LIGO-Virgo-KAGRA network for hunting gravitational waves
Underground and Cryogenic interferometric 3 km gravitational-wave detector at Kamioka, Japan

Contents
1. Gravitational Wave Overview
2. LIGO-Virgo-KAGRA Observational Results (GWTC-3)
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）

http://www.oit.ac.jp/is/shinkai/
JGW-G2113518

JGRG30 online

December 8, 2021

LIGO-Virgo-KAGRA network for hunting gravitational waves

Contents
1. Gravitational Wave Overview
2. LIGO-Virgo-KAGRA Observational Results (GWTC-3)
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）

JGRG30 online

December 8, 2021

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) JGRG30 (online) December 8, 2021

3

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

typical amplitude 10-22

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

GW151226<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
cosmological parameters

0

時間

5

究極理論の構築
uniﬁedtheorystandard way is to use matched ﬁltering techniquenecessary for GW templates in handHisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

5

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) JGRG30 (online) December 8, 2021

6

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) JGRG30 (online) December 8, 2021

7

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
more man power

LIGO-Livingstone

Virgo

Virgo

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

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GW International Network

KAGRA joined international network October 2019.

1330 members

465 members

460 members

860 authors

360 authors

200 authors

101 groups

96 groups

114 groups

20 countries

8 countries

14 regions
KSC board chair

LSC spokesperson
Patrick Brady

2021
Aug.

Virgo spokesperson
Giovanni Losurdo
HS
Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

Junʼichi Yokoyama
9Gravitational Wave Projects

Sensitivity Curve

Binary NS range
taget sensitivity
designed sensitivity
155 Mpc

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) JGRG30 (online) December 8, 2021

10

Gravitational Wave Projects

Sensitivity Curve

Sensitivity History

Binary NS range
taget sensitivity
designed sensitivity
155 Mpc

LVK collaboration, Living Rev Relativ (2020) 23:3
https://link.springer.com/article/10.1007/s41114-020-00026-9[1304.0670ver2020Jan]

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

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LIGO-Virgo-KAGRA network for hunting gravitational waves
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/

JGRG30 online

December 8, 2021

Gravitational Wave Projects

Observation Period⭐GW150914

2015

2016

Sep12

LIGO

⭐GW170817

Jan19

O1
60-80 Mpc

2017
Nov30

⭐GW190521 ⭐GW200115

2018

Aug25

Apr1̶Sep 30

O2

O3a

60-100 Mpc

2020

Apr1̶Sep 30

O2

O3a

30 Mpc2021

Nov1̶ Mar27

O3b

COVID-19 terminated O3b

120 - 130 Mpc

Aug 1-25

Virgo

2019

Nov1̶ Mar27

O3b

50 MpcApr7-21KAGRA

LVK analysis papers started
from O3b scientiﬁc results.

joined Oct 2019
1 Mpc

➡ 3BHBH➡ +4BHBH➡ +1NSNSGWTC-1
2018/12/3➡ 50 events in total

GWTC-2
2020/10/28➡ 11 events in total

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

➡ 55 total

GWTC-2.1➡ 90 total
2021/8/2
GWTC-32021/11/5
13

Gravitational Wave Projects

Observation Period
2015

2016

Sep12

LIGO

Jan19

2017
Nov30

O1

Aug25

O2

60-80 Mpc

Aug 1-25

O2
30 MpcPublic Alert started from O3a

2019
Apr1̶Sep 30

2020

O3b

COVID-19 terminated O3b

120 - 130 Mpc
Apr1̶Sep 30

Nov1̶ Mar27

O3a

O3b

50 MpcApr7-21https://gracedb.ligo.org

2021

Nov1̶ Mar27

O3a60-100 Mpc

Virgo

2018

KAGRA

LVK analysis papers started
from O3b scientiﬁc results.

joined Oct 2019
1 Mpc

➡ 50 events in total

GWTC-2
2020/10/28
https://monitor.ligo.org/gwstatus

https://www.gw-openscience.org

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

➡ 55 total

GWTC-2.1➡ 90 total
2021/8/2
GWTC-32021/11/5
14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

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

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GW transient catalog

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

GWTC1 (2018/12/3 released)

After O2：

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

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

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GW transient catalog

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

GWTC2 (2020/10/28 released)

After O3a：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
Hisaakilikely
Shinkai(OsakaBBH,
Institute
Technology)(online) December 8, 2021
GW190924_021846:
the lowest-masswith both ofblackholes exceeding 3JGRG30
solar masses

17

GW transient catalog

O3b (2019/11/1 - 2020/3/27)

GWTC-3 (2021/11/7 released)

After O3b：

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

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

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GW transient catalog

O3b (2020/11/1 - 2021/3/27)

GWTC-3 (2021/11/7 released)

After O3b：

BHs
unknowns(2.5-5M)
NSs

O1

O2

O3a

O3b

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

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

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# of Detections

Event Rate is consistent with O3a/O3b

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

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Itʼs hard to publish a review of GW Astronomy"Rika Nenpyo 2022" (Annual Scientific Databook, Ed. by NAOJ, Maruzen Publishing Co.) newly includes data pagesof gravitational waves, prepared by Takahiro Tanaka and HS.
The deadline of the draft was July this year, so the contents are of GWTC2.
ॏྗ೾ॏྗ೾ͷੜ੒‫ߏػ‬ɹҰൠ૬ରੑཧ࿦ʹΑΕ͹ɼେ࣭ྔͰίϯύΫτͳఱମ͕Ճ଎౓ӡಈ
͢Δ͜ͱʹΑΓɼॏྗ೾͕ൃੜ͢Δɽॏྗ೾‫ͯ͠ͱݯ‬͸࿈੕ͷ߹ମ΍௒৽੕രൃɼඇ‫ٿ‬ରশͳ੕ͷߴ଎ճస΍ɼӉ஦ॳ‫ݯىʹظ‬Λ΋ͭॏྗ೾͕Ӊ஦ۭؒΛ఻೻͍ͯ͠Δͱߟ͑ΒΕΔɽ
͜ΕΒͷ͏ͪɼσʔλͱͷ૬ؔղੳΛՄೳʹ͢Δ೾‫ܗ‬༧ଌ͕Ͱ͖Δͷ͸ɼ࿈੕߹ମ͔Βͷॏྗ೾Ͱ͋Δɽे෼ʹ߹ମલ͸χϡʔτϯྗֶʹ૬ର࿦ิਖ਼ΛՃ͑ͨϙετɾχϡʔτϯల։ʹΑΓɼ߹ମલ‫ޙ‬͸਺஋γϛϡϨʔγϣϯʹΑΓɼ߹ମ‫ޙ‬ϒϥοΫϗʔϧ͕ੜ͡Δ৔߹ʹ͸ϒϥοΫϗʔϧۭ࣌ͷઁಈʹΑͬͯ΋೾‫ܗ‬Ϟσϧ͕ಘΒΕΔɻ͜ΕΒͷϞσϧͱॏྗ೾‫ׯ‬ব‫Ͱܭ‬ಘΒΕΔ৴߸ͷ૬ؔΛͱΔ͜ͱͰɼ࿈੕ϒϥοΫϗʔϧʢҎԼ BBHʣ΍࿈੕தੑࢠ੕ (BNS)ɼ͓Αͼதੑࢠ੕ɾϒϥοΫϗʔϧ࿈੕ (NSBH) ͷ߹ମ‫ݱ‬৅ʹΑΔॏྗ೾ͷ‫ݕ‬ग़ɺ͓Αͼɺύϥϝʔλਪఆ͕ 2015 ೥ҎདྷՄೳʹͳͬͨɽॏྗ೾ͷ‫؍‬ଌɹ͜Ε·ͰʹɼถԤͷϨʔβʔ‫ׯ‬ব‫ ܭ‬LIGO, Virgo ʹΑͬͯɼO3a ͱ‫ݺ‬͹ΕΔ‫؍‬ଌ‫ؒظ‬ऴྃ·ͰʹɼBBH ʹΑΔॏྗ೾͕ 46 ྫɼBNS ʹΑΔॏྗ೾͕ 2 ྫใࠂ͞Ε
͍ͯΔɽ೔ຊͷ KAGRAʢ͔͙Βʣ΋ O3b ‫؍‬ଌ‫ؒظ‬ͷ࠷‫ڞʹޙ‬ಉ‫؍‬ଌʹೖͬͨɽO3b ‫ظ‬ͷॏྗ೾Πϕϯτ͸ 2021 ೥ 7 ݄࣌఺ͰະൃදͰ͋Δɽ‫ࡏݱ‬ɼ֤‫ׯ‬ব‫ܭ‬͸࣍ͷ‫؍‬ଌ‫ ؒظ‬O4
ʢ2022 ೥Ն͔Β 1 ೥ؒͷ༧ఆʣʹ޲͚ͯ‫؍‬ଌ‫౓ײ‬Λ্͛ΔͨΊɼ‫ׯ‬ব‫ܭ‬ͷվྑதͰ͋Δɽॏྗ೾Πϕϯτ͸ɼ‫؍‬ଌ͞Εͨ೥݄೔Λ༻͍ͯɼGW150914 ͷ‫໊໋͞Ͱܗ‬ΕΔɽO3a ‫ظ‬ΑΓɼ࣌෼ඵΛՃ໊͑ͨশ͕ਖ਼ࣜͱͳͬͨɽॏྗ೾Πϕϯτ͸଎ใମ੍͕औΒΕɼଟ೾௕ి࣓೾௥‫؍‬ଌ͕Մೳʹͳ͍ͬͯΔ͕ɼ͜Ε·Ͱʹ೾‫͕ݯ‬ಛఆ͞Εͨͷ͸ GW170817 ͷΈͰ͋Δɽද 1: ॏྗ೾Ϩʔβʔ‫ׯ‬ব‫ܭ‬ͷҐஔͱ࿹ͷ޲͖ʢྫ͑͹ N 36◦ W ͸ɼ๺͔Β੢ํʹ 36◦ ͷ޲͖Λࢦ͢ɽʣ‫ׯ‬ব‫ܭ‬࿹௕ (km)LIGO Hanford
LIGO Livingston
Virgo
KAGRA

ถࠃ
ถࠃ
Ԥभ
೔ຊ

4
4
3
3

Ң౓

‫౓ܦ‬

X-࿹

Y-࿹

46◦ 27" 19"" N
30 33 46 N
43 37 53 N
36 24 36 N

119◦ 24" 28"" W
90 46 27 W
10 30 16 E
137 18 36 E

N 36◦ W
N 18◦ S
N 19◦ EE 28.3◦ N

W 36◦ S
S 18◦ EW 19◦ N
N 28.3◦ W

ද 2: ա‫ڈ‬ͷ‫؍‬ଌ‫ؒظ‬‫؍‬ଌ‫ظ‬Advanced LIGO

O1
O2
O3a
O3b
O3GK

೥ ݄ ೔
೥ ݄ ೔
2015 9 12 –2016 1 19
2016 11 30 –2017 8 25
2019 4 1 –2019 9 30
2019 11 1 –2020 3 27–

Advanced Virgo
೥ ݄ ೔

೥ ݄ ೔
–
2017 8 1 –2017 8 25
ಉࠨ
ಉࠨ
–

KAGRA
೥ ݄ ೔

೥ ݄ ೔

–
–
–
2020 4 7 –2020 4 21‫؍‬ଌ͞ΕͨதͰಛච͢΂͖Πϕϯτɹಥൃతॏྗ೾Χλϩά 2(GWTC2) ͱͯ͠ 2020 ೥
10 ݄ʹൃද͞Εͨ΋ͷ͕ 2021 ೥ 7 ݄࣌఺Ͱ࠷৽Ͱ͋Δɽ
GW150914ɹ࠷ॳʹใࠂ͞Εͨ௚઀ॏྗ೾‫؍‬ଌΠϕϯτɽBBH ͷଘࡏΛ໌Β͔ʹ͠ɼଠཅ
࣭ྔʢM# ʣͷ 30 ഒҎ্ͷ BH ͷଘࡏΛॳΊͯ֬ೝͨ͠ɽใࠂ͞Εͨ BBH ͷΠϕϯτͷதͰ΋࠷΋γάφϧɾϊΠζൺ (SNR) ͕ߴ͍ɽGW170817ɹ࠷ॳʹใࠂ͞Εͨ BNS Πϕϯτɽ௚‫ʹޙ‬ଟ͘ͷ௥‫؍‬ଌ͕ͳ͞ΕɼϚϧνɾϝοηϯδϟʔఱจֶͷॳΊͯͷ੒ޭྫͱͳͬͨɽॏ
ྗ೾೾‫͔ܗ‬ΒಘΒΕͨதੑࢠ੕ͷঢ়ଶํఔࣜʹର͢Δ੍‫ݶ‬͸֩ີ౓ ρnuc = 2.8 × 1014 g/cm3ͷ 2 ഒͷີ౓ʹ͓͚Δѹྗͱͯ͠ (2ρnuc ) = 3.5+2.7
× 1034 dyn/cm2 (90% ৴པ۠ؒ) Ͱ͋ʵ 1.7
ΔɽΨϯϚઢͱॏྗ೾ͷ౸ண࣌ࠁͷࠩ 1.7 ඵ͔ΒಘΒΕͨॏྗ͸఻೻଎౓ͷޫ଎͔ΒͷͣΕͷׂ߹ʹର͢Δ੍‫ݶ‬͸ 1 × 10−15 ҎԼͰ͋Δɽ·ͨɼՄࢹɾ੺֎ʹ͓͚Δ௥‫؍‬ଌ͔ΒమҎ্ͷॏ‫ݩ‬ૉ߹੒ͷ‫ݟ͕੻ܗ‬ΒΕɼr-աఔ‫ݩ‬ૉ߹੒ͷॏཁͳνϟϯωϧʹͳ͍ͬͯΔ͜ͱΛ͍ࣔࠦͯ͠ΔɽGW190412ɹ໌Β͔ʹ࣭ྔൺͷҟͳΔ BBH ͔Βͷॏྗ೾Ͱɼॏྗ೾ͷߴ࣍Ϟʔυͷ‫ݕ‬ग़͕ͳ͞ΕͨɽGW190425ɹ 2 ൪໨ʹൃ‫͞ݟ‬Εͨ BNSɽGW190521 ૯࣭ྔ͕࠷େͷ BBH Ͱɼ߹ମ‫ޙ‬ͷ࣭ྔ͕ 150M" Λ௒͑Δ΋ͷͱߟ͑ΒΕΔɽ͍ΘΏΔத࣭ؒྔ
BH ͷྖҬͷީิఱମͷॳͷൃ‫ͨͬͳͱݟ‬ɽBBH ͷ߹ମͷୈ̎ੈ୅ͷ߹ମͱ΋ߟ͑ΒΕ͍ͯΔɽGW190814 ੕‫ܗ‬੒ͷγφϦΦͰ͸ෆՄೳͱ͞ΕΔ 2–5M" ͷ࣭ྔྖҬͷίϯύΫτ
ఱମ͔Βͷॏྗ೾ͱߟ͑ΒΕΔɽGW190924: ‫࠷ͰͰ·ࡏݱ‬খ࣭ྔͷ BBHɽGW200105,
GW200115: ͸͡Ί࣮ͯ֬ͳ΋ͷͱใࠂ͞Εͨ NS-BH ࿈੕‫߹ܥ‬ମɽද 3: ใࠂ͞Εͨओͳॏྗ೾ʢ2021 ೥ 7 ݄‫ࡏݱ‬ʣɽ࿈੕ͷ࣭ྔΛ M1 , M2 ͱͨ͠ͱ͖ͷɼνϟʔϓ࣭ྔ Mc = (M1 M2 )3/5 /(M1 + M2 )1/5 , ࣭ྔൺʢதԝ஋ͷൺʣM2 /M1 ɼ༗ޮεϐϯ χeff ɼ࠷ऴతʹ‫ܗ‬੒͞Εͨ BH ͷ࣭ྔ Mfinal (NS Λ‫ؚ‬Ή৔߹͸શ࣭ྔ M = M1 + M2 )ɼ
શ‫཭ڑ‬ɼ೾‫ݯ‬ಛఆਫ਼౓ʢฏํ౓ʣ(∆θ)2 ɼγάφϧɾϊΠζൺΛࣔ͢ɽ෯ͷ͋Δྔ͸ 90% ͷ৴པ۠ؒɽ(छྨ͝ͱʹ೔෇ॱɽBBH ʹ͍ͭͯ͸ɼSNR ͕ 13.1 ΑΓେ͖͍΋ͷͷΈɽ)Πϕϯτ (BBH)
GW150914
GW170608
GW170814
GW190408 181802
GW190412
GW190521
GW190521 074359
GW190630 185205
GW190728 064510
GW190814
GW190828 063405
GW190910 112807
GW190924 021846
Πϕϯτ (BNS)

GW170817
GW190425Πϕϯτ (NSBH)
GW200105 162426
GW200115 042309

Mc (M" )28.6+1.7−1.5
7.9+0.2−0.2
24.1+1.4−1.1
18.3+1.9−1.2
13.3+0.4−0.3
69.2+17.0−10.6
32.1+3.2−2.5
24.9+2.1−2.1
8.6+0.5−0.3
6.09+0.06−0.06
25.0+3.4−2.1
34.3+4.1−4.1
5.8+0.2−0.2
Mc (M" )1.186+0.001−0.0011.44+0.02−0.02
Mc (M" )3.41+0.08−0.07
2.42+0.05
−0.07

࣭ྔൺ
0.86
0.69
0.82
0.75
0.28
0.72
0.78
0.68
0.66
0.11
0.82
0.81
0.56
࣭ྔൺ

χeff
-0.01+0.12−0.13
0.03+0.19−0.07
0.07+0.12−0.12
0-.03+0.14−0.19
0.25+0.08−0.11
0.03+0.32−0.39
0.09+0.1−0.13
0.1+0.12−0.13
0.12+0.2−0.07
0+0.06−0.06
0.19+0.15−0.16
0.02+0.18−0.18
0.03+0.3
−0.09

0.87
0.70
࣭ྔൺ

0+0.02−0.01
0.06+0.11
−0.05
χeff

0.21
0.26

-0.01+0.11−0.15-0.19+0.23
−0.35

χeff

Mfinal (M" )63.1+3.4−3.0
17.8+3.4−0.7
53.2+3.2−2.4
41.1+3.9−2.8
37.3+3.9−3.8
156.3+36.8−22.4
71.0+6.5−4.4
56.4+4.4−4.6
19.6+4.7−1.3
25.6+1.1−0.9
54.9+7.2−4.3
75.8+8.5−8.6
13.3+5.2−1.0
M (M" )
શ–
3.4+0.3−0.1
M (M" )
શ
10.9+1.1−1.2
7.1+1.5−1.4‫( ཭ڑ‬Mpc)
440+150−170
320+120−110
600+150−220
1550+400−600
740+140−170
3920+2190−1950
1240+400−570
890+560−370
870+260−370
240+40−50
2130+660−930
1460+1030−580
570+220−220‫( ཭ڑ‬Mpc)

(∆θ)2
179
392
87
–
21
940
500
–
–
19
520
–
380
(∆θ)2

SNR
24.4
14.9
15.9
14.67
18.86
14.38
24.38
15.64
13.64
22.18
16.04
13.42
13.16
SNR

40+7.0−15.0
160+70−70‫( ཭ڑ‬Mpc)

39
9900
(∆θ)2

33
13.03
SNR

280+110−110
300+150
−100

7700
900

13.9
11.6

ಘΒΕͨՊֶత੒Ռɹ࿈੕‫͍ͯͭʹܥ‬͸ɼͦͷ߹ମස౓ʹ͍ͭͯɼBBH ͸ɼ23.8+14.0
−8.7
+73
3
3
/Gpc3 /yrɼBNS ͸ɼ561+834−413 /Gpc /yrɼNSBH ͸ɼ45−33 /Gpc /yr ͱ‫ੵݟ‬΋ΒΕ͍ͯΔɽ͜ͷ΄͔ɼഎ‫ܠ‬ॏྗ೾ʹରͯ͠ɼӉ஦๲ு཰ʹରͯ͠ॏྗ೾ͷΤωϧΪʔ͕‫د‬༩͢Δׂ
߹ͱͯ͠ʢฏୱͳΤωϧΪʔεϖΫτϧΛԾఆ্ͨ͠ͰʣΩGW < 6.0 × 10−8 ͷ্‫͕ݶ‬ಘΒΕ͍ͯΔɽ࿈ଓॏྗ೾ͷॏྗ೾ৼ෯ʹରͯ͠͸ɼ͓͓Αͦ 1 × 10−25 ఔ౓ʢ200 Hz ·ΘΓʣͷ্‫͕ݶ‬ಘΒΕ͍ͯΔɽ·ͨɼ‫ط‬஌ͷύϧαʔ͔Βͷ࿈ଓॏྗ೾ʹରͯ͠΋‫ݸ‬ʑʹ্‫ݶ‬͕ಘΒΕ͍ͯΔɽ
Ұൠ૬ରੑཧ࿦ͷ‫ূݕ‬΋ߦΘΕɼ਺͋Δςετ͢΂ͯͰɼҰൠ૬ରੑཧ࿦͔ΒಘΒΕΔ༧
‫؍ͱݴ‬ଌ͞Ε͍ͯΔॏྗ೾৴߸ͱͷؒʹໃ६͸ੜ͍ͯ͡ͳ͍ɽࠓ‫ޙ‬ɼൃ‫ͭʹ͢૿͕਺ݟ‬Εͯ࿈੕‫ܥ‬ͷ‫ܗ‬੒γφϦΦ͕໌Β͔ʹͳΔ͜ͱ͕‫ظ‬଴͞ΕΔɼকདྷతʹ͸ɼۜՏ‫ܗܥ‬੒γφϦΦ΍ॳ‫ظ‬Ӊ஦ͷ৘ใͳͲʹ΋ɼॏྗ೾‫؍‬ଌ͔Βଟ͘ͷ஌‫͕ݟ‬΋ͨΒ͞ΕΔͰ͋Ζ͏ɽ

1

Springer Handbook of GW Astronomy will be ready in 2022.
The deadline of the draft was May this year, so the contents are of GWTC2.

2➡ 50 events in total➡ 55 total➡ 90 total

GWTC-2
2020/10/28

GWTC-2.1
2021/8/2

GWTC-32021/11/5

21

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) JGRG30 (online) December 8, 2021

22

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) JGRG30 (online) December 8, 2021

23

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. deg

17 August 2017

time of merger

12:41:04 UTC

signal-to-noise ratio
false alarm rate

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.
PRL 119 (2017) 161101

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

Images: time frequency traces (top), GW sky map(left, HL = light blue, HLV = dark blue,
improved HLV = green,
optical source location = cross-hair)
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 region24

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) JGRG30 (online) December 8, 2021

25

２. LV & LVK Observational Results

GWTC-2
Gravitational Wave Transient Catalog 2
arXiv:2010.14527*39 events in O3a
50 events in total* False-Alarm Rate < 2 / 1 yr
* GWyymmdd̲hhmmss for new events• 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

Test of GR
arXiv:2010.14533 Population properties26

２. LV & LVK Observational Results

GWTC-2
Gravitational Wave Transient Catalog 2

GWTC-2.1
Gravitational Wave Transient Catalog 2.1
arXiv:2108.01045

arXiv:2010.14527* re-calibrated data in O3a* includes 1201 events of FAR < 2 / 1 day* 44 events Pastro > 0.5 ( 8 new in O3a)
* 3 events retracted since Pastro < 0.5*39 events in O3a
50 events in total

55 events in total* False-Alarm Rate < 2 / 1 yr
* GWyymmdd̲hhmmss for new events

Pastro+Pterre=1
noise• GW190917 _114630 (P = 0.77) potentially NSBH
• GW190426 _190642 (P = 0.75) total mass 185 M -> 175M final (maximum ever)• GW190403 _051519 (P = 0.61) & GW190805 _211137(P = 0.95) have χ > 0.8 BH
astro• 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 effectivealigned spin of all O3a events“glitch”
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
onesourcethe latter either the lightest black hole or heaviest neutronstar observed
in aofcompact
binaryisholestheexceeding
scatter
GW190924_021846: likely the lowest-mass BBH, “glitch”
with both black3
solar masses

arXiv:2010.14529 Test of GR
arXiv:2010.14533

of the laser

Population properties

astro
astro

astro

GWTC-2GWTC-2.1

BHBH

add 36 (total 46)+8 -3 (51)NSNS

+1 (2)+0 (2)

BH+unknown+ 2 (2)+0 (2)

Total+ 39 (50)+5 (55)NSBH

27

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) JGRG30 (online) December 8, 2021

28

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) JGRG30 (online) December 8, 2021

29

LIGO/Virgo/KAGRA

GWTC-3 (Gravitational Wave Transient Catalog 3)* added 35 events in O3b

arXiv:2111.03634

90 events in total

32 BHBH, 0 NSNS, 3 NSBH
* 1048 events of FAR < 2 / day* FAR < 2/ day & Pastro > 0.5* O3b made 39 public alerts
̶> 18 were real
̶> 17 newly added as events

BHBH
NSNS
NSBH
BH+unknown
Total

Nov 5, 2021

GWTC-3add 32 (total 83)+0 (2)+3 (3)+0 (2)+ 35 (90)

arXiv:2112.xxxxx

arXiv:2111.03606
Population properties
Test of GR

BHBH
GW200220_061928 87M + 61M -> 148M

Largest in O3b

GW191204_171526 12M + 8 M -> 19 M

Eﬀective inspiral spin > 0

GW191129_134029 10.7 M + 6.7 M -> 16.8 M

Smallest in O3b

GW191109_010717 65 M+ 47 M - > 107 M

Eﬀective inspiral spin < 0**Discovery of NSBH
GW191219_163120

31M + 1.2 M

GW200105_162426**

9M+1.9M

GW200115_042309**

6M + 1.4 M

GW200210_092254

24M+2.8M

ApJL 915; L5 (2021)

retracted since Pastro = 0.36

30

LIGO/Virgo/KAGRA

GWTC-3 (Gravitational Wave Transient Catalog 3)

Nov 5, 2021

arXiv:2111.03606

Gravitational-Wave Transient Catalog 3

compact binary coalescences fromthe second part of the third observing run (O3b)

BBH
BBH
BBH
BBH
BBH
BBH
BBH
BBH
BBH
BBH
BBH
NSBH
BBH
BBH
NSBH
BBH
NSBH
BBH
BBH
BBH
BBH
BBH
BBH
NSBH / BBH
BBH
BBH
BBH
BBH
BBH
BBH
BBH
BBH
BBH
BBH
BBH
BBH

Properties of the events reported in the O3b catalog are listed above: chirp mass, in solar masses, mass
ratio , effective inspiral spin
, effective precession spin
, and distance, in Gigaparsecs.
Also listed for each event is the most likely source classification. Events labelled BBH are those that we areconfident are binary black hole coalescences. Events labelled NSBH are those that are possible neutron starand black hole coalescences. (We consider compact objects that are likely to have masses less than 3 times themass of our sun to be possible neutron star candidates).
Credits: Martin Hendry, Hannah Middleton

31

LIGO/Virgo/KAGRA

GWTC-3 (Gravitational Wave Transient Catalog 3)

Nov 5, 2021

arXiv:2111.03606

32

Population Properties in GWTC-3 (1)

LIGO/Virgo/KAGRA

Consistency of GWTC-2 & 3

arXiv:2111.03634* Populations of 77 events of FAR < 1 / year
The observations in GWTC-3 are consistent with the predictions from GWTC-2

+
-

33

Population Properties in GWTC-3 (2)LIGO/Virgo/KAGRA

Neutron Stars

arXiv:2111.03634* 7 events with NS

GW190814 is outlier

Mmax is consistent with galactic pulsars.

consistent with uniform distribution.

34

Population Properties in GWTC-3 (3)LIGO/Virgo/KAGRABlack HolesarXiv:2111.03634

binary parameters

primary mass m1

mass ratio q

power-low with single peakat 35M ﬁts well the distribution

few events over 45M
comparing with GWTC-2

35

Population Properties in GWTC-3 (3)LIGO/Virgo/KAGRABlack Hole SpinsarXiv:2111.03634

GWTC-2GWTC-3+binary formation was+ co-evolution-- dynamical

power-low with single peakat 35M ﬁts well the distribution

GWTC-3GWTC-2

χeﬀ centered at 0.05

GW191204_171526 12M + 8 M -> 19 M

Eﬀective inspiral spin > 0
0.16-0.05+0.08

Eﬀective inspiral spin < 0
GW191109_010717 65 M+ 47 M - > 107 M-0.29-0.31+0.42

χeﬀ

36

Population Properties in GWTC-3 (4)LIGO/Virgo/KAGRA

Merger Rates

GWTC-2

arXiv:2111.03634

GWTC-337

GW transient catalog

O3b (2020/11/1 - 2021/3/27)

O1

O2

GWTC-3 (2021/11/7 released)

After O3b：

O3a

O3b

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

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

38

２. LV Observational Results

GWTC-3

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

39

２. LV Observational Results

GWTC-3

Existence of IMBH over 150 Msun！
No gap over 90 Msun！
Origin of BH？

Origin of BBH？

A peak at 35 Msun in BH
mass distribution？

Compact objects
in 3‒5 Msun mass gap ?

Hyper-massive NS ? Ultra-light BH?
Exotic Object?

Max Mass of NS?

EOS of NS?

Less BNS than expected？

Origin of BNS?

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 202140

http://www.oit.ac.jp/is/shinkai/linkGW.html
LVK-EPO (Education & Public Outreach)provides Science Summaries

https://www.ligo.org/science/outreach.php

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

41

LIGO-Virgo-KAGRA network for hunting gravitational waves
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

JGRG30 online

on behalf of KAGRA collaboration

December 8, 2021

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) JGRG30 (online) December 8, 2021

43

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) JGRG30 (online) December 8, 2021

44

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) JGRG30 (online) December 8, 2021

45

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) JGRG30 (online) December 8, 2021

46

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) JGRG30 (online) December 8, 2021

47

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) JGRG30 (online) December 8, 2021

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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) JGRG30 (online) December 8, 2021

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Status of KAGRA

Basic Idea of the Interferometer“Power-Recycled” Fabry-Pérot Michelson interferometer(TAMA300, initial LIGO, Virgo)

input mirrors
Laser Source

Power-Recycling
mirrorresonance

Photonget more effective
laserDetector
power

end mirror

Sensitivity (Lower the better)end mirror

Reduce shot-noiseof laser

Frequency

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

50

Status of KAGRA

Basic Idea of the Interferometer“Signal-Recycled” Fabry-Pérot Michelson interferometer(GEO600)

input mirrors
Laser Source

resonance

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

end mirror

Sensitivity (Lower the better)end mirror

get more finesse
with SR mirror

Frequency

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

51

Status of KAGRA

Basic Idea of the Interferometer“Resonant Side-band Extraction” interferometer(KAGRA, Advanced LIGO, Advanced Virgo)

input mirrors
Laser Source

Power-Recycling
mirrorSignal-Extraction
mirrorgetPhoton
more effective
DetectorGW signals
resonance N wavelength

end mirror

Sensitivity (Lower the better)end mirror

keep at relative low finesse
with SE mirror

Frequency

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

for optical losses
for GW cancellation

52

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) JGRG30 (online) December 8, 2021

53

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) JGRG30 (online) December 8, 2021

54

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) JGRG30 (online) December 8, 2021

55

Status of KAGRA

Relative Movement

Basic Idea of Suspension System

f-2
f-4

Frequency [Hz]Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

56

Status of KAGRA

Relative Movement

Basic Idea of Suspension System

f-2
f-4
f-6

Frequency [Hz]Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

57

Status of KAGRA

Relative Movement

Basic Idea of Suspension System

Frequency [Hz]Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

58

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) JGRG30 (online) December 8, 2021

59

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) JGRG30 (online) December 8, 2021

60

Status of KAGRA

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

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

61

Status of KAGRA

KAGRA (Kamioka Gravitational-Wave Observatory)

90cm snow in one night, Dec 17 2020
Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

62

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) JGRG30 (online) December 8, 2021

63

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

1,000
970

March 29, 2020

(LVK paper)

883

655
600

594

500

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) JGRG30 (online) December 8, 2021

64

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

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

Jim Lough, LIGO-G2001554

65

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) JGRG30 (online) December 8, 2021

66

Status of KAGRA

Toward O4
O1* 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,less 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

repair & installation

80
Mpc

LIGO

O3

O4

O5

120-130
Mpc

160-190
Mpc

Target
330 Mpc

50
Mpc

90-120Mpc

150-260
Mpc

1-30
Mpc

130+
Mpc

O2
100
Mpc

30
Mpc

Virgo

1
Mpc

KAGRA

Target
330 Mpc

LIGO-India
2015

2016

2017

2018

2019

2020

2021

2022

2023

2024

2025

2026

2027

updated from LIGO-G2002127-v4

commissioning
December 2022
O4 starts

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) JGRG30 (online) December 8, 2021

67

Gravitational Wave Physics & Astronomy : Outlook (1)Last 5 years★ The ﬁrst detection of GW was 6 years ago. Since then we detected 90 events.
Most of them are BBH, and 2 BNS, 2 BHNS and 2 BH+unknown.
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) JGRG30 (online) December 8, 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 in O5 will be seconds to minutes before its merger.
O1
80
Mpc

LIGO

O3

O4

O5

120-130
Mpc

160-190
Mpc

Target
330 Mpc

50
Mpc

90-120Mpc

150-260
Mpc

1-30
Mpc

130+
Mpc

O2
100
Mpc

30
Mpc

Virgo

1
Mpc

KAGRA

Target
330 Mpc

LIGO-India
2015

2016

2017

2018

2019

2020

2021

2022

2023

2024

2025

2026

2027

updated from LIGO-G2002127-v4

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

Hisaaki Shinkai (Osaka Institute of Technology) JGRG30 (online) December 8, 2021

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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) JGRG30 (online) December 8, 2021

70