短時間スケール突発天体の可視光サーベイ観測

諸隈 智貴 (Morokuma, Tomoki)(東京大学・天文学教育研究センター)
短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

1

Contents
Transients in optical “classical” surveys (days)
Current frontier of optical transient surveys (<1 day)Higher cadence survey observations in optical (second)
Summary

短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

2

Summary
Optical transient sky in a time scale of days has been
explored since discovery of acceleratedly expanding
universe with Type Ia supernova observations (late1990’s).
Recently, 1-day or shorter time scale transient havebeen discovered and studied.
Wide-field optical surveys in a time scale of seconds(or shorter) have been started.
requests: Please
propose science cases requiring high-cadence
observations
think about a theory explaining/predicting secondscale transient phenomena in optical.
短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

3

Time Scale vs Size
1 sec

1
1 hr day

100
days

t
h
lig

s
o
cr

g
n
i
s

e
m
ti

AGN AD (109 Msun)
SN IIn (CSM)

TDE
SN Ia (WD)

109

nova
NS

短時間スケール突発天体のサーベイ観測kilonova (NS)第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

4

−24

45

Luminous Supernovae
SCP06F6
SN2005ap SN2008es PTF09cnd
SN2006gy
PTF09cwl PTF09atu
PTF10cwr

−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

10

1 day

1

10

2

10

Characteristic Timescale [day]Kasliwal 2011

Figure 8.1 Framework of Cosmic Explosions in the Year 2011. Note that until 2005 (Fig-

短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

5

−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

#()*()
38
1

10
-3

−6

02

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

P60−M81OT−071213
38

1

10

1

1

10 1 10
-1
10

−6

39

Classical
Novae
M31 RV

1 day

10

10
-2

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),

knew
about(denoted
by
gray
In
six
years,
searches,
we onlyweknew only
aboutknew
threeclasses(denotedby gray
bands).three
In the理論懇シンポジウム
past(denoted
sixclasses
years,
we onlysystematic
knew about
searches,
three classes(denotedby gray
bands).
Inbands).
the pastthe
sixIn
years,
wepastonlythesystematic
knew theabout
searches,
threepastclassesby gray
bands).
In thesystematic
past searches,
six@2019/12/25-27
years, systematic
searches,
we only
knew
about
three
classesbygraybands).
In
six
years,
systematic
短時間スケール突発天体のサーベイ観測
第32回「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ
we
only
about
three
classes(denotedbygraybands).
pastsix(denoted
years,
systematic
searches,610

log ( Characteristic Timescale [day][sec])(z~1""""""""""""""""""""""""""2""""""""""""""""""""""""""3""""""""""""""""""""""""""4"""""""""""""""""""""""""5"""""""""""""""""""""""""6""""""""""""""""""""""""7"
0.2)

−2424

24

24

Luminous Supernovae

Luminous Supernovae

Luminous Supernovae

SCP06F6
SN2005ap SN2008es PTF09cnd
22
SN2006gy
PTF09atu
PTF10cwr PTF09cwl

SCP06F6
SN2005ap SN2008es PTF09cnd
22
SN2006gy
PTF09atu
PTF10cwr PTF09cwl

SCP06F6
SN2005ap SN2008es PTF09cnd
44
SN2006gy
10
PTF09atu
PTF10cwr PTF09cwl
10)*!&+()*)  
−2222



$$(.
10 0 M
+()*)
pc (C(*!&%!%&
om
a##'C)+lu
ster)
&+*
"


(


10 M
) &"


,
&
%
(
.'
)+'

pc

)
'

#
#
&(&
SN2007bi

1 Mp

c

Thermonuclear
Supernovae

SN2007bi

20

SN2002bj

−1818

−1616

PTF10iuv

−1212

−1010

1 m class −8−8
telescopes −6−6

PTF10fqs

Classical Novae

10

SN2008S-3

% Ca−rich%&,Transients41*+Luminous+&
PTF10fqs

.

(

Red
+)-

M31 RVNovae

10 M85 OT-2

M31 RV

8

P60−M81OT−071213

0NGC300OTPTF10fqs
P60−M82OT−081119

Luminous 101040
Red
Novae
M85 OT
M85 OTV838 Mon

V838 MonClassical Novae

1010SN2008S
PTF10acbp()12 *)

Luminous
Red
Novae

6

SN2005E

NGC300OT

#()*()
1

PTF10iuv

SN2008ha

14Ca−rich!#&%&,
Transients PTF10acbp

12

8

PTF11bij.Ia Explosions PTF09dav

16

SN2008ha

Core−Collapse
42Supernovae 1010

PTF10bhp

SN2005E&!%P60−M82OT−081119
$
+
#
M85
OT
10(
#*V838Mon

P60−M82OT−081119

P60−M81OT−071213-4

PTF10iuv

14

NGC300OT

0

PTF11bij.Ia Explosions PTF09dav

16

SN2008S
PTF10acbp

Core−Collapse
Supernovae

PTF10bhp

SN2005E

.'
SN2008ha−1414 ) &"Ca−rich("&+* Transients

43

10
10

18

Core−Collapse
Supernovae

PTF11bij.Ia Explosions PTF09dav

Thermonuclear
Supernovae

SN2002bj

18

PTF10bhp

SN2007bi

20

Thermonuclear
Supernovae

SN2002bj

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

V

Peak Luminosity [M ]

−2020

45

10
10

39

Classical Novae

10
M31 RV 10

P60−M81OT−071213

1 day
1

-1
10

6

Peak Luminosity [erg s−1]

1 Gpc

10

0

0

log (Characteristic Timescale [day] )

38

1010
1

1

10

2

2

Kasliwal 2011, Cooke (http://www.astro.caltech.edu/~ycao/B&ETalks/B&E_FRBs_Cooke.pdf)
短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27710log ( Characteristic Timescale [day][sec])c (z1""""""""""""""""""""""""""2""""""""""""""""""""""""""3""""""""""""""""""""""""""4"""""""""""""""""""""""""5"""""""""""""""""""""""""6""""""""""""""""""""""""7"
~1.4)
−2424

Luminous Supernovae

Luminous Supernovae

SCP06F6
SN2005ap SN2008es PTF09cnd
22
SN2006gy
PTF09atu
PTF10cwr PTF09cwl

SCP06F6
SN2005ap SN2008es PTF09cnd
22
SN2006gy
PTF09atu
PTF10cwr PTF09cwl

SCP06F6
SN2005ap SN2008es PTF09cnd
44
SN2006gy
10
PTF09atu
PTF10cwr PTF09cwl
10(z~0.(*!&%!
2)&##%+
−2020

V

Thermonuclear
Supernovae

SN2002bj

−1818

')

24

Luminous Supernovae)*!&+()*)  −2222

Peak Luminosity [M ]

1 Gpc

24

$$(.
SN2007bi
+()*)
20

SN2007bi

SN2007bi

20

Thermonuclear
Supernovae

Thermonuclear
Supernovae

SN2002bj

18

10 0 M
) &


,
&
%
(
.'
)+'


)
'

pc (C
#
#
&(&
.'o ma) &"
Clust
%
!#&%&,
er)("&+*
%&,
*)
)
(
+
+*
&

10 M
.
-(

)
+
&
pc
#+$!%
Core−Collapse
Supernovae

PTF11bij.Ia Explosions PTF09dav
PTF10iuv−1010

8 m class −8−8
telescopes −6−6

SN2008S
PTF10acbp

PTF10fqs

Classical Novae-410Ca−richTransients

NGC300OT

LuminousRed
Novae

PTF10fqs

P60−M82OT−081119

M31 RV-3-2

SN2005E

SN2008ha

Ca−richTransients

41

NGC300OT

12Luminous
Red
Novae

Classical Novae

M31 RV

810
10

SN2008S
PTF10acbp

PTF10fqs

P60−M82OT−081119

Luminous 101040
Red
Novae
M85 OT
M85 OTV838 Mon

V838 Mon

P60−M81OT−071213

0

PTF10iuv

10 M85 OT

#()*()
6

PTF11bij.Ia Explosions PTF09dav

14

SN2008S
PTF10acbp

Core−Collapse
42Supernovae 1010

PTF10bhp

SN2005E

12

8

1

16

SN2008ha

M85
OT
10(
#*V838Mon

P60−M82OT−081119

P60−M81OT−071213

0

PTF10iuv

14

NGC300OT

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

−1212.Ia Explosions PTF09dav

SN2005E

Ca−richTransientsCore−Collapse "&+*PTF11bij "(Supernovae

PTF10bhp

16

SN2008ha

−1414

43

10
10

SN2002bj

18

PTF10bhp

−1616

45

10
10

39

Classical Novae

10
M31 RV 10

P60−M81OT−071213

1 day
1

-1
10

6

Peak Luminosity [erg s−1]

10 Gp

10

0

0

log (Characteristic Timescale [day] )

38

1010
1

1

10

2

2

Kasliwal 2011, Cooke (http://www.astro.caltech.edu/~ycao/B&ETalks/B&E_FRBs_Cooke.pdf)
短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

8−6

1 local Universe
Transientsin10
theTransientsin thelocal
Universe
Transients
in
the
local
Universe
Transientsin the local Universe log
383
Transientsin
the
local
Universe-3-1( Characteristic Timescale [day][sec]) 383

Occurence Rate [Gpc
0

10

yr ]

10

383383383 383

2

TransientsinthelocalUniverse

10

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]

]

= 0)
z
,
4
1
0
2
+
5 (Taylor

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
SCP06F6sGRB:by1e2
SCP06F6
we only
about three(denotedgray(Mandhi+2019,z=0)
bands).
In thepast six years, systematic
searches,
FRB:
4e4knew(Totani,z<1)classes
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
long
GRB:
1e0
(Lan+2019,z=0)
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, Cadvanced−16−16
CSN: 1eVIRGO, LCGT, INDIGO) coming online. Detecting gravitational
waves from neutron&star
every month isyexpected to become routine. A basic common(mergersxathe electromagneticl.'
SN2008ha
aality
betweengravitational
wave
searchesandsearch describedabove is that
SN2008ha
41−14SN Ia: 2e4gSN2008ha
SN2008ha
SN2008ha
SN2008ha
4110
−14
/
41
41
41
41
−14 ) &"
−14
−14
−14
r
SN2008S
1540+3200-1220
10Ca−rich% Ca−richy Ca−rich
SN2008S
10(say,10PTF10acbp
10 poor10sky
SN2008S
SN2008Sknown
SN2008S
both are limited to the
local Universe< 200Mpc). A
challenge
will be SN2008S
theCa−rich/Ca−richCa−rich5
PTF10acbp
!#&%&,
(Maoz+2011,z=0) ("&+* Transients PTF10acbp 0
PTF10acbpPTF10acbp
PTF10acbp
Transients
Transients%&,
Transients
Transients rate
Transients
localizations of the gravitationalwave
signalandconsequent
large
false
positiveof electro1
NGC300OT(Abbott+2017)
4NGC300OT
NGC300OT
NGC300OT
NGC300OT
NGC300OT−12
0 &−12Kasliwal 2009). Therefore,) to the ambitious
magnetic(Kulkarni
priorsearch for an−12 −12candidates
−12
−12
*
1
)
(
40
+
Luminous:*
4010
Luminous
40 PTF10fqs
40
40
Luminous 1040
Luminous
Luminous+
LuminousE&
PTF10fqs
PTF10fqs
PTF10fqs
PTF10fqs

PTF10fqs.
10 only be prudent
10 buildelectromagnetic counterpart
Red 10 10this
Red RedRed to
TD to aRedgravitational+)wave-(signal, itRedwould

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 −10−10Classical Novae−10 M85 OT
V838 Mon

M31 RV 10

39

Classical
Novae 39Classical
Novae Novae
Classical
Novae
Classical
M31 RV 103838

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

39

Classical
Novae
M31 RVSFR evolution:−8−8−8−8 P60−M81OT−071213−8P60−M81OT−071213
P60−M81OT−071213 −8 P60−M81OT−071213
P60−M81OT−071213
P60−M81OT−071213
10 times#()*()
38
1 daylarger at z~2
3810
10
10
10
10
10
−6 02
−6 02
−6−6 0 −60 −6
0
1
2 2
1
11
1
1
2
0 10
2
10 10 10
10
10
10 10
100
101 10 10 10 102
-4
-3
-2
-1
10 10
than local
Characteristic[day]
Characteristic Timescale [day]log
Characteri
sticTimescale
TimescalTimescalee [day] [day][day]Characteristic
Timescale() Characteristic Timescale [day]Characteristic
universe
Kasliwal 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),
39
39
3910
M31
10
M31 RV 10
M31 10
RV RV

38

38

knew
about
(denoted
by
gray
In
six
years,
searches,
we onlyweknew only
aboutknew
threeclasses(denotedby gray
bands).three
In the理論懇シンポジウム
past(denoted
sixclasses
years,
we onlysystematic
knew about
searches,
three classes(denotedby gray
bands).
Inbands).
the pastthe
sixIn
years,
wepastonlythesystematic
knew theabout
searches,
threepastclassesby gray
bands).
In thesystematic
past searches,
six@2019/12/25-27
years, systematic
searches,
we only
knew
about
three
classesbygraybands).
In
six
years,
systematic
短時間スケール突発天体のサーベイ観測
第32回「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ
we
only
about
three
classes(denotedbygraybands).
pastsix(denoted
years,
systematic
searches,9

Optical Transient Surveys
wide

Yasuda+2019
all-sky

Kiso/Tomo-e Gozen

{

{

~2m

< 1m

CCD readout time~a few x 101 [sec]{~8m, HST{~4m

narrow
shallow
短時間スケール突発天体のサーベイ観測deep
第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

10

Optical Transient Surveys~2mshallow
短時間スケール突発天体のサーベイ観測

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

narrow

~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
第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

11

(All-Sky
Automated Survey
OpticalASAN-SN
Transient
Surveys

Yasuda+2019
LSST (8.4m), 2022all-sky

for Supernovae)

wide

Kiso/Tomo-e Gozen

{

{

~2m

< 1m

Subaru Telescope (8.2m)
HSC, 2014-{
Palomar Transient Factory (PTF)==> Zwicky Transient Facility (ZTF)~8m, HST{~4m
Pan-STARRS1 (1.8m)
2012-

narrow
shallow
短時間スケール突発天体のサーベイ観測

https://panstarrs.stsci.edu

deep

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

12

2012 Feb 05
2012 Feb 24
2012 Mar 16
2012 Apr 13
2012 Apr 30
2012 May 23
2012 Dec 16

+148
+167
+188
+216
+233
+256
+463

5962.895981.856002.716030.766047.79
6070.79
6277.56

2700
3600
3000
3600
3000
3000
3600

Recent SN Surveys = High Cadence SN Surveys
1990s (a few days): “tardy” surveys/monitoring (cosmology)
2010s (1 or <1 day): many “rapid”Notes.
phenomena recently reported.
ab2,450,000.5 has been subtracted from the Julian Date.
Relative to the epoch of B-band maximum (JD = 2,455,814.98).

Light curve examples of Type Ia Supernovae

Zhang+2016 (SN 2011fe)
10 days
10 days

Hamuy+1996
短時間スケール突発天体のサーベイ観測

Figure 2. The UV, optical, and NIR light curves of SN 2011fe, with UV datafrom Brown et al. (2012) and NIR data from Matheson et al. (2012).

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

13
6

Optical High-Cadence Transient Surveys
wide

Yasuda+2019

all-sky
Kiso/Tomo-e Gozen~2m{several visits per night{(< 1 day)

< 1m

(
S
T
i
H

r+
e
t
s
For

om
T
(
T

a+)
g
a
in

{

O
SHO

)

~8m, HST{~4m

narrow
shallow
短時間スケール突発天体のサーベイ観測deep
第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

14

Shock breakout in core-collapse supernovae
before

after
~days

progenitor = massive starshock breakout instellar surface?
CSM / wind?

~hours©Uni.v of Tokyo

Shock Breakout
The Astrophysical Journal, 832:155 (22pp), 2016 December 1©NAOJ, T. Moriya

短時間スケール突発天体のサーベイ観測

Forster+2018
Figure1. Schematic representation of the optical light curve of a red supergiant
15
第32回 理論懇シンポジウム「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ@2019/12/25-27
core collapse
supernova in arbitrary units (c.f.Figure1
in GarnavichRapidly Evolving Transients

w/ Subaru/HSC
Tanaka, Tominaga, TM+2016
Tominaga, TM+2019

progenitor stars of core-collapse supernovae

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

Tanaka et al.

June, 2014
2 contiguous nights
Subaru/Hyper Suprime-Cam(HSC, 1.8 deg2 FoV) survey
Subaru/FOCAS spectroscopic
follow-up (for hosts)
several “rapid transients”~10^-3 Msun/yr mass loss
> 1% of CCSN rate
Tanaka et al

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

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.

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
r 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
mples. 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 and observer frame, i.e.,2n (ne ) = [(4pd ) (1 + z )] fn (no ), where νe and νo are rest短時間スケール突発天体のサーベイ観測
ame and observer frame frequencies, and d is the luminosity

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.

cooling envelope

wind shock
breakout

16
3.2. Comparison withSNe
第32回 理論懇シンポジウム「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ@2019/12/25-27
Figure 9. Summary of absolute magnitudes and rising timescale (τ ≡1/ ∣Dm Dt∣) of transients. Our samples are compared with the following objects: SN 2010aq
riseHiTS = High Cadence Transient Survey

The Astrophysical Journal, 832:155 (22pp), 2016 December 1

Forster+2017

Table 1
2013,
2014,
2015
Selectionof Large-ﬁeld-of-view(FOV) Optical Astronom

4, 4, 5 nights (13nightsin total) Etend
Area
Field of View)
(deg2)(m2 de(m2Blanco
DECam on CTIO
(4m)
Kepler3.0 deg2 field-of-view
0.7
115
81.
HSCb
52.8
1.5
79.
No shock breakouts
discovered
DECam
11.3
3.0
33.
c
comparison
w/ 2.5
2 day
theoreticalmodelsPanSTARRS-1
13. Cumulative number of predicted SN detections during SBO optical peak (a) or at least twice
during the ﬁrst rest-frame
after shock 7.0
emergence(b) as a17.
iPTFdTominaga+2011,
7.8 Sariof redshift for the combined 13A, 14A, and 15A survey campaigns assuming the M30 distribution
and the Tominaga1.1
et al.Nakar(2011) models.
We show
the 8.
&
2010
Camerave number of SNe obtained with the empirical probability of detection P(m) and a perfect subtraction
thickblacklines5.7
in Figure 12), but 8.
SkyMapper(the sum of the1.4
ng
the contributionsof representationeach IMF-weighted
model
as explainedin Section 3.4. KMTNete
Figure1. Schematicof theexplosion
optical lightcurve
of a red supergiant
2.0
4.0
8.

l Journal, 832:155 (22pp), 2016 December 1

Förster et al.

core collapse supernova in arbitrary units (c.f.Figure1 in Garnavich
et al. 2016). Note that the wind SBO optical ﬂux depends on the propertiesof the circumstellar material and may not always be dominant at early times.

QUESTfLSSTg
ZTFh

from that of the total luminosity. While the total luminosity
generally declines monotonically after SBO, the NUV and
optical luminosity can decline and then rise again for several
days up to maximum optical light (e.g., Schawinski et al. 2008;
Tominaga et al. 2011).
The adiabatic approximation will be valid preferentially inthe denser inner layers, as the outer layers become dominatedby radiative diffusion with time. The radius where thistransition occurs is known as the diffusion wave radius, which
can be estimated by equating the star’s radiation diffusion timewith the time since explosion. In those stars, where radiative
diffusion is negligible during this phase, with initial radii of
0.91 -0.40
RE
100R,
theproductofcanbe constrainedR shouldein M
ej been
14.åPredicted cumulative
number of SNe thathave
detected

Notes. The collecting area, FOV, etendue (product of area
number of pixels of each survey telescope are given. All li
already operational, except for LSST and ZFT.
a
Limited bandwidth requires pre-selection of pixels.
b
Hyper Suprime Camera.
c
Panoramic Survey Telescope and Rapid Response System.
dIntermediate Palomar Transient Facility.
e
Koren Microlensing Telescope Network.
f
Quasar Equatorial Survey Team.
g
Large Synoptic Survey Telescope.
h
Zwicky Telescope Facility.

0.8
35.7
1.1

8.3
9.6
47

6.
344.
51.

subsequent SN explosion to discard other varistributionof the ﬁelds observed in the 2013A, 2014A, and 2015A HiTS campaigns
in equatorial(R.A., decl.) and galactic(b, l) coordinates.
SeeTriplets
短時間スケール突発天体のサーベイ観測
第32回
理論懇シンポジウム「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ@2019/12/25-27
be moreobtained
with17aFigure15. Total
number canof expected
SBO efﬁciently
peak detectionsin the combined
tails.

HiTS = High Cadence Transient Survey

Forster+2018

steep rise in light curves
24 among 26 SNe II
shock breakout in dense CSM
mass loss rate: > 10-4 Msun/yr
hour-scale (stellar surface) shock
breakout: rare?

短時間スケール突発天体のサーベイ観測18
第32回 理論懇シンポジウム「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ@2019/12/25-27
Figure4: Distribution of inferred and Ṁ values for the sample of
26 early SNe II candidates

Evolution of Seed BHs

MMUNICATIONS | DOI: 10.1038/ncomms2314

direct collapse

supermassive star

Big bang
200 Myr

REVIEW

Death of massivestars

Direct collapse

Track the growth of
The AstrophysicalJournal Letters, 809:L14 (6pp), 2015 August 10
black holes and

500 Myr

Baldashalos
Most halos are seeded but
seeds are ~100 solar masses~104 Msun
3 Gyr~102 Msun

Halos growvia merging.

Black holes growvia accretion andmerging.

Some black holes areejected by gravitational
wave radiation.

Observational consequences

Few halos are seeded, but seeds
are ~104 solar masses
Observational consequences

1 Gyr

Figure 3. Left: smoothed SDSS gri image of RGG 118 (ﬁlters colored blue, green, and re118. An X-ray source is clearly detected at a position consistent with the nominal SDSS p
smoothed with Gaussian kernel of T  3 pixels. Right: r band surface brightness versus
ELLIPSE package are shown as gray dots. The dark and light blue shading represents theblack lines plot the r-band PSF. The solid red line shows the best-ﬁt Sérsic+exponenti
components).

E(B–V) = 0.032 for RGG 118 (Schlaﬂy & Finkbeiner 2011).
For the inner Sérsic component (consistent with a pseudobulge,
as discussed in Section 3), we measure g  r  0.49 o 0.19,
which gives log10 (M L)r  0.23 and M*,inner = 108.8 o 0.2 M:.
10
Today virtually all >10 solar mass
For the exponential disk component we measuregalaxies contain supermassiveg  r  0.41 o 0.07, which yields log10 (M L)r  0.15 andblack holes
13.6 Gyr~100% of ~109 solar mass
~60% of ~109 solar mass
5
galaxies contain ~10 solar
M*,disk = 10 9.3 o 0.1 M:. Combined, the masses of the bulge andgalaxies contain >105 solar
mass black holes
mass black holes
disk are consistent with the NASA-Sloan Atlas total stellar
mass of M* = 10 9.3 M:. We also obtain a bulge-to-disk mass
olution of seed black holes. Schematic of the evolution of seed black holes assuming two different formation mechanisms (the death of ratio
the of ∼0.3.
6 Gyr

n of massive stars versus the direct collapse of gas into a black hole). Dark matter halos and the galaxies in them grow through merging. Blackoth via merging and by accreting gas. One additional complication is that after merging, gravitational radiation ‘recoil’ (see text for details) may
k hole out of the galaxy. At present, we can distinguish between the two scenarios based on the fraction of small galaxies that contain massive
we call this the ‘occupation fraction’).

3. BH MASS AND SCALING RELATIONS

rel
at

Se
2.7
no
rep

10
po
11
AG


Strong evidence for BH accretion in RGG 118 comes fromofnarrow emission line ratios (Figure 1), broad Hα emission, andcom
a nuclear
X-rayCircles
point andsource(seerepresent
Section systems
2.2). Assuming
theFigure 4.
Both:formation
black solid/dashedlines representifvarious
determinations
scaling
relations.
squareshaving dynamicallymasks it. Furthermore,
the correlation
betweenofblacky were shining via the energy released as material
falls
ha
RGG
118 is plotted
the pink
star. Errorbars
Ho and2013)bulge
with massclassical
and pseudobulges,
respectively.
Left:emission
broad
indeed thesignatureof gas as
rotatingarounda
MBHT*isrelation.
mass
applies,the black holes
in smaller
The hole &ccreted by) the central supermassive blackmasses
hole23. (Kormendy
scatter inused makes
to determine
the BH mass;
velocityerrorsincludein theusing
relation
betweenstellar andthenucleardispersion
BH, we canestimate
thescatter
BH mass
standard
virialarethelesscorrelations
massive, which
their emission
weaker.
f real supermassive black holes, with accountmasses forof thegalaxies
dispersion
52 (Barth which
et al. 2004;
Thornton
et al.in2008)
and NGC(Filippenko
techniques
assumethe gasthe broadline4395
regionf millions of times the mass of the Sun
became(Barth et al. 2008). We also show the well-studied dwarf AGN POX(turquoise
diamonds).
For
NGC
4395,
which
is
bulgeless,thevelocity
dispersion
is
an
upper
limit
and
referstothenuclearstar
cluster(Filippenko
surrounding the BH is in virial equilibrium (Peterson & Ho 2
accepted, but it was far less clear whether these
relation.
Total
masses aregalaxies.
plotted for
52 (Thornton
2008), The
and NGC(Filippenko& Ho 200
dashed black
gives theevidence
MBHMfor
4et POX
al. 2004;
Bentz etetal.al.2010).
virial 4395
relationshipgivesbulge black
Dynamical
holes
in low-massFor
epresented a rare and long-lived phenomenon,
or linetoBH r RBLR %V 2 G , where RBLR is the radius of the broadgalaxies contained supermassive black holes with the handful of low-mass galaxies nearest to us, it is possible M
search for the gravitational signature of a central black hole. line
In emitting region, and %V is a characteristic velocity of gas 19
bright episodes.
短時間スケール突発天体のサーベイ観測
第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ@2019/12/25-27
stark
contrast theto bulge-dominatedgalaxies,explanations
these nearby smallears later we finally learned that supermassive
Weblack
do notconsiderabove to be likely
forin the broad
formation
pathwaysmustthat produce
line region.
We usethe exist
Hα emission
line to BH se

Volonteri 2011, Greene 2012blind survey (SDSS optical spectroscopy) +follow-up spectroscopy (Baldassare+2015)
RGG 118 @ z = 0.0243 (~100 Mpc)
5x10 Msun BHsub

A Rapidly Variable AGN w/ A Low-Mass Black Hole
TM+2016

low-mass BH==> small accretion disk==> rapid variability?
Subaru/HSC
2 consecutive nights
Subaru/FOCAS
spectroscopy ==> AGN
w/ 2.7x106 Msun BH @z=0.164

10% variability assumed

Subaru/Hyper Surpime-Cam
Subaru/Prime Focus Spectrograph

短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

20

High-Cadence Surveys w/ 1m-class Schmidt telescopes
2012-2017: Kiso Supernova Survey (KISS, TM+2014, 1.05m, 5 deg2)
2018-: Zwicky Transient Facility (ZTF, Bellm+2019, 1.2m, 47 deg2)
2018-: Tomo-e Gozen Supernova Survey (1.05m, 20 deg2)
Tanaka, TM+2014 (KISS)
TM+2016, Gabanyi+2017
19.0

The Astrophysical Journal Letters, 793:L26 (6pp), 2014 October 1

light curves of 20 lowest-z SNe Ia
Yao et al.

2003

N

KISS

2014

g

Epoch

The Astrophysical Journal
793:L26 (6pp), 2014 October 1
1 2 3Letters,B

19.5

19

E
Magnitude

20.0

60”

N

KISS

19

E

20

20.5

Magnitude

Yao+2019 (ZTF)

The Astrophysical Journal, 886:152 (22pp), 2019 December 1

21.0

21

22

SDSS

22

22.0
22.5

The Astrophysical Journal-1Letters, 793:L26
0 (6pp), 20141 October 1

2
19.0 UT)
MJD-56711.0 (2014-02-23
2003

KISS

2003

FIRST

20.0

19.5

短時間スケール突発天体のサーベイ観測

Magnitude

20.0
20.5
21.0
21.5

60”

5.4’’

20.5

2014

21.0
21.5 10’’

2003

2

22.0

20.0

Epoc
1 23

20.5
21.0
21.5
22.0
22.5

g
B
Rc
J+2.0

1-hour cadence@g, 100 deg2 per night
rapid variability of a radio-loud AGN
SDSS

-5

22.5
Figure 1. Left: discovery image of SDSS J1100+4421
taken-1
0 on 2014
1 Febrimage (lower; the beam√size is 5.′′ 4 as shown with the circle; White et al.
MJD-56711.0 (2014-0
separated by a factor of 2. Right: light curves of SDSS J1100+4421 arounin black show the epochs of spectroscopic data. Our photometric data are
19.0(left panel and shaded region). Magnitudes are given in
SDSS magnitudes
2003
2014
(A color version of this figure is available in the online journal.)
19.5

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

5.4’’

19.0
19.5

19.5
100 kpc

E

2014

3

MagnitudeN

Magnitude

19.0@2,500 deg2
127 SNe Ia in 2018 @ <z> = 0.074

21

60”

21.5

SDSS

FIRST
100 kpc
3 g + 3 r (in total 6 epochs)
per night)

20

21

Optical imagers w/ CMOS or EMCCD
some previous observations w/ photomultiplier tubes (PMTs)
pulsar: Crab etc.
e.g., Cherenkov telescopes (CTA, MAGIC, HESS, VERITAS, …)
MAXI J1820+070# of (wide-field) “CMOS/EMCCD” instruments is increasing.
OASES
Kiso/Tomo-e Gozen (1.05m)
TAOS-II (3x1.3m)
WHT (4m), VLT (8.2m), NTT (3.5m)/ULTRACAM
NTT/GravityCam (lucky imaging, 3.5m)
TNT/ULTRASPEC (2.4m)
GTC/HiPERCAM (10m)Subaru/CMOS Suprime-Cam (8.2m)
We now can do a “survey” for second-scale transients.

短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

22

Optical Transient Surveys
wide

Yasuda+2019
all-sky

Kiso/Tomo-e Gozen

{

{

~2m

< 1m

{

~8m, HST{~4m□ high cadence (< 1 day)narrow
shallow
短時間スケール突発天体のサーベイ観測deep
第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

23

Optical Transient Surveys

Yasuda+2019

wide

all-sky
Kiso/Tomo-e Gozen

{

{

~2m

< 1m

Tomo-e Gozen{~8m, HSTCMOS Suprime-Cam (Subaru)
Tomo-e Gozen{~4m□ high cadence (< 1 day)narrow
shallow
短時間スケール突発天体のサーベイ観測deep
第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

24

Kiso Schmidt telescope (1.05m)
Tomo-e Gozen (巴御前; 84 CMOS, Sako+2016)
completed in April, 2019wide field-of-view (20 deg2), fast readout (>2Hz)
蔀関月作, 「巴御前出陣図」,
high-cadence supernova survey
東京国立博物館,©Image: TNM Image Archives==> “all-sky” (~7,000 deg2) & high-cadence (~2 hrs)
2 Hz x 12 frames (6 sec exposure)Start the survey from October in 2019second scale transient search (Richmond, Tanaka, TM+2019)

短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

25

短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

26

Low-mass X-ray BH binary: MAXI J1820-070
http://www.ioa.s.u-tokyo.ac.jp/tomoe/MAXIJ1820+070/MAXIJ1820+070.html

15 Hz
15 sec

Sako+2018

短時間スケール突発天体のサーベイ観測

160 Hz

3 sec
第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

27

Low-mass
X-ray
BH
binary:MAXIJ1820-070
L64 J. A. Paice et al.

L64

J. A. Paice et al.

Figure 1. Left: Section of optical (top) and X-ray (bottom) light curves. The left-hand panel shows a lon
over 150 points (0.5 s), while the right-hand panel shows a zoom-in (illustrated by the dotted line, vert
bands are ugrizs (blue/green/red/dark red/black, bottom-to-top at the 4 s mark). Representative error bars
flaring of the source, down to ∼10 ms time-scales (e.g. at +3.4 s and at +3.96 s). Right: Optical versus X
A positive lag here denotes optical emission lagging X-rays. The colours denote which optical band is cr
the bands is (bottom-to-top) zs –us in order of wavelength. Error (in all bands) was calculated from bootMultiwavelength timing of MAXI J1820

Figure 1. Left: Section of optical (top) and X-ray (bottom) light curves. The left-hand panel shows a longer term trend, binned with a moving average function
broad feature seemfrequencies. Noteover 150 points (0.5 s), while the right-hand panel shows a zoom-in (illustrated by the dotted line, verticalscalesareidentical)
withnobinning.
The
opticalHz.
What can the wavelength dependence100Theretellu
are threebands are ugrizs (blue/green/red/dark red/black, bottom-to-top at the 4 s mark). Representative error bars on individual time bins are shown. Note the rapid
red
between0.02 and 0that there iswit
some odence
of characteristic
emission
wavelength
to the X-rays, or,flaring of the source, down to ∼10 ms time-scales (e.g. at +3.4 s and at +3.96 s). Right: Optical versus
X-ray
DCF
calculated
over52
segments
30s
inlength.
simultaneous
observations
frequency are main
compactlag)
is offarbetfnificantplateau
A positive lag here denotes optical emission lagging X-rays. The colours denote which optical band is central
cross-correlated
withobject
X-rays.(hence,
Around 0time
lag, theorder
to the peak sub-sec
lag drops with inc
optical:the bands is (bottom-to-top) zs –us in order of wavelength. Error (in all bands) was calculated from bootstrapping
over GTC/HiPERCAM
10000 iterations.
andis in fact
a key
prediction for the(10m)
opticallythof the upwards trenin X-ray:compact NICER
jet theory (Blandford & Königl 1
broad feature seems
dominate
PSDs as they
declinehigher indatatoonly
showthea roughly
12 percentatchange
Optical(late)
lags optical
X-ray (early)
frequencies. Notethat wewavelengthseesignificant
beyondto b
opticalrange; thispower
is tooup
shallow
100 Hz.
bya linear~160dependence.
ms.
Similarly, our slope of ∼3.2
There are three significant features of the time lags. The first isof 50 smaller from that found in XTE J1118+4
between 0.02 and 0.2 Hz, where phase−1 lags of close to +π indicate
This isdelayed
too greata differenceµs Å ).
that there is some(2003,
optical160
component
strongly
withrespectmass)
and is consisten
to the X-rays, or,length
if they(andare thus
instead−π ,scaling,that variations
at thisthereanticorrelated.
are other factorsthat affecttheseislags,
sucfrequency are mainly
Following
that, therea sig28

There are a num
particular one at 0.
lags and the firstalong with frequencoincide with a ch
bands. As noted icause a loss of coh
Lorentzians are ind

3.3 Wavelength d

Paice+2019

Figure 2. Relations between g and X-rays: (from top to bottom) X-ray
短時間スケール突発天体のサーベイ観測
理論懇シンポジウム「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ
and optical power spectra; intrinsic@2019/12/25-27
coherence; phase lags; and time lags.
Figure 3. Peak (open circles) and 第32回
centroid(filled circles) lagsof the subs

This is the first tim
on very short sub-s
DCFs using 2 s seg
bootstrapping, takments (with the sam
each iteration, we cthe sub-second lag
A linear trend w
for each iteration, aTomo-e “flash”

Sun

Kikuchi 2016 (master thesis)

Tomo-e Gozen prototype (PM): 8 sensors = ~2 deg2 FoV
a transient only in 1 frame (2 Hz)
nature: astrophysical? something artificial? (reflectedsunlight by space debri)# of “flashes”:
14 flashes in 23 hours ==> satellites?
~zero (but not zero) in Earth’s shadow
very roughly comparable to FRB rate?

stat
o
e
g

yo
r
a
ion

low

短時間スケール突発天体のサーベイ観測

rb

th
ear

,0
6
3
it (~

o

0

<2
~
(
rbit

m)
k
0

k
,0 0 0m)

E

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

29

Tomo-e “flash” after Kikuchi-kun’s thesis
Morii+2017: Tomo-e movies are decomposed to low-ranked sparse
matrix w/ GoDec.
data compression (& systematic data reduction)
Started systematic observations w/ completed Tomo-e Gozen (10times wider FoV)Now comparable “[area]x[time]”.
Data analysis ongoing (by Arima-kun, D1/UT)

Galactic Plane©N. Arima
短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

30

Second Scale Transient Search

Publications of the Astronomical Society of Japan (2019), Vol. 00, No. 0

9

1x10

Limits of search, for sources with toy spectrum
V=12.6
V=13.6
V=14.6
V=15.68

Upper limit on volumetric rate (event/Gpc3/year)

6

Max redshift z

Limits of search, for sources with toy spectrum
Tomo-e Gozen prototype (PM):
8 sensors = ~2 deg2 FoV
10
V=12.6~8 half nights ==> (2-3)x106 seconds
deg2 surveyed
V=13.6
V=14.69
V=15.6 duration
No transients w/ 1.5-11.5 seconds
8
asteroid/comet-WD collision
31 [erg])(De Stefano+2015; 1014 [g],∂t~1[sec],
E~10
7 likely to be extinguishedoptical prompt emission from a GRB

Richmond, Tanaka, TM+2019

1

1x10

1x107

6
Publicationsof the Astronomical Society of Japan (2019), Vol. 00, No. 05

6

Downloaded from https://academic.oup.com/pasj/advance-article-abstract/doi

other two are the initial images of the next chunk, then that1x10
object will not pass the tests. Since this applies only to a4very small fraction of all possible transients (about 0.6%
acceptof those consisting of exactly three or four detections), we
1000003
accept the losses.
Condition 5 causes us to ignore a thin strip around theedges of each image, amounting to 2.7% of the area of the2
acceptsurvey. We will account for this small inefficiency in our10000
calculations of the control time and transient rates later in1
this paper.
Describing the “limiting magnitude” for an instrument 1000
reject0
48 can 49
50
48
49
50
51
52
53
be approachedin51several 52
ways. For53example, under
12
Publications of the Astronomical Society of Japan (2019), Vol. 00, N
Log10optimal[Rest frame(10 keV a- star
2000ofkeV)
Lγ (erg/s)]
log10 [Rest frame (10 keV - 2000 keV) Lγ (erg/s)]
conditions,magnitude
V = 18.5 produces
a signal-to-noise ratio of 5 in a 1-s exposure with Tomo-e
Fig.
9.
Upper
limitstoat whichour
survey couldlevel)
detect for rates
Fig. 10.ofUpper
to the volumetricrates of GRBs with bright prom
Table
5.the
Upper
limits(95%
confidence
verylimits
luminous
sources.
accept(Sako
et redshifts
al. 2018);
so
one
might
say thatthe 0.5-s
expoprompt optical flashes from GRBs. (Color online)
optical flashes.
sures we studied ought to have a limiting magnitude of
V = 12.6
V = 13.6
V = 14.6
V = 15.6
V = 17.7. However, since our search was often conducted−1 ) is52
When weIf setof
A so that
optimally
the
of1.0
one
progenitor
may provid
Lin
(erg
sthan
greaterthanthe model× a10more
2.5properties
× 1052× type1052 of GRB
4.0 ×
1051
lessvalue
optimalconditions,
we6.3
take
conservaγ theaccept−3−1
matches thethen
gamma-ray
opticalof the thealimiting
rayof hope.
rate(Gpc andyr this) ispaper.
lessobservations
than
3700
4000
5800
tive
approachin
In order to 3600
calculatethree comparison
events (to
an we
order
of magnitude
TheNrate at which short GRBs (Berger 2014) occu
magnitude
forwithina chunk,
begin
by countinginthe number
-3
-1
52
−1
of “good”
imageswithinthe10chunk.
This
is normally
close
erg
s
.
This
all
cases),
wederive
a
value
of
L
has
been
estimated
atroughly∼
1–10
per Gpc3 per yea
γ = 6×1 2 3 4 5 6 7 8 9
to 360,
but may
be smallersome frames
implies that events
similarto thosein the if
comparison
set are rendered(Wanderman & Piran 2015), although a few authors sug
population of objectsunusable
which give
rise
to
them,
our
surveyPi of the Sky (Sokolowski 2008; Obaraet al. 2014)by clouds,
seeing,passing
airplanes, gestor otherwould
be detected to redshiftsz > bad9 evenfor ourbrightest
higher values of ∼ 10–100 per Gpc3 per year (NakaFig. 4. Examples of sequences of images with detections (filled
rectanbecomessomewhatmore
relevant.
Thecompareclass ofthe
short
GRBs
sists
of 2006;
one system
Chile,
two 31camegles) and non-detections (empty rectangles), andour algorithm’s
deciproblems.
We thennumberof images
in whichetal.
Guetta in& Atacama,Piran2006).
Even withthe higher
end ochoiceof magnitude
limit.
短時間スケール突発天体のサーベイ観測
第32回
理論懇シンポジウム「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ@2019/12/25-27
Examples of accepted and rejected transients<==> 10^1 [Gpcsion at the right. (Color online)

yr ] (sGRB)Fast Radio Burst (FRB)
still unknown origin / many many theories proposedradio survey projects
Parkes (SUPERB), ASKAP, CHIME, Molonglo (UTMOST), VLA (realfast), …
some repeating FRBs (FRB 121102, FRB 180814)
some host galaxies identified (FRB 150418@z=0.492, FRB 121102@z=0.193),
several from ASKAP
no optical detections so far
an “interesting” candidate w/ Subaru/HSC (Tominaga+2019)
Tomo-e & CHIME (Canada) coordinated simultaneous observations?

短時間スケール突発天体のサーベイ観測

https://chime-experiment.ca/frb

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

32

Opt/Radio simultaneous obs. For a repeating FRB121102
2804

L. K. Hardy et al.

optical: ULTRASPEC on Thai National
Telescope (2.4m), 70.7 msradio: Effelsberg Radio Telescope (100m)
13 bursts detected in radio<==> No bursts detected in optical
Optical limit: 0.33 mJy @767nm==> < 0.046 mJy ms fluence==> alpha < -0.2
Similar trial w/ Kiso/Tomo-e Gozen &Yamaguchi radio telescopes (山口トモエ)
FRB location

A search for optical bursts from FRB 121102

comparison star

2805

Downloaded from https://academic.oup.com/mnras/arti

Figure 2. ULTRASPEC light curves of FRB 121102 showing the sky-subtracted counts per pixel as a function of time. The sub-plots on the right-hanshow a zoomed-in view of the light curves close to the arrival times of a sample of the Effelsberg radio burst detections. The occasional short peri
larger scatter are likely due to the increase in sky noise during passing cloud cover. The dashed line shows the 5σ level for each light curve, where σ
standard deviation in the counts. Red stars show the single ULTRASPEC measurements for the frames closest in time to the simultaneous Effelsberg
burst detections. Blue stars represent the summed optical flux (counts pixel−1 ) from the two temporally closest frames to a radio burst detection, in ca. Stacked images consisting of 22 ULTRASPEC frames observed at the same time as the 12 Effelsberg radio bursts. The left image isburst
centredonspreadthe across two frames. The single blue data point at the right-hand side of each plot represents the stacked flux (counts pixel−1 ) from all
may bein each run. Theoferror bar is the 1σ error in this value. Two bursts (the second and third observed in the third observing run) were observed just 34 ms a
position of FRB 121102, while the right image is centred on the comparison star PSO J053154.854+330815.385. The full width at half-maximum

短時間スケール突発天体のサーベイ観測

Hardy+2017

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

33

© K. Kashiyama

2 Hz monitoring of
known whitedwarfsshort periodicity?

短時間スケール突発天体のサーベイ観測
第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27
http://www.ioa.s.u-tokyo.ac.jp/kisohp/RESEARCH/symp2019/index.html

34

Occultation of a star by a Trans-Neptunian Object©ARIMATSU, Ko

occultation observations of known asteroids
simultaneous observations at multi-sites
size, shape, atmosphere, comet-like activity,
ring, satellite etc.
“movie”: an occultation of a star by a TNO, Quaoar
w/ Kiso/Tomo-e gozen==> almost no atmosphere (< 16 nbar)(Arimatsu+2019b)

ring discovery (Braga-Ribas+2014)

http://www.ioa.s.u-tokyo.ac.jp/kisohp/NEWS/quaoar2019/quaoar2019.html

短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

35

Occultation survey for unknown asteroids©ARIMATSU, Ko

occultation survey w/ two 0.28-m telescopes (OASES) at Miyako-Jima Island
discovery of a small-size (r < 10 km) Kuiper-belt (Arimatsu+2019a, Nature
Astronomy)
discovery of “Oort Cloud” objects?
first discovery of an occultation event candidate by a small-size (~1 km radius)
TNO (Arimatsu et al. 2019a, Nature Astronomy, 3, 301)

短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

36

calculated. The fractions of the meteors which might pass through within
3! of the radiants were at most 6% and 3% for April Lyrids andη-Aquariids, respectively. These fractions were consistent with thenumber of sporadic meteors randomly coming from the radiants. We

Meteor (Ohsawa+2019)

ere extracted from the movie data cube with theTomo-e Gozen prototype (PM)
8 sensors = ~2 deg2 FoV
2 Hz readout
2 nights in 2016
1514 & 706 sporadic meteors
absolute magnitude: +4 - +10 mag
mass: 8.3x10-2 - 3.3x10-4 [g]LF slope: r=3.1+/-0.4
R. Ohsawa et al.

Planetary and Space Scie

Fig. 6. Comparison of luminosity functions obtained in different observations. The present result is indicated by the blue region. (For interpreta

he number of meteors and the magnitude zero-point. The periods of cloudy weather are indicated
the
green
hatchedregions.
The gray
to colour inby
this
ﬁgure
legend,the reader
is referredto the Web version of this article.)n no data due to pointings or troubles. (For interpretation of the references to colour in this ﬁgure legend, the reader is referred to the Web

短時間スケール突発天体のサーベイ観測

4.3. System efﬁciency comparison between Tomo-e PM and Tomo-e Gozen

on the elevation angle α. The EMCAs at zenith are37
第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ
System 1, 2, and 3, respectively. At α ¼
630km2 for@2019/12/25-27

Meteor: optical + radio@R. Ohsawa, Kiso Schmidt Symposium 2018
http://www.ioa.s.u-tokyo.ac.jp/kisohp/RESEARCH/symp2018/
短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

38

New CMOS multi-band
cameraon Seimei(3.8m)
多色カメラ+ 近赤外装置
概念図
近赤外装置
NIR
せいめい望遠鏡 多色カメラ

detector(CMOS)
検出器
detector (CMOS)

tel.
望遠鏡
detector
検出器
focus
焦点面

optical多色カメラ
multi-band

多色カメラ

インストルメント
ローテータ

検出器
detector(CMOS)

field-of-view: 6.4 x 11.3 arcmin2
FY2020 first light w/ partial spec.
FY2021 spectroscopic mode?

©Matsubayashi, Ohta
短時間スケール突発天体のサーベイ観測

sensitivity (S/N=5)- 3-band (g, r, i) simultaneous imaging~ 18 mag (10 Hz)~ 16 mag (100 Hz)- spectroscopy (R~500)~15 mag (1 Hz)~13 mag (10 Hz)

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

39

CMOS Suprime-Cam on Subaru telescope (8.2m)
CMOS specifications / performance
2,560 x 10,000 pixels (7.5 um square pixel)
Full well ~ 30,000 e
readout noise: 2 e, dark current: 90 e/s/pix @ 300 K~10 Hzfuture plan: put 10-sensor camera to prime focus of Subaru (similar FoV
to Suprime-Cam; ~size of the moon)©Miyazaki, Komiyama

September 2, 2019 @ Hiroshima

短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

40

Summary
Optical transient sky in a time scale of days has been
explored since discovery of acceleratedly expanding universe
with Type Ia supernova observations (late 1990’s).
Recently, 1-day or shorter time scale transient have been
discovered and studied.
Wide-field optical surveys in a time scale of seconds (orshorter) have been started.
Kiso/Tomo-e Gozen survey
2 Hz (“flash”, HeSO, occultation, meteor) - 200 Hz (pulsar)
Please join us, Tomo-e Gozen Science WGsrequests: Please
propose science cases requiring high-cadence observations
think about a theory explaining/predicting second-scaletransient phenomena in optical.

短時間スケール突発天体のサーベイ観測

第32回 理論懇シンポジウム 「天文学・宇宙物理学の変遷と新時代の幕開」@NAOJ @2019/12/25-27

41