JGW-G1301945-v2

Status of KAGRA
andfor the Detection of Gravitational Waves from SNe
Nobuyuki Kanda (Osaka City U.)
KAGRA collaboration
30th Oct. 2013, Conference on Supernovae
YIPQS lon-term workshop “Supernovae and Gamma-Ray Bursts in Kyoto, 2013”

Plan of Talk
Gravitational Wave
• What ?
• How to detect
KAGRA• Conceptual Design• Schedule• Construction Status
GW from SNe• Possible Radiation Scenario• What can be obtained from GW detection?
(GW and GRB)
2

What is Gravitational Wave ?
Gravity distorts the space-time !
Einstein Eq. 1
Rµgµ R =Tµ
2
ct x y z ct
metric tensor
1 0 0 0“flat” space-time (Minkowski)x
0 1 0 0gµ = µ =0 0 1 0 y
0 0 0 1 z
“curved (distorted)” space-time

gµ

=

µ

small perturbation ‘h’ --> Waves
g µ = µ + hµ
2
1
2
h
=
0
µ
c 2 t2
3

flat space-time

distorted space-timeby mass = gravity

Gravitational Wave
propagation of distortion4

GW radiation• Sourcechange (time derivative) of quadrupole
moment of mass distribution
Iµ =dV (xµ x

12µ r ) (r)3

• Amplitude
inversely proportional to the distance2G ¨
between source and observer
hµ =
Iµ
Rc4

• Energy
total energy is given as : EGW
4... ...µ
G
>
<
I
I
µ
5c5

Need direct measurement.
Why direct measurement ?
• We have to test in ‘strong’ gravity field !
Past experimental GR tests had been done in weak gravity
field (in Solar system)
Direct measurement of wave property is importantas the test of a fundamental interaction .
• GW waveform carry information of its sources
New probe for astrophysics and cosmology• Tagging GW events = seeing sources
Gravitational Wave Astronomy
Possible sources are also attractive for us:
black-hole, neuron star, supernovae, cosmic string, etc...
5

Possible GW sources
Event Like
It will occur suddenly. Sometime it can be luminous!
• Compact Binary Coalescence(Neutron Star-NS, NS-Blackhole, BH-BH)• Supernova(Stellar-core collapse)• BH QNM• Pulsar glitch
Continuous
It exists anywhere, anytime in our universe ...
• Rotating Pulsar• Binary• Stochastic Background(+Unknown sources)

typical target : h
6

10

22

10

24

GW signal (example: NS-NS Coalescence)time seriesInspiralmergerringdown

strain equivalent noise spectrum [1/rHz]

Inspiral7

mergerBH ringdown

frequency
domain

-20

10

-21

10

-22

10

LCGT sensitivity limit
VRSE(D)
VRSE(B)NS NS h(f)*f^(1/2)

Inspiral

-23

10

???
mergerringdown

-24

10

10

100
frequency [Hz]1000

GW signal (example : Supernova)
Supernova (type II) will emit
short duration GW (Burstwave) according to various
processes in it.
• Rotational Core
collapse (Bounce)• Convection• Proto-neutron starformation and g-mode
instability• Standing-AccretionShock Instability• ...

Dimmermeier et al.
8How to detect GW
Free
Test
Masses&Laserinterferometerx
flat space-time

Free mass = mirror

Mirrorlight

distorted space-timet

Beam Splitter
Laser Lightx

MirrorInterferencecos( 2 pi 2dL /lambda)

Michelson Interferometert9How to detect GW
Free
Test
Masses&Laserinterferometerx
flat space-time

Free mass = mirror

Mirrorlight

distorted space-timet

Beam Splitter
Laser Lightx

MirrorInterferencecos( 2 pi 2dL /lambda)

Michelson Interferometert9How to detect GW
Free
Test
Masses&Laserinterferometerx
GW

flat space-time

Free mass = mirror
lightt
distorted space-time

MirrorBeam Splitter
Laser Lightx

MirrorInterferencecos( 2 pi 2dL /lambda)

Michelson Interferometert
9

Schematic Figure• Free mass --> suspended mirror
To integrate strain ‘h’ --> long
baseline arms.
• Limited size --> Folding arms /Storage cavity• Against noises -->high power laser
Coolingetc..

merit on long base-line<-- mirror and suspensionof CLIO interferometer(prototype of KAGRA)
10h =Global Network of GW detectors

LIGO (Livingston) 4km

GEO 600m

advanced LIGO

Virgo 3km

LIGO (Hanford) 4km & 2km

advanced Virgo

IndIGOTAMA 300m
CLIO 100m(LIGO-India)

3km
11KAGRA
Underground• in Kamioka, Japan• Silent & Stableenvironment
Cryogenic Mirror• 20K• sapphire substrate
3km baseline© ICRR, university of Tokyo
Plan• 2010 : construction started• 2015 : first run in normal temperature• 2018 (or late 2017)- : observation with cryogenic mirror
12

LCGT

KAGRA
Underground• in Kamioka, Japan• Silent & Stableenvironment
Cryogenic Mirror• 20K• sapphire substrate
3km baseline~1000m under themountain© ICRR, university of Tokyo
Plan• 2010 : construction started• 2015 : first run in normal temperature• 2018 (or late 2017)- : observation with cryogenic mirror
12

LCGT

KAGRA~1000m under themountain

Underground• in Kamioka, Japan
Thedetectorwillbeconstructed
Cryogenicmirrorswill• Silent & Stable
underground Kamioka
undergroundKamioka.
beusedtoreducethe
be used to reduce theenvironment
thermalnoise.
 Reductionofseismicnoise(by2@0.550Hz).
approximately10
Cryogenic Mirror
Hopingtoreachtheworldbestsensitivity.
• 20K(NSNSmergerwithin>200MPctobeobserved.
• sapphire substrate
3km baseline© ICRR, university of Tokyo
Plan• 2010 : construction started• 2015 : first run in normal temperature• 2018 (or late 2017)- : observation with cryogenic mirror
12

LCGT

4

KAGRA~1000m under themountain

Underground• in Kamioka, Japan
Thedetectorwillbeconstructed
Cryogenicmirrorswill• Silent & Stable
underground Kamioka
undergroundKamioka.
beusedtoreducethe
be used to reduce theenvironment
thermalnoise.
 Reductionofseismicnoise(by2@0.550Hz).
approximately10
Cryogenic Mirror
Hopingtoreachtheworldbestsensitivity.
• 20K(NSNSmergerwithin>200MPctobeobserved.
• sapphire substrate
3km baseline© ICRR, university of Tokyo
Plan• 2010 : construction started• 2015 : first run in normal temperature• 2018 (or late 2017)- : observation with cryogenic mirror
12

LCGT

4

KAGRA collaboration
viewgraph by K.Kuroda

KAGRA Collaboration in the world• Research organizations of laboratories anduniversities are 41 in Japan and 38 in overseas• 158 researchers in Japan and 67 in abroad,
225 members in total

13

Sensitivity Limit of KAGRA
h ~ factor x 10-24 [/√Hz] for observation band
KAGRA sensitivity limit
VRSE(D)
VRSE(B)-20

strain equivalent noise spectrum [1/rHz]

10

Noise budget
mirror substrate Brownian thermal noise
mirror substrate thermoelastic noise
seismic noise
standard quantum limit

-21

10

VRSE(D) quantum noise
VRSE(B) quantum noise
suspension thermal noise

-22

10

-23

10

-24

10

-25

10

10

100
14
frequency
[Hz]

1000

Detection Range

100Myr

1Gyr

10Gyr

13Gyr

100Gpc
10Gpc
1Gpc
10Mpc

For supernovae, the
0.01
range may be
typically 100kpc~1Mpc or as like, 0.001
depending on themodel (waveform).

Look Back Time

0.1

100MpcLuminocity Distance-> 10 event/yr

LCGT detection range (VRSE-D)
Detection Range (with optimal direction)
for CBC| for BH QNM
SNR=3
|
SNR=3
SNR=8
|
SNR=8
SNR=100|
SNR=100

1.4Msolar (Typical Neutron Star)(~158Mpc in all sky
average, LIGO definition)

Cosmological Redshift : z

KAGRA’s NS-NS
10detection range is
280 Mpc for optimal
direction and orbit
1
inclination.

10

0

10

15

1

2

10
mass of one star [Msolar](BH mass = 2M)

10

3

10

4

Schedule&
TargetBudgetandrevisedschedule
Calendaryear

2010

2011

2012 20132014 20152016

Oct2013

by T.Kajita

2017 2018

Projectstart(~1yeardelay…)

Tunnelexcavation
initialͲKAGRA

iKAGRA obs.
baselineͲKAGRA

Adv.Opticssystemandtests
Cryogenic system
Cryogenicsystem

Observation
GWIC
roadmap
Budgethttps://gwic.ligo.org/roadmap

LeadingͲedge…
Excavation
Additionalbudget
Budget foroperation?
GrantsͲinͲaid forSci.?

Detector(notapprovedyet)
16

Requested.Wehavenotofficiallychanged
theschedule(yet).

iKAGRA and bKAGRA

iKAGRA andbKAGRA
andbKAGRA viewgraph by T.Kajita

iKAGRA (~2015)

bKAGRA (2016~)䂹Simpleinterferometerwith:roomtemperatureoperation,
10Wclasslaser,andnopowerandsignalrecycling
䂹 However,fullendͲtoͲend(relativelyshort)observation,in
ordertoexperiencetheoperation
andtounderstandthepotential
problemsassoonaspossible.

䂹Advancedinterferometerwith:powerandsignalrecycling,butstill
roomtemperatureoperation.
䂹 FullbKAGRA with;powerandsignalrecycling,
cryogenicsapphiremirrors,
and>150Wlaser.

17
KAGRAprojectͲͲ TakaakiKajita

17tunnelby T.Uchiyama•

Excavation from Mozumi entrance finished on
2013/03/06.
The Yend has been completed except for thevertical hole. Length of the Y arm tunnel is1165m.
Center area has been completed except for thevertical hole.
The current progress of Xarm and Yarm are 1950m
and 1385m, respectively.
Yarm tunnel will be completed on 2013/12.
 on 2014/03.
The excavation will be completed


6

•


5
(%
Rail methodJ

••••1165m 1385ｍ;I0 J

Tunnel subgroup brief report for the KAGRA
international collaboration meeting on 2013/10/09.
&
"$%*!'
2F Tire method#'&")!"
1950m
J



5


4

"(%*!',*'*)+
,*'*)+
&*(&1 J

 J

Mozumi tunnel
Tire method





J



'/+%"*+&&$
$(.-"-*"& 


J


1




2


3


3


2

J

,*'*)+*+&&$"(%*!'Y arm (Mozumi side)
;I0J
Tire method (%,*'*)+ &*((Y end
"(%*!'"(%*!'
Tire method;I0J

JGW-G1301891
'/+%"&*(&

18

Takashi Uchiyama, ICRR

Tunnel Excavation

Tunnelexcavation

viewgraph by T.Kajita

NewAtotsu entranceEndofApril,2012

MidJune,2012

KAGRAprojectͲͲ
19 TakaakiKajita

19Tunnel Excavation

20

Tunnel Excavation20Vibration isolation and cryostat
viewgraph by K.Yamamoto,
S.Koike & R.Takahashi

14 m

Vibration
Isolation

Cryostat21

Cryogenic mirror

Cryostat22

Cryostat

Cryostats

Cryostat #1, #2, #4 : Move to the Miyakawachou Storage

viewgraph by T.Suzuki(7/27, 7/28)

Cryostat #3 : Extra cooling test of 1/2 payload with dummy baffles in July and Aug.
Vibration measurement by Roma and ICRR accelerometers.
Waiting for transportation to Miyakawachou Storage.

Y. Sakakibara

23

D. ChenClean Booth Plan for Cryostats
viewgraph by S.Miyoki

24Optics ( Mirror,
Buffle ) polish
Sapphire
Sapphiretest-polish
We confirmed sapphire,although it is very hard,
wassuccessful.
can be polishedas theZYGOCALTECH

Unit: [nm]

180mm

140mm

180mm

140mm

RMS
(-6 terms)

0.48

0.24

0.45

0.21

Z2,2

-0.68

-0.41

-0.30

-0.13

Z2,-2

0.45

0.26

0.29

0.27

same level as silica.
Next challenge is how
well uniformity
viewgraph
byand
N.Mio
homogeneity of opticalproperties) can beachieved on it.

Example of a large baffle
#3 Narrow-angle baffle
Material: A5052

400#mm#radius

Surface: electro-chemical buffed (ECB)
Blackened surface: Solblack

ECB: low scattering
Solblack: Vacuum Compatibility (10-7Pa), Cryogenic compatibility (<8K), Low
reflectivity (~2%@1064nm), Applicablefor a large work

25

LSC meeting xxxviewgraph by T.Akutsu
10Network design for control and DAQ

NetworkdesignforcontrolsandDAQ
RFMRTcontrolsignal:verylowlatency
DAQGWdata:hugeamount,lowlatency
Timing: Synchronizationforall
RTPCandADC/DAC

GPSantenna

TCP/IP:EPICS,NFS,networkboot
Mozumi
Entrance

GWbuildings
atKamioka
RemotecontrolData
storage

NewAtotsu
Entrance

MainData
storage
ICRR@Kashiwa
26 TakaakiKajita
KAGRAprojectͲͲ

viewgraph by
O.Miyakawa
35

iKAGRA Data System
The equipments will be installed at Kamioka and Kashiwa by the end of February 2014.
Kamioka Mine

Kamika (outside)

Kashiwa campus, ICRRSINET(ICRRʼ s VPN)
VPN

VPN

DGS

DGS

frame writer

frame writer

KAGRA general pupose intranet

primary storage primary storage

precess

precess

precess

precess

login

login

node

node

node

node

serverserverserverserverdata server
FC

DGS Storage

FC

100 TiB Luster file system
for iKAGRA two months obs.

optial ﬁber(~4.5km)capacity >100 TiB
job mamagement

DGS Storage

serverdata server

200 TiB Luster file system

job mamagement

for safety spool and general purpose
on-site processing/studies.

servercapacity >200 TiB

A. Inside MineB. Analysis Building at Kamioka

27

5PB system will beavailable for bKAGRA.

C. Kashiwa Campus

iKAGRA Data System
The equipments will be installed at Kamioka and Kashiwa by the end of February 2014.
Kamioka Mine

Kamika (outside)

Kashiwa campus, ICRRSINET(ICRRʼ s VPN)
VPN

VPN

DGS

DGS

frame writer

frame writer

KAGRA general pupose intranet

primary storage primary storage

stream of raw data

precess

precess

precess

precess

login

login

node

node

node

node

serverserverserverserverdata server
FC

DGS Storage

FC

100 TiB Luster file system
for iKAGRA two months obs.

optial ﬁber(~4.5km)capacity >100 TiB
job mamagement

DGS Storage

serverdata server

200 TiB Luster file system

job mamagement

for safety spool and general purpose
on-site processing/studies.

servercapacity >200 TiB

A. Inside MineB. Analysis Building at Kamioka

27

5PB system will beavailable for bKAGRA.

C. Kashiwa Campus

Amount of Data
phase

iKAGRA
commissioningbKAGRAduration

about 2~3 months
at end of 2015

data rate / duty

total expectedamountfrom -> to20MB/s / 100%

100 TiB

Kamioka -> Kashiwa

1MB/s / 100%

5TiB

Kamioka -> Osaka City U./Osaka U.

20MB/s / ?(5~10%)?

Kamioka -> Kashiwa

1MB/s / ?(5~10%)?

Kamioka -> Osaka City U./Osaka U.

20MB/s / 100%

3PB / 5yrs

Kamioka -> Kashiwa

1MB/s / 100%

150 TiB / 5yrs

Kamioka -> Osaka City U./Osaka U.

2016-20172017 (end of KAGRA)

iKAGRA : normal temperature operation at end of 2015
bKAGRA : cryogenic hi-sensitivity observation after midof 2017 or 201828

Data Analysis

Data$analysis$ac+vi+es

Current$ac+vi+es:$! Development$of$data$analysis$package$for$KAGRA$! We$have$determined$the$name$of$data$analysis$
library$for$KAGRA.$$$$"KAGALI":$KAGRA$Algorithmic$Library$$! We$are$now$wri+ng$the$data$analysis$white$paper.$29

GW from supernovae
Supernova will emit GW
in various phase of its development.
• core bounce• convection• formation of proto-neutron star
g-mode oscillation• neutrino emission• accretion
cf: SASI (standing-accretion-shock instability)• etc.
30

Dimmermeier at al.

GW from supernovae
Supernova will emit GW
in various phase of its development.
• core bounce• convection• formation of proto-neutron star
g-mode oscillation• neutrino emission• accretion
cf: SASI (standing-accretion-shock instability)• etc.
What is a key feature

Dimmermeier at al.

from the view of GW detection and analysis ?
30

GW waves : view of event detection ...
Features

Supernovae

Compact Binary Coalescence

GW waveform“Burst” various prediction,
but is NOT well-known or hard to
give waveform analytically“Chirp” Post-Newton+“Merger” Numerical Relativity+“Ringdown” Perturbation of BH(analytical + NR waveforms)

Detection(SignalIdentiﬁcation)•Excess power ﬁlter(Integration of signal power),•Time-Frequency analysis(Sonogram by Short-FFT, Wavelet
etc.)

Matched ﬁlter between
signal and templates(Winer optimal ﬁlter)≤1Mpc~200 Mpc

EM (visible-infrared,
X-ray, Gamma-Ray),
Neutrino

EM (visible-infrared,
X-ray, Gamma-Ray),
Neutrino

Typical Rangefor current detectors.

Follow-ups /Counterparts

31

Detectability of GW from SNe
Typically, the detection range is
ΔTroughly ≤1Mpc.
Excess power filter• Integrate signal power between wider
frequency band around certain arrivaltime.
• It may give most high S/N.
• Structure (waveform, accurate timing)of the signal might be lost.
Time-Frequency analysis• There are many methods !
(Sonogram/Spectrogram with ShortFFT, Wavelet etc.)• These are looks fine to give
example : ROC for the SNe at Galactic center in
information in t-f domain.
h(t)time[ms]32

KAGRA study (See M.Asano’s poster [P49] )Obtained from GW of SNe
What can be obtained from GW
observation of SNe ?
Simply three things :• Structure• Dynamics• Kinematics
33

Structure
If we will get the GW,
the SN is not spherical symmetry !
• There are some asymmetric development of SNe, at core?
shock? convection?(density or temperature), etc.
• It is simply happy scenario for both GW experimentalists andtheorists.

If we will NOT found any GW at close SN event(s),the SN might be completely symmetric.
• ...It is terrible scenario for experimentalists (and current
simulation predictions also!)..., but unhoped-for exciting
situation...
It may hard to proof really no GW or detector disorder...
34

Structure
If we will get the GW,
the SN is not spherical symmetry !
• There are some asymmetric development of SNe, at core?
shock? convection?(density or temperature), etc.
• It is simply happy scenario for GW
both or
GWno-GW
experimentalists
andis simple,
theorists.
however, have to be confirmed

foratcurrent
our works.
If we will NOT found any GW
close SN
event(s),the SN might be completely symmetric.
• ...It is terrible scenario for experimentalists (and current
simulation predictions also!)..., but unhoped-for exciting
situation...
It may hard to proof really no GW or detector disorder...
34

predict waveformndenceternti detectors

Supernova

Dynamics

Fig.1 KAGRA antenna
pattern

When strong GW will be emitted ?
• GW before neutralization burst suggest that thecore is highly rotating.
after neutralization
burst,
does notrotate.
GW
and core
Neutrino
signalson • GWTime-correlated

sis motivation, method and results

ming window
neutrinos

el are used

h longte highhigh

No core rotation casecore rotation : pi[rad/s]

GW waveform

GW waveformNeutrino luminosity

Neutrino luminosity

short
te low
low

ysis

N

-O

-M
-E
can
-C
FAR

Res
-W

- In
wou

Simulation by Y.Suwa (drawn
byT.Yokozawa)S/N threshold dependence of
35

efficiency, False Alarm Ratio

Timing analysis is important !

Neutron tagging is a key point to identify interaction

trino-GW
Timing ofcoincidence analysis e.g. Neutrino and GW timingd Neutrino information :• neutrino
GW time : t1
detected
GW signal (Use 0.2[sec]-)
mber of observed event : N• Neutrino
istributionof t1 for each N
e window width which can 99% GW signalve • EMte S/N threshold from window width andNeutrino interact rate [event/1msec]
areimportanttoe-5[/window]
Start observation from 0.18[sec]know
thecase of Galatic Center SNe
N=23 neutrinos
are observedof SN.
dynamics

ow width = 0.61[sec]hreshold 5.03
iency 54.3%
of N=15~35, GW detection efficiency
53-55%

mary

1st observed neutrino time (N=23)

99% GW observable timing window widthSeeposter byobserved
T.Yokozawa
Time profile
of neutrino
event inin detailcase of[P08]N=2336

erating with Theory, Neutrino analysis group and GW analysis group, make Supernovae simulation

Timing analysis is important !

Neutron tagging is a key point to identify interaction

trino-GW
Timing ofcoincidence analysis e.g. Neutrino and GW timingd Neutrino information :• neutrino
GW time : t1
detected
GW signal (Use 0.2[sec]-)
mber of observed event : N• Neutrino
istributionof t1 for each N
e window width which can 99% GW signalve • EMte S/N threshold from window width andNeutrino interact rate [event/1msec]
areimportanttoe-5[/window]
Start observation from 0.18[sec]know
thecase of Galatic Center SNe
N=23 neutrinos
are observedof SN.
dynamics

ow width = 0.61[sec]hreshold 5.03
1st observed
neutrino time (N=23)
Comparison between
GW andiency 54.3%
should be done inof N=15~35, GW detectioncounterparts
efficiency
53-55%

marytime domain.

99% GW observable timing window widthSeeposter byobserved
T.Yokozawa
Time profile
of neutrino
event inin detailcase of[P08]N=2336

erating with Theory, Neutrino analysis group and GW analysis group, make Supernovae simulation

h [10-21 atKinematics

10
50
B12X1β0.1

-5
-10

all
hyd & grav
mag

-15

• Where dominant GW power come from -20? core-bounce? convection? SASI?
0
20
40
60
80
100
• Does Magnet-Hydro Dynamics
induce large mass ejecta t-t? [ms]& BURROWS
Vol. 707b25

h [10-21 at 10 kpc]

20
15
10
5
B12X5β0.1

0all
hyd & grav
mag

-5
-10

Figure 2. Sample ofMurphy,
GW strain (hthe distance,
D, vs. time after+ ) times
Ott,
Burrows,
2009
bounce. This signal was extracted from a simulation using a 15 M% progenitor
model (Woosley & Heger 2007) and an electron-type neutrino luminosity ofLνe = 3.7 × 1052 erg s−1 . Prompt convection, which results from a negative
entropy gradient left by the stalling shock, is the first distinctive feature in the
GW signal from 0 to ∼50 ms after bounce. From ∼50 ms to ∼550 ms pastbounce, the signal is dominated by PNS and postshock convection. Afterward
and until the onset of explosion (∼800 ms), strong nonlinear SASI motions
dominate the signal. The most distinctive features are spikes that correlate with37

30
25

0

20

40
60
t-tb [ms]80

Takiwaki & Kotake, 2011

GW might suggest what is a15dominant process to51 erg.
supply explosion energy
of
10
10
-21

at 10 kpc]

20

5

100

h [10-21 atKinematics

10
50
B12X1β0.1

-5
-10

all
hyd & grav
mag

-15

• Where dominant GW power come from -20? core-bounce? convection? SASI?
0
20
40
60
80
100
• Does Magnet-Hydro Dynamics
induce large mass ejecta t-t? [ms]& BURROWS
Vol. 707b25

h [10-21 at 10 kpc]

20
15

10 NR simulations
How to : Theories and5
propose possible mechanisms.
B12X5β0.1
↓↑ 0
all
-5
grav
How much : GW measurement may hyd & mag-10
obtain how much energetic
0
20 really,
40
60
80
100
t-t [ms]
respectively.
30bFigure 2. Sample ofMurphy,
GW strain (hthe distance,
D, vs. time after+ ) times
Ott,
Burrows,
2009
bounce. This signal was extracted from a simulation using a 15 M% progenitor
model (Woosley & Heger 2007) and an electron-type neutrino luminosity ofLνe = 3.7 × 1052 erg s−1 . Prompt convection, which results from a negative
entropy gradient left by the stalling shock, is the first distinctive feature in the
GW signal from 0 to ∼50 ms after bounce. From ∼50 ms to ∼550 ms pastbounce, the signal is dominated by PNS and postshock convection. Afterward
and until the onset of explosion (∼800 ms), strong nonlinear SASI motions
dominate the signal. The most distinctive features are spikes that correlate with37

25

Takiwaki & Kotake, 2011

GW might suggest what is a15dominant process to51 erg.
supply explosion energy
of
10
10
-21

at 10 kpc]

20

5

Obtained from GW of SNe !
• Structure : Symmetry or NOT• Dynamics : Rotating or NOT• Kinematics : Where come from51
explosion energy 10 erg
Important key is ‘timing’ analysis.
(GW itself and between counterparts)
38

GW and GRB
Features

Supernovae

Follow-ups / EM (visible-infrared,
X-ray, Gamma-Ray),Counterparts
Neutrino

Compact Binary Coalescence
EM (visible-infrared,
X-ray, Gamma-Ray),
Neutrino
Metzger & Berger

e event (Phinney 2009; Mandel & O’Shaughnessy, for example an association with specific stellar
ations (e.g., Fong et al. 2010).
tivated by the importance of EM detections, in thiswe address the critical question: What is the mostsing EM counterpart of a compact object binary
er? The answer of course depends on the definition
most promising”. In our view, a promising counBerger,
rt should exhibit four CardinalMetzger
Virtues, &namelyit 2011d:“Kilonova”

Jet−ISM Shock (Afterglow)
Optical (hours−days)
Radio (weeks−years)

Ejecta−ISM ShockRadio (years)

θobs
GRB

(t ~ 0.1−1 s)

Kilonova

Optical (t ~ 1 day)θj

Merger Ejecta
Tidal Tail & Disk Wind

Be detectable with present or upcoming telescope
facilities, provided a reasonable allocation of resources.

v ~ 0.1−0.3 c

BH

EM Follow-ups are expected for
GW. aLIGO,
Virgo alreadystartedAccompany
high fractionof GW events.
these cooperative works.

Be unambiguously identifiable (a “smoking gun”),
such that it can be distinguished from other astrophysical transients.

NS-NS merger
may emit EM
radiation.

39

Fig. 1.— Summary of potential electromagnetic counterparts

KAGRA also starts cooperation...
“New Developments in Astrophysics Through Multi-Messenger
Observations of Gravitational Wave Sources” (Head : T.Nakamura)by Grant-in-Aid for Scientific Research on Innovative Areas, MEXT
Japan
Invite possible counterparts / follow-up channels of Japan !!
• X-ray and Gamma-ray• Optical, Infrared and Radio• Neutrino• GW low latency analysis• Theory for GW andcounterpart
The project started in 2012.
KAGRA and these partners
are ‘open-minded’ for also international partners.
40

Summary• First GW detection is near future !
• KAGRA construction steadily
iKAGRA ~ end of 2015
bKAGRA 2018~ (or late 2017~)• Supernova is promising GW source.
GW is expected to give rich informationfor SN - its structure, dynamics andkinetics.
41