重力波天体からの電磁波放射
Electromagne2c Emission from
Gravita2onal Wave Source

田中 雅臣
Masaomi Tanaka(Na$onal Astronomical Observatory of Japan)

GW sourcesSupernova
massive stars

NS or BH

NASA

M. Weiss

Rate

Compact binary merger~ 0.01-0.02 yr-1 Gal-1

NS-NS: ~ 10-4 yr-1 Gal-1
BH-NS/BH-BH: ~ 10-6 yr-1 Gal-1

Extragalac2c

Distance

Galac2cd ~100 Mpc - 1Gpc
z~ 0.02-0.2

Expected
number

~ 0.01-0.02 events yr-1

~ 0.1-100 events yr-1

The ﬁrst detec2on!!

- Direct proof of GWs- Existence of ~30 Msun BH- Existence of
30 Msun BH binary=> Kanda-san’s talk

LIGO Scien$ﬁc Collabora$on
and Virgo Collabora$on, 2016, PRL, 061102

1 degSDSS

GW150914
Localiza2on ~ 600 deg2(~< 10 deg2 with
Advanced Virgo and KAGRA)

10 degElectromagne2c (EM)counterparts- Redshi_ (distance)- Host galaxy- Local environment
Talks by Kanda-sanand Yoshida-sanhUp://www.ligo.org/detec$ons.php

Degeneracy between
inclina2on and distance

Local environments
7

Figure 11:

FIG. 2. etPosterior
PDFs for the source luminosity distance DL and
AbboU
al.
2016
the binary inclination ✓JN . In the 1-dimensional marginalised
distributions we show the Overall (solid black), IMRPhenom(blue) and EOBNR (red) PDFs; the dashed vertical lines mark the

HubbleWide-Field Camera
3 images
location
FIG. 3. SpacePDFsTelescope
for the source-frame
mass andspin of ofthetheremBerger(forGRBs)hostofgalaxies
arcsecond
positionsandno(host-lessInant BH 2014
producedbyshortthecoincident
coalescence
the binary.
In bursts).
thewidefield and thebottom paneldistributions
is zoomed onwe
the show
GRB location(red circ1-dimensional
marginalised
the Overall“G2”
represent
the objects withlowestand second(solidinblack),
IMRPhenom(blue)theand
EOBNR(red) lowest
PDFs; probabil
thefield. The magnitude limits at the GRB positions are mF160W > 26 mag,Electromagne2c Emission from
Gravita2onal Wave Source• EM emission from compact binary mergers• Kilonova/macronova emission andthe origin of r-process elements

Electromagne2c signature from compact binary merger(NS-NS or BH-NS)•

X-ray/gamma-ray

strophysical Journal, 746:48 (15pp), 2012 February 10

specific stellar populations). Because merger counterparts
redicted to be faint, obtaining a spectroscopic redshift
allenging (cf. Rowlinson et al. 2010), in which caseroscopy of the host galaxy is the most promising means
taining the event redshift.
s important to distinguish two general strategies for conng EM and GW events. One approach is to search for a
signal following an EM trigger, either in real time or at
t-processing stage (e.g., Finn et al. 1999; Mohanty et al.
). This is particularly promising for counterparts predicted
cur in temporal coincidence with the GW chirp, such as-duration gamma-ray bursts (SGRBs). Unfortunately, mostpromising counterparts (none of which have yet been
endently identified) occur hours to months after coales.6 Thus, the predicted arrival time of the GW signal willn uncertain, in which case the additional sensitivity gained
this information is significantly reduced. For instance, if
me of merger is known only to within an uncertainty ofurs (weeks), as we will show is the case for optical (radio)
erparts, then the number of trial GW templates that mustarched is larger by a factor ∼104 –106 than if the merger
is known to within seconds, as in the case of SGRBs.
second approach, which is the primary focus of this paper,
M follow-up of GW triggers. A potential advantage in thisis that counterpart searches are restricted to the nearby• Radio

Metzger & Berger

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

Ejecta ISM ShockRadio (years)

GRB

obs

(t ~ 0.1 1 s)

Kilonova

Optical (t ~ 1 day)j

Merger Ejecta
Tidal Tail & Disk Windv ~ 0.1 0.3 c

BH• Op2cal/NIR

Figure 1. Summary of potential electromagnetic counterparts of NS–NS/
NS–BH mergers discussed in this paper, as a function of the observer angle
θobs . Following the merger a centrifugally supported disk (blue) remains around& accretion
Bergerlasting2012!1 s
the central compact object (usually Metzgera BH). Rapid
powers a collimated relativistic jet, which produces a short-duration gamma

Short gamma-ray burst (GRBs)
VisibleNot visible

Opening angle ~ 10 deg=> probability ~ a few %

20
18

Long

16

Short

Number

14
12
10
8
6
4
2
0
0

5

10
15
20
25
Opening Angle θ (degrees)

30

35

j

(C) ESO

Figure 18:

Fong+14

Distributions of jet opening angles for short (blue) and long (red) GRBs, based on breaks in their afterglow

NS/
o the
989;
e and
have
and
first

ob
se
r

ve
d

Metzger & Berger

all s
ky

preetter
g on
make
with
Tranopes
arize

Cumula2ve redshi_ distribu2on of short GRBs

Mpc detection
800 Mpc
Figure 300
2. Cumulative
rate of SGRBs with measured redshifts < z(thick solid line), calculated using 19 (mostly Swift) SGRBs (e.g., Berger 2011).
Dashed vertical lines mark the estimated sensitivity rangeof ALIGO/Virgo
Metzger& Berger 2012
to NS–NS and NS–BH mergers, respectively, including a boost due to the920525..............................
921022..............................
931222..............................
951007..............................
961225..............................
990712..............................
000107..............................

0.500
0.077
0.023
0.461
0.197
0.902
0.397

1.025
1.333
1.172
1.475
2.001
2.617
1.677

0.061
0.036
0.097
0.084
0.072
0.033
0.236

0.748
0.773
1.070
0.421
1.140
0.906
1.298

0.097
0.012
0.019
0.079
0.043
0.041
0.277

Late-phase ac2vi2es?
a

b

0.730
0.580
0.913
0.285
0.570
0.346
0.774

0.104
0.018
0.077
0.056
0.030
0.016
0.198

Ratio of emission in the spike to the extended emission.
Ratio of the extended emission hardness ratio to the spike emission hardness ratio.

Signatures
enginesin SGRBs“Extended”
emissionof magnetar central“Plateau”
emissione bursts in the Lazzati et al. sample must be dimmer than theverage. At least 30 BATSE short bursts with Fp > 10 photons
m!2 s!1 show no individual evidence of extended emission,
hereas three of our sample have comparable peak fluxes (seeg. 3). The initial spike in GRB 931222 is "2 times more intensethan the peak in the extended emission. We conclude that the
dynamic range in the ratio of peak intensities, spike:extended, is"104.
The range in the ratio of total counts is also large. For our
BATSE sample, the dynamic range of the ratio, spike:extended,

104 105020
40
2me (s)60

Fig. 7.—Time profiles for the three bursts of Fig. 2 with the brightest and most fluent extended emission. The vertical axis truncates the initial spike to emphasize
tended emission. Dotted lines indicate intervals (same as in Fig. 2) analyzed for spectral evolution in x 2.2. Error bars to the right of the spikes represent #1 !
ctuations.

Norris & Bonnell 06

Rowlinson+13

X-ray emission to wider solid angle?
The Astrophysical Journal Letters, 809:L8 (5pp), 2015 August 10

The Astrophysical Journal Letters, 809:L8 (5pp), 2015 August 10
Kisaka, Ioka, & Nakamuraof the ejecta is described by⎛ v ⎞⎛ t ⎞⎟⎜⎟ cm.
r ~ 3 ´ 1013 ⎜⎝ 0.1 c ⎠ ⎝ 10 4 s ⎠(2 )On the other hand, the radius of the plateau emission region isestimated as
rplateau ~Figure 1. Schematic picture for the scattering of plateau emission and theengine-powered macronova. X-ray photons emitted from the inside of the jet(light blue region) are scattered by the optically thick ejecta (thick arrow). The
gray region is effectively thin, and the red region is effectively thick.

Kisaka+15

with the sensitivity of X-ray observations. In Section 3, we
present the model of a macronova powered by the plateau
activity, which explains the observations of GRB 130603B.
Finally, we present discussions in Section 4.

G2cDt ~ 3 ´⎛ G ⎞2 ⎛ Dt ⎞12⎟
10 ⎜ ⎟ ⎜⎝ 10 ⎠ ⎝ 1 s ⎠

cm,

(3 )

where Γ is the bulk Lorentz factor of the emitter and Dt is theﬂux variability timescale. Both Γ and Dt have some range foreach event, so that the emission continues overrplateau ~ 1011–1014 cm in an approximately logarithmic way.
Since the Lorentz factor is low, G ~ 10 , inside the jet due tothe cocoon conﬁnement (Nagakura et al. 2014) and thus therelativistic beaming angle is larger than the jet opening angle
1 G 2 qj, most emission from the jet can reach the boundary
between the jet and the ejecta as shown in Figure 1. In addition,
the range of rplateau covers the sweet spot for the scattering,
rplateau ~ r G ~ 3 ´ 1012 cm . Therefore, the observers with alarge viewing angle (2qj) with respect to the jet axis would
detect the scattered X-ray photons of the plateau emission.
We parameterize the scattered luminosity of the plateau
emission L rf using a parameter ò as

~ plateauL iso,pl , (the black dashed curve)(4 )Figure 2. Light curves ofL rfthe
and its scattered3
2. SCATTERED X-RAY EMISSION= 10
the red solid
curve).
Red ofcrosses
are the plateau emission
emissionswhere (L iso,plis the; observed
isotropic
luminosity
the plateau
130603B
thethedistancechangedemission.
We ﬁrst withconsiderisotropicallyscatteredfrom
compo-the original redshift
Figure 1 shows a schematic picture for the scattering of theof GRB
to 100
Mpc.
Observational
nent whoseenergyis comparable
to that data
beforearethe obtained
scattering. from the UK Swiftemission from the jet (the thick arrow). A signiﬁcant fraction ofz = 0.356
photons that are emitted with angle 2qj relative to the jet axisScienceThen,luminosityof the lines
scatteredis limits for the soft
DatatheCentre.
Blue dottedshow component
the sensitivity
2

-3

2

Mass ejec2on fromNS mergers- 2dal disrup2on- shock hea2ng

M ~ 10-3 - 10-2 Msunv ~ 0.1 - 0.2 c
Rosswog 99, 00, Ruﬀert & Janka 01
Hotokezaka+13, Bauswein+13

Hotokezaka+13

1

200 Mpc

150MHz, n=1.0cm-3Radioemission(a_erglow)
10

jet ( 0°)ass ejection
and radio signals from NS mergers
jet (45°)

10

10
10

10000

1.4GHz,nn=1.0cm
150 MHz,= 0.1-3-3cm-3150MHz,n=0.1cm

11[mJy]
FFνν [mJy]

1

1000

jet
jet (( 0°)
0°)
jet
(45°)
jet (45°)jetjet (90°)(90°)
dynamical
dynamical
breakout
breakout3jet (90°)
dynamical
breakout

100t [day]0.1

0.1 mJy
0.1
0.1

0.01

0.01
0.01

0.001

0.001
0.001

1

10

100
t [day]

1000

10000

11

10

Delayedby ~> years
jet ( 0°)jet (45°)
the diﬀerent componentsof the ejecta. Also marked are the deceleration
10
jet
(90°)
The star in each component shows the fiducial model. Right panel: adynamicalof the ejecta
on the meridional plane. The distribution of the dynamical
breakout). Other components are added schematically.
1

Depends on ISM density

10000

jet ( 0°)jet (45°)
jet (90°)
dynamical
breakout

10
10

11Fν [mJy]

cording to these numerical simulations, the mass and ki0.1netic energy of the dynamical ejecta are expected to be in
the range 10−4 ! Mej ! 10−2 M⊙ and 1049 ! E ! 1051 erg,
respectively. The median value of E in the general relativis50
0.01tic simulations is a few times 10 erg. The properties of the
dynamical ejecta are as follows.
The tidal ejecta. A fraction of the material obtains suﬃ& Piran
11 and is ejected via tidal interaction
cient angularmomentum0.001Nakar
1 to non-axisymmetry
10
100the gravitational
1000
10000
due
of
forces.
This
Hotokezaka
&
Piran
15
t [day]matter is ejected even before
the two stars collide with each

1000

-3 -3
1.4GHz,n=0.1cm
1.4 GHz,nn=0.01cm= 0.1 -3cm
150MHz,150MHz, n=0.1cm-3- Not immediate iden$ﬁca$on- Good for conﬁrma$on- Not aﬀected by visibility

100t [day]0.1 mJy
0.1
0.1

0.01
0.01

0.001
0.001

11

10

100
t [day]

1000

10000

Radio transient sky is “quiet”

The Astrophysical Journal, 818:105 (27pp), 2016 February 20

NSm

Mooley et al.

erg
erFigure 22. Top: the phase space of slow extragalactic transients. The panel shows the upper limits to the transient rates from previous radio surveys (colored wedges;
95% conﬁdence), the rates derived from radio transient detections (2σ error bars), and the expected transient rates. The transient detection labeled as “Le+02”
represents an SN II having a peak radio luminosity of 3×1027 erg s−1 Hz−1 and an evolution timescale of ∼15 yr (Levinson et al. 2002; Gal-Yam et al. 2006). The
one labeled “Ba+11” is a nuclear transient, SUMSS J060938–333508, with a peak radio luminosity of 6×1029 erg s−1 Hz−1 and an evolution timescale of <5 yr(Bannister et al. 2011a, 2011b, K. Bannister 2015, private communication). All observed quantities are color-coded according to the observing frequency. The solid
gray line is the rate claimed by Bower et al. (2007), plotted for reference. The upper limit to the extragalactic transient rate from our pilot survey (this work) and thephase space probed by the full CNSS survey are shown as thick green wedges. The phase space probed by the VLA Sky Survey all-sky tier (VLASS) is also shown.
The solid red line denotes the source counts from the FIRST survey, and the dashed red line denotes the approximate counts for strong variables at 1.4 GHz (1% of thepersistent sources). Bottom: the Galactic transient phase space. Symbols have similar meanings as in the top panel. Black solid lines denote the source counts from theMooley+2016

Low contamina2on rate
* Higher L(radio)/L(op2cal) than supernova

L(radio) <= v
L (op2cal) <= MElectromagne2c signature from compact binary merger(NS-NS or BH-NS)•

X-ray/gamma-ray

strophysical Journal, 746:48 (15pp), 2012 February 10

specific stellar populations). Because merger counterparts
redicted to be faint, obtaining a spectroscopic redshift
allenging (cf. Rowlinson et al. 2010), in which caseroscopy of the host galaxy is the most promising means
taining the event redshift.
s important to distinguish two general strategies for conng EM and GW events. One approach is to search for a
signal following an EM trigger, either in real time or at
t-processing stage (e.g., Finn et al. 1999; Mohanty et al.
). This is particularly promising for counterparts predicted
cur in temporal coincidence with the GW chirp, such as-duration gamma-ray bursts (SGRBs). Unfortunately, mostpromising counterparts (none of which have yet been
endently identified) occur hours to months after coales.6 Thus, the predicted arrival time of the GW signal willn uncertain, in which case the additional sensitivity gained
this information is significantly reduced. For instance, if
me of merger is known only to within an uncertainty ofurs (weeks), as we will show is the case for optical (radio)
erparts, then the number of trial GW templates that mustarched is larger by a factor ∼104 –106 than if the merger
is known to within seconds, as in the case of SGRBs.
second approach, which is the primary focus of this paper,
M follow-up of GW triggers. A potential advantage in thisis that counterpart searches are restricted to the nearby

Short GRB: strongly beamed
Late ac2vity: isotropic??

• Radio

Delayed by years
Low contamina2on rate

Metzger & Berger

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

Ejecta ISM ShockRadio (years)

GRB

obs

(t ~ 0.1 1 s)

Kilonova

Optical (t ~ 1 day)j

Merger Ejecta
Tidal Tail & Disk Windv ~ 0.1 0.3 c

BH• Op2cal/NIR

Delayed by only ~ 1 week
Isotropic

Figure 1. SummaryMetzgerof potential&electromagnetic
counterpartsof NS–NS/
Berger 2012,
ApJ 746,
48
NS–BH mergers discussed in this paper, as a function of the observer angle
θobs . Following the merger a centrifugally supported disk (blue) remains aroundthe central compact object (usually a BH). Rapid accretion lasting !1 s
powers a collimated relativistic jet, which produces a short-duration gammaElectromagne2c Emission from
Gravita2onal Wave Source• EM emission from compact binary mergers• Kilonova/macronova emission andthe origin of r-process elements

Mass ejec2on fromNS mergers- 2dal disrup2on- shock hea2ng

M ~ 10-3 - 10-2 Msunv ~ 0.1 - 0.2 c
Rosswog 99, 00, Ruﬀert & Janka 01
Hotokezaka+13, Bauswein+13

Hotokezaka+13

abun

10

10
r-process nucleosynthesis
in NS mergers
10-7=> solar abundances-6higher T
higher Ye

νe + n -> p + en + e+ -> νe + p
ν

-8

10
(e.g., Wanajo+14, Just+15, Wu+16)

0

50

10-2

100
150
mass number

200

250

solar r-abundancemass-averaged

10-3
-4

abundance

10

10-5
-6

10

-7

10

-8

10

0

50

100
150
mass number

200

250

ら れ る． こ の 加 −熱はr-process nucleosynthesis in core-collapse
supernovae
νe＋
n→p＋e
ニュートリノ（νe）捕獲

Wanajo, Janka, & Mül5Ye, min = 0.466

The Astrophysical Journal Letters, 726:L15 (4pp), 2011 January 10

1D 2D

および陽子（p）の反電−νe＋n→p＋e
Ye, min = 0.404

mass [10-3 solar]

4
3
2

＋

ν̄ e＋p→n＋e
および陽子（p）の反電
1

0
0.40

0.45

Ye

0.50

0.55

Figure 2. Ejecta masses vs. Ye for the 1D (blue) and 2D (red) explosion mod
The width of a Ye -bin is chosen to be ∆Ye = 0.005. The minimum values oare indicated for both cases.
(A color version of this figure is available in the online journal.)

expands continuously, and a neutrino-powered explosion sets in
at t ∼ 100 ms p.b. in 1D and 2D essentially in the same way
and with a very similar energy (∼1050 erg; Janka et al. 2008).
In the multi-dimensional case, however, the negative entropyn relative to solarによるものである．超＋ν̄ e＋p→n＋e
Diﬃcult to produce
r-process elements
により，この二つの反in (normal) core-collapse supernovae

Figure 1. Snapshot of the convective region of the 2D simulation of an ECSN
at
262 ms after coreWanajo
bounce with
Wanajo+11,
14entropy per nucleon (s; left) and Ye (right).
Mushroom-shaped lumps of low-Ye matter are ejected during the early phase of
the explosion.
(A color version of this figure is available in the online journal.)

104
3

10

102
101
0

Ca

Cr
Ni
Ge
Kr
Zr
Ti
Fe
Zn
Se
Sr
Mo
1D 2D

NS merger as a possible origin of r-process elements

Event rate
RNSM

~ 103 Gpc-3 yr-1

Ejec2on per event
Mej(r-process) ~ 10-2 Msun

~ 30 GW events yr-1
(w/ Adv. detectors, < 200 Mpc)

GW

LIGO O1RNSM < 104 Gpc-3 yr-1

EM

Enough to explain the r-process abundance in our Galaxy
M(Galaxy, r-process) ~ Mej(r) x (RNSM x tG)~ 10-2 x 10-4 x 1010 ~ 104 Msun

Table 2. Sensitive space-time volume hV T i and 90% confidence upper limit R90% for NS
Constraints
onThe
the
mergerrate
spin distributions.
NSNS-NS
spin magnitudes
are inthe range [0, 0.04] and the BH spin ma
are shown for both the pycbc and gstlal pipelines. hV T i is calculated using a FAR
Expected
limit is calculated using a uniform prior on L
= RhV T ievent
and anrates
18% uncertainty in hV T i f

BH-BH

O3

Dominik et al. pop syn

O2

O1

O1: 2015-2016
O2: 2016-2017

de Mink & Belczynski pop syn

O3: 2018

Vangioni et al. r-process
Jin et al. kilonova
Petrillo et al. GRB
Coward et al. GRB
Siellez et al. GRB
Fong et al. GRB
Kim et al. pulsar
aLIGO 2010 rate compendium
100

101

102

103

104

BNS Rate (Gpc 3yr 1)

arXiv:1607.07456
Figure 6.
A comparison of the O1 90% upper limit on the

Figure 7.

A comparis(C) NASAHea2ng by radioac2ve
decayof
r-processnucleiTransients from compact object mergers

NS
m

2653

erg
ve heating ofer 1 hr 1 day 10 daysrtı́nez-Pinedo
aptures, phons.
latters-1
43 erg10The
β delayed fistes for nuclei& Thielemann
1040 erg s-1
models: the995) and theth Strutinsky
y 1996). For
tron-induced
β-decay rates
Metzger+10
Figure 1. Radioactive heating rate per unit mass Ė in NS merger
ejecta(for= 0.01 Μsun)
cay
areM
from

“kilonova/macronova”

Li & Paczynski 98, Metzger+10,
MT & Hotokezaka 13, MT+14,
Kasen+13, Barnes & Kasen 13◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆◆
研究奨励賞

いるため，放出物質

Type Ia SN
NS merger

射性不安定な原子核プロセスですので，核の放射性エネル
L ~ 1040-41 erg/sに光るはずです．こ@ ~1 weekの放射性崩壊で電ます．

Luminosity (erg/s)

応（r-process）が進

de
cay
e

ne
rg

y

Mej = 0.01 Msun

イデア自体は 1999ですが 15），詳細なになっていませんでDays a_er the merger

Magnitude=3m=

2.5 log(F/F0 ) + m0

Absolute magnitude
brightness if the object is located at 10 pc
The sun: Observed magnitude = -27 mag
Absolute magnitude = +4.8 mag

Days after the merger

Type Ia SN

18-18
Type Ia SN
NS-NS
BH-NS
Wind

20

Disk wind(lower opacity)

22

24

BH-NS
(higher T)

NS-NS

26

1m
-16

4m
8m

-14

-12

Absolute magnitude

Observed magnitude (200 Mpc)

i-band,i-band Mej = 0.01 Msun

-20

Observed magnitude (200 Mpc)

16

-10

28
0

5

10
15
Days after the merger

Talks by Yoshida-san and Tominaga-san20
MT 2016

FIG. 2: Expected observed magnitudes of kilonova models at 200

Constraints from short GRBs
SN 1998bw

kilonova

GRB(C) ESO

Constraints from short GRBs (1/3)

Time since GRB 130603B (d)of the afterglow21 and the host galaxy22 were
1
10
356.
10–11
nature of the merger of two neutron stars or a
X-ray
21
k hole is the production of a kilonova (someF606W
acronova’ or an ‘r-process supernova’) due to
22
F160W
species produced and initially ejected duringother words, an event similar to a faint, short23
ailed calculations suggest that the spectra of
10–12
will be determined by the heavy r-process ions24
rich material. Although these models10–13 arerealistic, a robust conclusion is that the optical
25
nished by line blanketing in the rapidly expandiation emerging instead in the near-infrared
10–13
ced over a longer timescale than would other26
akes previous limits on early optical kilonova
source. Specifically,NIR
the NIR
light curves are expected27
ing after a few days and lasting a week or morelatively modest redshift and intensive study of
28
10–14
rime candidate for searching for such a kilonova.
ation of the burst with the NASA/ESA Hubble
29
at two epochs, the first ,9 d after the burst
Tanvir+2013,
Berger+2013
105
106
104
d ,30
d after the burst(epoch 2). On each occaTime since GRB 130603B (s)ration was obtained in both the optical F606W
R F160W filter (1.6 mm) (full details of the imag- Figure 2 | Optical, NIR and X-ray light curves of GRB 130603B. Left axis,
Possiblealso
inalysisdiscussed detec2ons
here are given in
Supplemenoptical and NIR; right axis, X-ray. Upper limits are 2s and error bars are 1s. The
optical data (g, r and i bands) have been interpolated to the F606W band and
HSTGRB
images060614
are shown(z=0.125)
in Fig. 1; theYang+15,
key result isJin+15
ames (right-hand panels), which provide clear the NIR data have been interpolated to the F160W band using an average
GRBsource
050709Jin+16
ransient
in the(z=0.16)
NIR in epoch
1 (we note spectral energy distribution at ,0.6 d (Supplementary Information). HST

GRB 130603B

AB magnitude

X-ray flux (erg s–1 cm–2)=> ejec2on of M ~0.02 Msun

24

epoch-1 points are given by bold symbols. The optical afterglow decays steeply

S HORT GRB 1501

Constraints from short GRBs (2/3)
81024 mag

10
10

42

41

40

r-bandTanaka+ 2014 (NS-NS)

22

Tanaka+ 2014 (NS-BH)

23

Kasen+ 201524

200 Mpc shallow
25
deep

26
27

30

0

10

22
23
24
25
26

10

10

27

30 10010110Time after Burst (days)

38
-1

J

10

29

29

39

21

28 10

28

10

10

Barnes & Kasen 201320

Near-IR Luminosity λLλ (erg s-1)

10

21

43

10

AB magnitude

21 mag10

20

AB magnitude@ 200 Mpc

Optical Luminosity λLλ (erg s-1)

10

GRB 150101B
Previous sGRBs

44

0

10
10
Rest-frame Time after Burst (days)

1

10

Figure 4. Optical r-band and near-IR JHK-ban
Figure 7. Constraints onkilonova
emissionfor
GRB 150101B
and allprevious
short GR
are
four
sets
of
kilonova
modelsingrey
regions(left) and near-IR J-band (right) emission. Triangles denote 3 limits, Fong+16
from this work
(crossed)and NS-BH
Hotodenote limits
061201
at a tentative
redshift ofmergers
z = 0.111, (speckled;
and at the mediansh
Mfor~<GRB
0.3
Msun

kilonova following GRB 130603B (black asterisk; Berger et al. 2013a; Tanvir et al. 201

Constraints from short GRBs (3/3)
GRB 160821B (z=0.16)

z = 0.162(Levan+16)

Pan-STARRS1 (r-band)

F606W ~ 25.8 mag @ z=0.16=> Mabs -14 mag=> ~22 mag @ 200 Mpc

M ~ 0.01 Msun

Re-processed emission of extended/plateau emission

gust 10its scatteredeau emission

Kisaka, Ioka, & Nakamura

Kisaka+15

Figure 3. Theoretical light curves of engine-powered macronovae at the nearinfrared (F160W, red) and optical bands (F606W, blue). We consider threemodels of the energy sources, plateau emission with qj = 4 (solid line),==> Need detailed follow-up of GW sourcesEM emission from GW sources• X-ray/gamma-ray• Short GRBs: promising, but strongly beamed• Central engine ac2vity (isotropic??)• Radio• A_erglow: delayed by ~ years• Good for conﬁrma2on and low contamina2on rate
• Op2cal/infrared• r-process nucleosynthesis => kilonova/macronova• Probably detected in short GRB observa2ons• GW + EM => r-process produc2on rate
Mul2-messenger astronomy ==> Origin of r-process elements