Prospects of KAGRA
Observationin the Multi-messenger Era
Keiko Kokeyama
On behalf of the KAGRA collaboration
Mar 27, 2018
at ICEHAP, Chiba University
JGW-G1808116
3/27/18

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Contents• Introduction• Detector upgrades and Near Future Observation
Prospects – LIGO and VIRGO• KAGRA Status• KAGRA’s contribution on upcoming Observations• Future Prospects of the Field

3/27/18JGW-G1808116

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Introduction• Gravitational wave astronomy has finally started 100years after the Einstein prediction• LIGO’s detection• The first detection GW150914• 2 BH-BH in Observation 1 (O1)
• 3 BH-BH in O2• LIGO-VIRGO detection• BH-BH• NS-NS – Multi-messenger Observation

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figure: LIGO Lab2

Gravitational-Waves

時間

時間
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Overview of the Detectors
Test mass (mirror)hung by a large suspension
to be isolated from seismic motions
Test mass

Fabry-perot cavities
to accumulate the effective
light path length

Power-recycling mirror
to enhance the effective
laser circulating power

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StabilizedLaser

Beam splitter

Signal-recycling mirror
to tune the frequency response

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Controlling the IFO
Lengths of optical cavities
must be the integer multipleof the laser wave length

L=Nλ
λ： laser wave length
N： Integer

ミラー

LaLIGO, VIRGO & KAGRA have 5 DoF to control
Jan/26/'17

JGW-G1706090

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Figure: M Evans

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Sensitivity Curve

Sensitivity during O2
PRL 119 141101 (2017)

Supernovae

Seismic Noise

Quantum Noise
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Thermal Noise
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7Detectors with State-of-ArtTechnologies
Quantum Noise

Seismic Noise

Thermal Noise

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Figures: H Yamamoto

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B Barish, LIGO-G1600214
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9L-V Observation Plan
LIGO

80-100 Mpc

120 Mpc

O2

post O2
2017. 8O3

2018. 11O4

Post O3
2019. 112020. 11

VIRGO
24Mpc

60 MpcCommissioning

O2
2017. 7
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post O2
8O3

2018. 112019. 11JGW-G1808116

O4

Post O3
2020. 1110

Upgrades towards O3
LIGO• Power up to 50W• Squeezing input• 40% reduction of shot noise• Optic swap
• Stray light control• Vacuum System repair

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Upgrades towards O3
LIGO• Power up to 50W• Squeezing input• 40% reduction of shot noise

Barsotti, LIGO-G1800598• Optic swap
• Stray light control• Vacuum System repair

Target 3dBSqueezing
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Upgrades towards O3
VIRGO• Monolithic suspension• vacuum system upgrade &cleaning• Laser High power amp(100W) installed• squeezer being installed• Newtonian noise
subtraction

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Beam splitter

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International Observation
Network in the near Future
2011
600m Arms

GEO600-HF2015
4km Arms

aLIGO
Hanford

2019
3km Arms

aLIGO
Livingston
2015
4km Arms

KAGRA

Advanced
VIRGO
2016
3km Arms

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LIGO India
2025?
4km Arms

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KAGRA

Toyama BayToyama City

XMASS
(Dark matter)

XMASS

CLIO
CLIO
(重力波)

Kamland(Neutorino)

Kamland

Super K

KAGRA
KAGRA
(重力波)
KAGRA Entrance
SK Entrance

Figure: O Miyakawa

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Underground and Cryogenic
X arm

KAGRA
Tunnel

A Shoda, JGW-G1605219

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Figure:Yamamoto JGW-G1808095

KAGRA Status
Engineering run

Phase-13km
CryoPhase-2
2018. 5Phase-3O3?

2019. ?
UpgradedConfig

Noise Hunting
Further Upgrades

Higher power
3km cavities
Recycling mirrors?

LIGO & VIRGO
120 Mpc
O2

post O2

O3O4

Post O3

DesignSensitivities

60 MpcO2
2017.
89
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post O2
2018. 11O3
2019. 11JGW-G1808116

O4

Post O3
2020. 1117

Detectors Status
RealSapphire
Spare
Sapphire
1W

PR2 (type Bp)

BS (type B)

Cryogenic ETMYEY (type A)

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Figures: KAGRA VIS & CRY team

Cryo-payloadwith a sapphire hung18Detectors Status

Figures: KAGRA AOS teamWide Angle Baffle
Transmitting port
detection bench
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Sensitivity Threshold for O3- Tagoshi, JGW-G1808094

Considering various BNS range of KAGRA
Various possibilities of KAGRA's sensitivity

KAGRA(1Mpc)
KAGRA(5Mpc)
KAGRA(10Mpc)
KAGRA(20Mpc)
Virgo(60Mpc)
LIGO(120Mpc)
JGW-T1707556
JGW-T1707569
JGW-T1808031
LIGO, Virgo: taken from arXiv:1304.0670
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20Improvement forSource localization (preliminary)- Tagoshi, JGW-G1808094

An example case study:

3/27/18•BNS range (average observable distance with SNR=8):o KAGRA: 10Mpc
o LIGO: 120Mpc
o Virgo: 60Mpc•Source:o BNS (1.4, 1.4) Msolar at 40Mpc
o Uniform distribution for sky location, inclination, polarizationo 5000 realizations•Method :o Fisher matrix, Simple TaylorF2 waveform
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Improvement for
Source localization (preliminary)- Tagoshi, JGW-G1808094

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22Improvement forSource localization (preliminary)- Tagoshi, JGW-G1808094

Only ρKAGRA > 2 cases
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GW170817 case: ΔΩ ~ 30 deg223

Sky Localization Accuracy- Tagoshi, JGW-G1808094

Baysian parameter estimation simulation
Source:BNS (1.4, 1.4) Msolar at 40Mpc
Inclination = 30 deg
BNS range of detectors:
LIGO: 120Mpc, Virgo: 60Mpc , KAGRA: 10Mpc
Detectors

HL

HLV

HLK

HVK

LVK

HLVK

90% ΔΩ [deg2]

66.4

14.0

32.5

15.7

27.6

10.1

Injected SNR 19.4 (H), 26.2 (L), 2.7 (V), 3.5 (K)Detectors

HL

HLVHLK

HVK

LVK

HLVK

90% ΔΩ [deg2]

10030.2

50.3

308.3

35.4

19.1

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Summary• KAGRA will perform test operation with cryogenic Michelson
configuration in April (phase-1)• Upgrade to the Full-configuration Cryogenic Interferometer will follow• KAGRA will try to join O3• Evaluation of sensitivity threshold to join O3 has started among KAGRA
Joint efforts with LIGO and Virgo are starting soon
We are working very hard to join the next LIGO and Virgo observation

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- from Tagoshi, JGW-G1707454-v3

Future: With Full KAGRA Sensitivity
NS-NS@180Mpc (95%CI)(1.4,1.4)Msun
LHV
median of δΩ [Deg2]

30.25

J.Veitch et al., PRD85, 104045 (2012)(Bayesian inference )See also Rodriguez et al. 1309.3273

LHVK
9.5

L:LIGO-Livingston
H:LIGO-Hanford
V: Virgo
K: KAGRA
I: LIGO-India

direction, inclination, polarization angle
are given randomly

BH-NS@200Mpc(10,1.4)Msun

LHV

LHVK

LHVKI

median of δΩ [Deg2]

21.5

8.44

4.86

Tagoshi, Mishra, Arun, Pai, PRD90, 024053 (2014) , Fisher matrix
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Further Future Outlook
Next Generation:- LIGO Voyager (silicon cryogenic)
Future Ideas:- Cosmic Explorer (US, 40km, cryogenic…etc)- Einstein Telescope (EU, 10km) … or identical detectors?

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