA
network should improve 2-3 times over O3; one binary merger per day.
★ Alert system will also be improved.
In O3, the alerts were made within minutes of data acquisition for compact binary mergers.
Improved alerts for BNS will be seconds to minutes before its merger.
O1
80
Mpc

LIGO

O3

O2
100
Mpc

O5

110-130
Mpc

160-190
Mpc

Target
330 Mpc

50
Mpc

90-120Mpc

150-260
Mpc

25-130
Mpc

130+
Mpc

30
Mpc

Virgo

O4

1
Mpc

KAGRA

Target
330 Mpc

LIGO-India
2015

2016

2017

2018

2019

2020

2021 2022

2023

2024

2025

2026

LIGO-G2002127-v4

R Magee et al 2021 ApJL 910 L21 [arXiv:2102.04555]

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

69

Gravitational Wave Physics & Astronomy : Outlook (3)Next 10 years★ The 3rd generation GW detectors, Cosmic Explorer (US) and
Einstein Telescope (Europe), will observe the entire Universe.

Cosmic Explorer

Einstein Telescope

40km L-shape

10km Triangle

EM counterparts(certain)

1

Evan Hall, MIT★ Space mission, LISA and with other proposed missions
projects (DECIGO, BBO, ALIA, TianQin, …) will
explore new GW phenomena in low frequency.

NS+NS

BH+BH

1.4+1.4M

30+30M

Hisaaki Shinkai (Osaka Institute of Technology) “GW physics, Status of KAGRA” Cosmology From Home 2021

70