Optical Time Domain andMulti-Messenger Astronomy

Tomoki Morokuma(University of Tokyo)

Contents(Extragalactic) Transients in Optical
Transient Surveys in Optical
Multi-Messenger Astronomy in Optical
Gravitational Wave
High-Energy Neutrinos
Collaborative Observations in optical & VLBI
Summary

EAVW-2019@Ibaraki University

2019/09/24-26

Optical Time Domain and Multi-Messenger Astronomy

2

−24

45

Luminous Supernovae
SCP06F6
SN2005ap SN2008es PTF09cnd
SN2006gy
PTF09cwl PTF09atu
PTF10cwr

factor of 100

−22

44

10

SN2007bi

Thermonuclear
Supernovae

43

10SN2002bj−1−18

Peak Luminosity [erg s ]−20Peak Luminosity [MV]10Core−Collapse
Supernovae

PTF10bhp.Ia Explosions−16

PTF11bij
PTF09dav
PTF10iuv
SN2005E42

10SN2008ha−14Ca−richTransients

41

10

SN2008S
PTF10acbp
NGC300OT−12
PTF10fqs
P60−M82OT−081119

−10

40

10

M85 OTV838 MonClassical Novae−8

LuminousRed
Novae

M31 RV

39

10

P60−M81OT−071213
38

−6

10
0

1

10

Kasliwal 2011

EAVW-2019@Ibaraki University

10

2

10

Characteristic Timescale [day]2019/09/24-26

Optical Time Domain and Multi-Messenger Astronomy

3

−6

0

10

1 local Universe
Transientsin10
theTransientsin thelocal
Universe
Transients
in
the
local
Universe
Transientsin the local Universe log
383
Transientsin
the
local
Universe( Characteristic Timescale [day][sec]) 383

10383383383 3832

10TransientsinthelocalUniverse

PTF10bhp
Core−Collapse
PTF10bhp
Core−Collapse
PTF10bhp
PTF10bhp
PTF10bhp
Core−Collapse
Core−Collapse
Core−Collapse
SupernovaeCore−Collapse 421042
PTF11bij*+Supernovae&
PTF11bij"42
42 Supernovae.Ia Explosions
42 10 42Supernovae
Supernovae
PTF11bij
PTF11bij "(Supernovae
PTF11bij
PTF11bij
PTF09dav.Ia
Explosions

10
10
10
10
.Ia
Explosions.Ia
Explosions&
PTF09dav−16−16.Ia Explosions PTF09dav .Ia Explosions)

PTF09dav
PTF09dav
PTF09dav−16−16

PTF10iuv,&%(
PTF10iuv
PTF10iuvv
SN2005E .' PTF10iuv)+'PTF10iuv PTF10iuSN2005E
SN2005E &##')
SN2005E SN2005E
SN2005E
PTF10bhp

Peak Luminosity [erg s−1]

Peak Luminosity [erg s−1]

−1

Peak Luminosity [erg s ]Peak Luminosity [erg s−1]

−18

Peak Luminosity [erg s−1]]
Peak Luminosity [MPeak Luminosity [erg s−1]

Peak Luminosity [M

−18

V

]

V

V

]

Peak Luminosity [M ]V
Peak Luminosity [M ]
V

−18
−18
Peak Luminosity [MV

Peak Luminosity [M ]1""""""""""""""""""""""""""2""""""""""""""""""""""""""3""""""""""""""""""""""""""4"""""""""""""""""""""""""5"""""""""""""""""""""""""6""""""""""""""""""""""""7"454510−24−2410 45 1),Figure2011).
Notethat until 2005
45 in the Year 2011 (Kasliwal
45
45 (Fig.
−24 4. Framework of Cosmic Explosions
−24
−24
−24
LuminousSupernovae
LuminousSupernovae
10
10
10
10
LuminousSupernovae
LuminousSupernovae
LuminousSupernovae
LuminousSupernovae
SCP06F6
SCP06F6
we only knew about three classes(denoted by gray bands).
In thepast six years, systematic
searches,
SCP06F6
SCP06F6SCP06F6 SN2005ap SN2008es
SCP06F6
SN2008es
PTF09cnd
SN2005ap
PTF09cnd
SN2008es PTF09cndsearches have uncovered
SN2008es
SN2008es
serendipitous
discoveries
andarchivala plethoraof novel,raretransients.
DiscovSN2005ap
SN2005ap
SN2005ap SN2008es PTF09cnd
SN2005ap)*!&+()*)
−22−22
PTF09cndSN2006gy
PTF09cnd
SN2006gy−22−22−22 PTF10cwrPTF09cwl−22
PTF09atu
44
SN2006gy
SN2006gy
SN2006gy
SN2006gy
PTF09cwl
PTF09atu
4410
eries by the Palomar Transient
FactoryandP60-FasTING(Kasliwal
etal.
2011a)
aredenotedby?.
Several
PTF10cwr
PTF09atu
PTF09atu
PTF09atu
PTF09atu
44
44
44 10 44
PTF09cwl
PTF09cwl
PTF09cwl
PTF10cwr PTF09cwl
PTF10cwr
PTF10cwr 10
PTF10cwr
101010
$$(.
SN2007bi
new classes are emerging and the governing physics is being widely debated: luminous
red
novae
(electron
SN2007bi
SN2007bi
SN2007bi
SN2007bi
SN2007bi−20+()*)
−20(*!&collapse of rapidly −20rotating O–Ne–Mg white−20 induced−20−20
capturedwarfs?),luminous
supernovae(magnetars
Thermonuclear%
Thermonuclear!%+ThermonuclearThermonuclear
Thermonuclear
Thermonuclear
43
Supernovae
4310
Supernovae
&explosions?),or pair instability.Ia
explosions(heliumdetonations
inultra-compact
white
dwarf
binaries),


43
43
43
43
Supernovae
Supernovae
Supernovae
SupernovaeSN2002bj
10##') SN2002bj101010
10SN2002bj
SN2002bj
SN2002bj
SN2002bj

Calcium-richhalotransients(helium
deflagrations?).
−18−18

&*$$(.('*()

(advanced
LIGO, advanced VIRGO, LCGT, INDIGO) coming online. Detecting gravitational−16−16
waves from neutron&star
every month is expected to become routine. A basic common(mergers
.'
SN2008ha
ality between
wave searches and SN2008ha
the electromagnetic
search describedabove is that
SN2008ha
41−14 gravitational
SN2008ha
SN2008ha
SN2008ha
4110
−14
41
41
41
41
−14 ) &"
−14
−14
−14
SN2008S
10Ca−rich% Ca−rich
SN2008S
10(say, < 200
10PTF10acbp
10 poor10sky
SN2008S
SN2008Sknown
SN2008S
both are limited to the
Universe
Mpc). A
challenge
will be SN2008S
theCa−richCa−richlocal
Ca−richCa−richPTF10acbp
!#&%&,
PTF10acbp
PTF10acbpPTF10acbp
PTF10acbp
Transients("&+*
Transients%&,
Transients
Transients rate
Transients
localizationsof the Transients
gravitational wave signal
andconsequent large false
positiveof electroNGC300OT
NGC300OT
NGC300OT
NGC300OT
NGC300OT
NGC300OT−12magnetic(Kulkarni &−12Kasliwal 2009). Therefore,priorsearch for an−12 −12candidates−12−12*) to the ambitious)(
40+
Luminous*
4010
Luminous
40 PTF10fqs
40
40
Luminous 1040
Luminous
Luminous+
Luminous&
PTF10fqs
PTF10fqs
PTF10fqs
PTF10fqs

PTF10fqs.
10 10this10 only be prudent
10 buildelectromagnetic counterpart to aRedgravitational wave
itRedwould
Red to(signal,
Red

Red
Red

)
Novae Novae&+Universe.
Novae
Novae
Novae
Novae
%
!
P60−M82OT−081119
complete inventoryoftransients
in
the
local
$
P60−M82OT−081119
P60−M82OT−081119
P60−M82OT−081119
P60−M82OT−081119
M85 OT−10 P60−M82OT−081119
#+
M85 OT(
#*−10V838
Mon−10 −10
−10

−8−8

−6−6

Classical Novae−8 −8V838 Mon39

M31 RV 10

P60−M81OT−071213
P60−M81OT−071213
P60−M81OT−071213
P60−M81OT−071213

−6
0
0 −60
10 10 100 10-4−10 M85 OT−8Classical
Novae 39Classical
Novae Novae
Classical
Novae
Classical
M31 RV 10−8

P60−M81OT−071213

1

10
-3

02

10
-2

39
39
3910
M31
10
M31 RV 10
M31 10
RV RV

38

10

1

10

1

1

10 1 10
-1
10

−6

39

Classical
Novae
M31 RVP60−M81OT−071213

#()*()
38−6

M85 OT M85 OT
M85 OTV838 Mon
V838 Mon
V838V838
Mon Mon

38

10
02

100

1

101

2

10

Characteristic[day]
Characteristic Timescale [day]log
Characteri
sticTimescale
TimescalTimescalee [day] [day][day]Characteristic
Timescale(Characteristic) Characteristic Timescale [day]

38 38
3810

10 10
2
2 10 2102
10
10Kasliwal 2011,
Cooke/www.astro.caltech.edu/~ycao/B&ETalks/B&E_FRBs_Cooke.pdf)
Figure4.(http:/
FrameworkofExplosions
CosmicExplosions
in Yearthe Year2011(Kasliwal
2011).
2005
Figure4.
FrameworkofCosmicExplosionsintheYear2011(Kasliwal2011).
Notethatuntil2005(Fig.1),
Figure4.
FrameworkofCosmicExplosionsintheYear2011(Kasliwal2011).
Notethatuntil2005(Fig.1),
Figure4.
FrameworkofCosmicExplosionsintheYear2011(Kasliwal2011).
Notethatuntil2005(Fig.1),
Figure4.
Frameworkof Cosmic
in theinYear
2011(Kasliwal
2011).
Note
thatNote
until
2005
(Fig.
1), (Fig.
Figure4. Frameworkof Cosmic
Explosions
the2011(Kasliwal
2011).
Note
thatthat
untiluntil
2005
(Fig.
1), 1),
only
knew
about
three
(denoted
by
gray
In
past
six
years,
searches,
we onlywe
knew
aboutknew
threeclasses(denotedby graythreebands).
In theclasses
past(denoted
sixclasses
years,
we onlysystematic
knew about
searches,
three classes
by gray
bands).
Inbands).
the pastthe
sixIn
years,
weDomain
onlythesystematic
knew theabout
searches,
threeandclassesby gray
bands).
In thesystematic
past searches,
six years, systematic
searches,
we only
knew
about
three
classesbygraybands).
In
past
six
years,
systematic
EAVW-2019@Ibaraki
University
2019/09/24-26
OpticalTime
Multi-Messenger
Astronomy
we
only
about
(denotedby(denotedgraybands).
pastsix(denoted
years,
systematic
searches,4

Optical Transient Surveys
wide

Yasuda+2019
all-sky

Kiso/Tomo-e Gozen

{

{

~2m

< 1m

{

~8m, HST{~4m□ high cadence (< 1 day)

EAVW-2019@Ibaraki University

1 uJy

shallow

100 uJy

narrow

2019/09/24-26

deep
Optical Time Domain and Multi-Messenger Astronomy

5Optical Transient Surveys~2m□ high cadence (< 1 day)narrow
shallow
EAVW-2019@Ibaraki University

SN Ia@z~1, CCSN@z~0.5

~4m

{

< 1m

CCSN@100 Mpc{

AT2017gfo (GW170817)

Kiso/Tomo-e Gozen{

TXS 0506+056 (IceCube-170922A)

all-sky{↑SN 2011fe (Ia)@M101 (7 Mpc)

wide

Yasuda+2019~8m, HST

deep
2019/09/24-26

Optical Time Domain and Multi-Messenger Astronomy

6

Kiso Schmidt telescope (1.05m)
KWFC (8 CCDs, 2012-)==> Tomo-e Gozen (巴御前; 84 CMOS, Sako+2016)
completed in April, 2019wide field-of-view (20 deg2), fast readout (>2Hz)
high-cadence supernova survey==> “all-sky” (~7,000 deg2) & high-cadence (~2 hrs)
Start the survey from this October !!!!
second scale transient search (Richmond, TM, submitted)

EAVW-2019@Ibaraki University

2019/09/24-26

蔀関月作, 「巴御前出陣図」,
東京国立博物館,©Image: TNM Image Archives

Optical Time Domain and Multi-Messenger Astronomy

7

Rapidly Evolving Transientsprogenitor stars of core-collapse supernovae

he Astrophysical Journal, 819:5 (15pp), 2016 March 1

Tanaka et al.

20 minutes

1 day

SN 2016gkg@NGC 613

gure 3. Light curves of the ﬁve rapidly rising transients on Days 1 and 2. The g- and r-band photometry is shown by the blue and red points, respectively. Triangles
ow the 3σ upper limit. For the g-band data, photometry for one visit (5×2 minute exposures) is shown in pale blue while photometry in the one-night stacked data
shown in blue.

~10^-3 Msun/yr
mass loss

he [O II] λ3727 emission line is detected from all the hostalaxies, which indicates that they are all star-forming galaxies.
he redshifts range from z = 0.384 (SHOOT14jr) to z = 0.821
SHOOT14or).
3. LIGHT CURVES
3.1. Overview

Figure 3 shows light curves of our samples on Day 1 anday 2. Hereafter, the epochs of stacked g-band data on Day
are taken to be t=0 unless otherwise mentioned. The
hotometry is performed in the subtracted images using thenal references (e.g., Day 1 – Day 327 and Day 2 – Day 327
or the g-band).
Throughout the paper, we do not take into account full Korrection for absolute magnitudes since only limited informaon about the spectral energy distribution is available for our
amples. Instead, we correct only the effect of redshifts, i.e.,
M = m - m + 2.5 log (1 + z ), where M and m are absolutend observed AB magnitudes (measured as fν) and μ is the
stance modulus. The last term originates from the difference
the frequency
bins in the restframe andUniversity
observer frame, i.e.,
EAVW-2019@Ibaraki(n ) = [(4pd 2 ) (1 + z )] f (n ), where ν and ν are rest-

Tanaka,Tominaga,
TM+2016w/ Subaru/HSC

at wavelengths shorter than the wavelengths corresponding
to the observed r-band. Therefore the blackbody temperatures
for our objects are TBB13,000, 15,000, 13,000, 11,000,
and 13,000 K for SHOOT14gp, 14or, 14 ha, 14jr, and 14ef,
respectively. Note that the intrinsic colors can be bluer due tothe extinction in the host galaxies.
SHOOT14or and 14jr are detected in the images ofDay 1 – Day 327. We measure the rates of rise fromDay 1 to Day 2 using the g-band one-day stacked images:
−1
+1.11
+0.39
∣Dm Dt∣=3.12for SHOOT14or0.70 and 1.61-0.32 mag day
and 14jr, respectively (errors represent 1σ, Table 3). Note thatthe rate of rise is measured in the restframe, so the time interval
used for the measurement varies with the source redshift(Δt=0.55 days for SHOOT14or while Δt=0.72 days for
SHOOT14jr). The other three objects (SHOOT14gp, 14 ha, and14ef) are not detected in the subtracted images of Day 1 – Day
327. The 3σ lower limits of the rate of rise measured in theg-band are ∣Dm Dt∣>3.10, 1.21, and 1.17 mag day−1. These
are also high enough to match our criterion for rapidly risingtransients.
In the following sections, we compare the light curves of oursamples with those of previously known SNe and transients.

2019/09/24-26

NatureOptical Time Domain andBersten+2018,
Multi-Messenger Astronomy

9Multi-Messenger Astronomy
in Optical

1. Gravitational Wave (LIGOx2, Virgo, KAGRA)
2. High-Energy Neutrino (IceCube)

EAVW-2019@Ibaraki University

2019/09/24-26

Optical Time Domain and Multi-Messenger Astronomy

10Gravitational Wave detections w/ LIGOx2, Virgo (O1, O2)

10 BH-BH mergers
1 NS-NS merger

https://www.ligo.org/detections/O1O2catalog.php
EAVW-2019@Ibaraki University

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Optical Time Domain and Multi-Messenger Astronomy

11

Observing Run 3 (O3)https://gracedb.ligo.org/superevents/public/O3/

31 detection candidates(some retracted)
no EM counterpart identified

better GW sensitivity ==> larger telescopes
EAVW-2019@Ibaraki University

2019/09/24-26

now

Optical Time Domain and Multi-Messenger Astronomy

12First Kilonova: Gravitational Wave Source incl. NSs
Fermi(gamma)GW
Publications of the Astronomical Society of Japan (2017), Vol. 00, No. 0

5

red color/spectrum due to broad absorption.
very different from supernova spectra
lanthanoid elements
high-speed ejecta (~0.1-0.3c)
different from expectations….
bluer in early phase.
brighterneed more samples
different viewing angles, rate, yield, etc.
EAVW-2019@Ibaraki University

Before GW170817, very limited observational constraints
2019/09/24-26
Time Domain
Multi-Messenger
on kilonova Opticalproperties(shortandGRB
afterglow) Astronomy 13

wide-field surveys for IceCube EM counterparts

http://icecube.wisc.edu
High Energy neutrino detector
isotropic ==> extragalactic?
~1 deg localization
no correlation
w/ TeV gamma sources or GRBs
54 events (1347 days, 2010-2014)
automatic alert since 2016/04==> electromagnetic follow-up
New alert system: GOLD & BRONZE(2019/07-)
EAVW-2019@Ibaraki University

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Optical Time Domain and Multi-Messenger Astronomy

14

Origin of high-energy (TeV-PeV) neutrinos (cosmic ray)transient (variable)~<27% (Fermi)(Aartsen+2017)©U. Tokyo©NASA/Fermi?
(peculiar) supernova
TDE w/ jet<5-10%(Senno+2017)©Science

EAVW-2019@Ibaraki University©NSF

blazar: AGN relativistic jet©NASA<1% (Aartsen+2017)2019/09/24-26~<30%@100 TeV(Bechtol+2017)

GRB starburst galaxy

Optical Time Domain and Multi-Messenger Astronomy

15

Neutrino from Choked-Jet Supernova
Type Ic broad-line supernova(GRB, Type Ic broad-line)

Senno+2017

Neutrino from interaction between SN ejecta & CSM

Type IIn supernova

Murase+2014
EAVW-2019@Ibaraki University

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Optical Time Domain and Multi-Messenger Astronomy

16

wnloaded from http://science.sciencemag.org/ on July 13, 2018

bin was ð5:3 T 0:6Þ $ 10 cm s , measured isource,appearingin threecatalogs of Fermi
as signalness
discussedincompanion
paper(26). analysis ofand mayerties Althoughthat hintatmosphericat contributions
extra- trinos
in so-calledaare
flaringstateatatenergies
thetimewith 100
enhancedarth’satmosphere.
neu- fromprobability,
theofatheevent
completerelevantprior
to Although
dominant
below
TeV,(14), was reported
to databe 56.5%(17).
31 October 2017. Although no additional excess
sources
(23,
24,
29)
at
energies
above
0.1,
50,
and
the
week 4 to 11 July 2017. Strong flux variationin. Highgalacticatsources,
although
the TeV,
individual
sources
g-ray
activity
insteeplythe(17).
GeV
range. Follow-up
ob- IceCube
rinos
are dominantenergies
below 100
(14),
was theirreported
to befalls
56.5%
Although
31 October
2017. Although
no additional
excessspectrumwithallowing
can robustly
identify astrophysicalneuof neutrinos was found from the direction of TXS
High-energy
g-rayenergy,
observations
of
10
GeV,
respectively.
Anexamination
of
the
were
observed during the g-ray flare, the most prom
heir spectrumremain
falls steeplywithenergy, allowing
IceCuberobustly
identify
astrophysicalneuof
neutrinos
was foundthe directionof TXS neutrinos
produced
as yetunidentified.
Continuously
mon-canservations
by imaging
Cherenkov
astrophysicalneutrinos
to atmospheric
be moreeasilyidentitrinos
at PeVfrom
energies,
for individual
0506+056 near the time of the alert, there are
TXS
0506+056
Fermi
Variability(FAVA) (30)inent being a flux increase from ð7:9 T 2:9Þ$to bemoreskyeasilytrinosneuat PeV
energies,forindividual
0506+056
near
the timeof All-Sky
theTeV,
alert,
areAnalysiso,strophysical
optical, neutrinos
itoring theentireforidentiastrophysicalnotably
theneutrinos
Major Atmosphericfiedtelescopes,
at higher
energies.
Themuon-neutrinoas-Largeat
severalhundredanthereatmosphericoriginindications
8 the% 3s
1photometric
light
curve
for
this
objectshowedcm 2 s%level
in ofthehigh-energy
week 8 to neutrino
15 August 201
10%at
On
28
September
2017,
the
Fermi
Area
ed at higher energies. The muon-neutrino asat several hundred TeV,Gammaan atmosphericoriginindications at the 3s level of high-energy neutrino
Imaging Cherenkov(MAGIC)%7
that TXS 0506+056 had brightened considerto ð4:0 T 0:5Þ $ 10 cm% 2 s% 1 in the week 15 t
Telescope (LAT) Collaboration reported that thetelescopes, revealed periods whereably in the GeV band starting in April 2017 (16).
22 August 2017.
direction of origin of IceCube-170922A was conFig. 1. Event display
for g-ray flux from the blazar
the detected
Independently, a g-ray flare was also found by
The Astro-Rivelatore Gamma a Immagini Leg
sistent with a known g-ray source in a state ofig. 1. Event display forneutrino event
IceCubereachedenergiesup(16).
to 400
GeV. Mea-is a pairFermi’s
Automated
Science
Processing[ASP(25)].
gero(AGILE) g-ray telescope (31) confirmed thenhancedemission
Fermi-LAT
eutrino event IceCube170922A. Thesurements
time at whicha source have alsoof theSuchflaringisnotunusual
for
a
BL
Lac
objectandelevatedlevel of g-ray emission at energies abovconversion
telescopeaboardthe
Fermi
Gamma70922A. The time at which a
DOM observedasignalisbeencompletedatx-ray,
optical,andwould not have been followed up as extensively if
0.1 GeV from TXS 0506+056 in a 13-day window
ray Space Telescope sensitive to g-rays with energies
OM observed a signal isreflected in thecolorof thehit,
radio
wavelengths.
We
have
investheneutrino
were
notdetected.
(10 to 23 September 2017). The AGILE measure
from
20
MeV
to
greater
than
300
GeV
(27).
Since
eflected in the color of the hit,with dark blues
for earliest
hitstigatedmodelsassociating
neutrino
Figure3shows
theFermi-LAT
light
curve
and
flux ofð5:3 T 2:1Þ $ 10% 7 cm% 2 s% 1 is consistent wit
August2008,
ithas
operated
continuously,
priwith dark blues for earliest hits
and yellow forlatest.
and
g-ray
and
find Itsthatthe detection time of the neutrino alert. The lightthe Fermi-LAT observations in this time period
marilyinTimes
anproduction
all-sky survey
mode.
wide fieldnd yellow for latest. Times
shown are relative
to
the
first
correlationoftheneutrino
with
the
curve
of
TXS
0506+056
fromAugust2008
toHigh-energy g-ray observations are shown i
of
view
of
~2.4
steradian
providescoverageofthehown are relative to the first
DOM hit according
toTXS
the
track
October2017
wascalculated
in
bins
of
28
days
for
Figs.
3 and 4. Details on the Fermi-LAT and AGIL
entire
g-ray
sky
every
3
hours.
The
searchforposflareof
0506+056
isstatisticallyOM hit according to the trackreconstruction,
andearlierandtheenergy
range
above
0.1
GeV.
An
additional
analysescan be found in (25).
siblecounterparts
to
IceCube-170922A
was
part
of
significant at the level of 3 standard
econstruction, and earlier andlater times are
shown
with
the On the basis
light curve with 7-day bins was calculated for thetheFermi-LAT
collaboration’sroutinemultiwavedeviations(sigma).
of theater times are shown with the
Very-high-energy g-ray observations ofsame colors length,
as
the
first
and
period around the time of the neutrino alert. The
multimessenger
program.
redshift of TXS 0506+056, we derive
ame colors as the first and
TXS 0506+056
last times, respectively.
g-ray flux of TXS 0506+056 in each time bin was
Inside theTheerror
regionof the neutrino event,constraints
for themuon-neutrino
ast times, respectively. The
determined through a simultaneous fit of thisFollowing the announcement of IceCube-170922A
aluminosity
positional
was andfoundwith a pretotal time theevent tookcoincidence
to this sourceforfindotal time the event took tosource
and
the
other
Fermi-LAT
sourcesina
TXS 0506+056 was observed by several groundviouslycataloged
g-raysource,
0.1°
from
the
bestcross the detector
is
~3000
ns.
them to be similar to the luminosity
ross the detector is ~3000 ns.
10°
by
10°
regionofinterest
along
with
the
based Imaging Atmospheric Cherenkov Tele
fitting
neutrino
direction.
TXS
0506+056
isa
The size of a coloredisobservedspherein g-rays.
he size of a colored sphere is
Galactic and isotropic diffuse backgrounds, using
scopes (IACTs). A total of 1.3 hours of observation
BL Lacertae (BL Lac) type. Its redshift ofproportional blazar
to theoflogarithm
roportional to the logarithmamaximum-likelihood
technique(25).
The
intein the direction of the blazar TXS 0506+05
z¼
0:3365T0:0010
wasmeasured
only
recentlyof the amountCONCLUSION:of light
The energies of the
f the amount of light
grated
g-ray
flux
of
TXS
0506+056
for
E
>
0.1
GeV,
were taken using the High-Energy Stereoscopi
based
on
the
opticalemission
spectruminaobserved at theDOM,
g-raysandwiththe neutrino indicate thatbserved at the DOM, withaveraged over all Fermi-LAT observations spanSystem (H.E.S.S.) (32), located in Namibia, o
study
triggeredthe observationof IceCubelarger spheres
corresponding
blazarjets mayby
acceleratecosmic rays
arger spheres corresponding
%8
%2 %1
cm
s
.
The
ning
9.5
years,
is
ð7:6
T
0:2Þ
$
10
23 September 2017 [Modified Julian Date (MJD
170922A(28).
to larger signals.
total
to atThe
least
several PeV. The observedo larger signals. The total
chargerecorded
is of
~5800
photoelectrons.
Insettrackis an direction
overheadisperspective
viewof the event. The best-fitting track direction is shown as an arrow,associationa high-energy
neutrino
harge recorded is ~5800 photoelectrons. Inset is an overhead
perspective
view
theof
event.
The best-fitting
shown as anarrow,
þ0:50
witha blazar
duringa periodof enconsistent witha zenithangle
5:7"0:30
degrees
below the horizon.
onsistent with a zenith angle 5:7þ0:50"0:30 degrees below the horizon.
Ahanced g-ray emission suggests thatblazars may indeed be one of the longMultimessenger observations of blazar TXS 0506+056. The
sought sources of very-high-energy
50% and 90% containment regions for the neutrino IceCubecosmic rays, and
170922A (dashed red and solid gray contours, respectively),- hence responsible forBoverlain on a V-band optical image of the sky. Gamma-ray sources a sizable fraction of the cosmic neutrino flux observed by IceCube.
in this region previously detected with the Fermi spacecraft are
shown as blue circles, with sizes representing their 95% positional
The list of author affiliations is available in the fulluncertainty and labeled with the source names. The IceCube
C
article online.
neutrino is coincident with the blazar TXS 0506+056, whose*The full lists of participating members for each
optical position is shown by the pink square. The yellow circle
team and their affiliations are provided in the
supplementary materials.
shows the 95% positional uncertainty of very-high-energy g-rays†Email: analysis@icecube.wisc.edu
detected by the MAGIC telescopes during the follow-up campaign.
D
Cite this article as IceCube Collaboration et al.,The inset shows a magnified view of the region around TXS 0506+056 Science 361, eaat1378 (2018). DOI: 10.1126/
on an R-band optical image of the sky.
science.aat1378

1, 146 (2018)

Downloaded from http://science.sciencemag.org/ on July 13, 2018▪

IMAGES: PHOASAS-SN FOR THE V-BAND OPTICAL; KANATA FOR THE R-BAND IN MAGNIFIED VIEWEM Counterpart Discovery of IceCube-170922AE

1 of 113 July 2018

F

IceCube Collaboration+ 2018

pixel,
detected
photonsofwith
energy of 1 to 300 GeV in a pixel,
2° by using2°
ig. 2. Fermi-LAT and MAGIC observations of IceCube-170922A’s
detected photons with energy of 1 to 300 GeV in a 2° by 2°
Fig. 2. Fermi-LAT
andusing
MAGIC
observations
IceCube-170922A’s
regionaroundTXS0506+056.
The map
has a pixel
size
of 0.02°
and wasocation. Sky position of IceCube-170922A in J2000 equatoriallocation.
coordinates
regionaroundTXS0506+056.
map hasa pixelsize
of 0.02°
and wasSkyFig.
positionof
IceCube-170922A
in J2000
equatorial
coordinates
dashedline marks theThe
detection
timeof theneutrino
IceCube-170922A
3. Time-dependent
multiwavelength
observationsof TXSsmoothed
witha
0.02°-wide
Gaussiankernel.
MAGIC
data
are
shown
as
verlaying the g-ray counts from Fermi-LAT above 1 GeV (A) andthe signal
smoothed
witha
0.02°-wide
Gaussiankernel.
MAGIC
data
are
shown
as
overlaying
the
g-ray
countsfrom
Fermi-LAT
above
1
GeV
(A)
and
the
signal
The left set of panels shows measurements between MJD 54700
0506+056 before and after IceCube-170922A. Significant variability of

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EM Counterpart Discovery of IceCube-170922A
IceCube alert (GCN 21916): 2017/09/22, 20:54:30 (UT)
7 BROS (blazar candidates, Itoh+ in prep.) sources within error region
TXS 0506+056 variability detected with Kanata/HONIR==> Fermi/LAT variabilities (gamma, ATel #10791, Tanaka+)==> multi-wavelength follow-up (IceCube Collaboration+2018)
optical/NIR imaging, spectroscopy, polarization: incl. MITSuME, Kiso,
Nayuta, Kanata, IRSF (OISTER) + Subaru (TM+ in prep.)z=0.336 (Paiano+2018, GTC/OSIRIS)

ublications of the Astronomical Society of Japan, (2014), Vol. 00, No. 0

3

IceCube-170922A 増光天体探索②
いた。

かなた
9/23

カ

3/23
かなた
9/23
ー
2MASS
差分
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2MASS

Kanata/HONIR
J-bandTM+ in prep.

3/23 - 3/2418

Optical Time Domain and Multi-Messenger Astronomy

Optical Time Domain/transient + VLBI?
supernova ejecta interaction w/ CSM
mass loss history just before explosion= end of life of massive stars
progenitor stars of Type Ia supernovae
relativistic jets for Type Ic supernovae/GRBs
jet in kilnovae (GW170817)/sGRBs
high-energy neutrino sources?
relativistic jets in AGN
blazars
high-energy neutrino sources?
radio-loud NLS1s

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19

VLBI observations for nearby SNe
detection: all Type II or Ib/c
massive star origin
ejecta-CSM interaction
CSM density, ejecta density,
magnetic field~> 1 mJy / beam @ 8.4 GHz(~0.5-1 mas)distance ~< 10 Mpc
rate: ~1 SN / yr“movie”
SN 1993J (~3 Mpc): Type IIb

Bietenholz+2003

8.4 GHzEAVW-2019@Ibaraki University

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Optical Time Domain and Multi-Messenger Astronomy

20Type Ia supernova progenitors: single/double degenerate?
recent mass loss expected for single degenerate
no detection even for nearest cases
SN 2011fe@M101 (Chomiuk+2012, <19 uJy@5 GHz?)
SN 2014J@M82 (Perez-Torres+2014, <12-41 uJy@1.5-22 GHz)
tight constraint on mass loss rate: several x 10^-10 Msun/yr==> likely double degenerate (at least for these two)

double degenerate (DD)EAVW-2019@Ibaraki University

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single degenerate (SD)©AAVSO

Optical Time Domain and Multi-Messenger Astronomy

21

GW170817 kilonova w/ VLBIRESEARCH LETTER

a

12

102

A3 (Tj,0 = 0.04, Tj,p = 0.08, Tobs = 0.50)
A1 (T < Tj,p)A1 (T > Tj,p)Day 754101

FQ (μJy)

Declination offset (mas)8

Narrow jet
Tjet
A1 (Tj,0 = 0.04, Tj,p = 0.08,
Tobs = 0.35)
Tobs≤5°
A2 (Tj,0 = 0.04, Tj,p = 0.08, Tobs = 14°–28°
0.25)

0

b 102
–4

n ≈ 10–4–5×–5×10–3 cm–3
B: very narrow jet (Tj,0 = 0.03, Tj,p = 0.06, Tobs = 0.3)
E ≈= 10
C: wide jet (Tj,0 = 0.07, Tj,p = 0.13, Tobs
0.549)–1050 erg

D: choked jet (Tobs = 0.6)

Day 230

–8

101

–12
8

6

4

2

0

–2

–4

–6

–8

Right ascension offset (mas)Fig. 1 | Proper motion of the radio counterpart of GW170817. The
offset positions of the centroid (shown by 1σ error bars) and 3σ–12σ
contours of the radio source detected 75 days (black) and 230 days (red)after the merger event using VLBI at 4.5 GHz. The two VLBI epochs haveimageMooley+2018
root-mean-square noise of 5.0 µJy beam−1 and 5.6 µJy beam−1(natural weighting), respectively, and the peak flux densities of GW170817
are 58 µJy beam−1 and 48 µJy beam−1, respectively. The radio source

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2019/09/24-26

10t (days)100

Fig. 2 | Radio, 3-GHz light curves of several representative simulat
models. The black error bars (1σ) are the 3-GHz flux density (Fν) valu
for GW170817. The grey shaded regions denote the VLBI epochs:
75 and 230 days after the merger. a, A narrow jet with an initial openi
angle of θj,0 = 0.04 rad (2.3°), total energy of E = 1050 erg and isotropic1053 ergand
at thecore, as observedat threeequivalentenergy ofiso =Fig. 4 | SchematicofEthephysicalgeometric
parameters
deriveddifferent
viewing
angles(models
A1–A3).
For
all
light
curves,we takefor GW170817. GW170817 has a successful jet (yellow) that drives
22aOpticalTime
DomainandMulti-Messenger
Astronomy
theenergyfractionofaccelerated
electrons
to
be
ε
=
0.1,
assumee ejecta (blue).aTh
cocoon (red) through interaction with the dynamical

E

Magnitude

AGN w/ relativistic jets

20.0
20.5

so many blazar studies
identification of Fermi/LAT unID
21.0sources w/ VLBI and optical variability
IceCube neutrino-related
studies60”
21.5
serendipitous discovery of a radio-loud narrow line Seyfert 1
22.0 Supernova Survey (TM+2014)
SDSS rapid brightening (<1 day) in Kiso
10^7 Msun black hole (Tanaka, TM+2014)
22.5
1556
K.
É.
Gabányietal.
radio follow-up: JVN, EVN (Gabanyi, TM+2017)-1
0, VERA1
2
3
MJD-56711.0 (2014-02-23 UT)
optical/NIR monitoring (TM+2017)
constant power-law
index
19.0
2014
no companion galaxy 2003g
physical Journal Letters, 793:L26 (6pp), 2014 October 1
Tanaka et al.
B==> not a merger19.5
system?
R
19.0

KISS

FIRST

100 kpc

20.0

Magnitude

E

60”

c

J+2.

g
B

Epoch
1 23

20.5

20.5
21.0 21.0
21.5

21.5

Gabanyi+2017
EVN, 5 GHz

22.0

SDSS

5.4’’

2014

19.5 20.0

Magnitude

N

2003

10’’

22.5 22.0

-1

0

1

2

3

Figure 1. Naturally weighted 1.7-GHzMJD-56711.0
EVN image (2014-02-23
of J1100+4421.
UT)
Observation took place on 2015 February 10. The peak brightness is22.5beam is 24.8 mas × 8.2 mas (FWHM)−1mJy
EAVW-2019@Ibaraki 19.4
University
2019/09/24-26
Optical Time Domain and Multi-Messenger Astronomy
19.0beam , the restoring

Tanaka,TM+2014 -5
◦

0

5

10

15

20

25

30

23

35

Summary
Time Domain Astronomy in optical is now rapidly evolving.
High-Cadence surveys (multiple visits per night) even for
extragalactic objects are now one of the frontier fields.
Multi-Messenger Astronomy is now one of the hot topics;
EM counterparts of gravitational wave sources: kilonovae
EM counterparts of IceCube high-energy neutrinos:
blazar? peculiar supernovae?
Optical-Time-Domain & VLBI collaborative observations
nearby SNe w/ CSM interaction
jets in kilonovae
AGN w/ relativistic jets

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24