Synergy between
Wide Field Transient Survey
and 3.8m Telescope- 広視野サーベイと連携した3.8m望遠鏡による突発天体観測 -Masaomi Tanaka(National Astronomical Observatory of Japan)
Tomoki Morokuma (U. Tokyo), Nozomu Tominaga (Konan),
Shigeyuki Sako (U. Tokyo)
on behalf of KISS collaboration

• Synergy with High-Cadence Survey• Synergy with Gravitational Astronomy- Low resolution spectrograph (ready to use anytime)- Flexible operation/instrument exchange2Survey area (deg )10000

PS (wide)
CRTS
PTF
La SillaSkyMapper
1000
PTFSDSSPS(deep)
ROTSE
100KISS
SNLS
1010.10.01<1d1-5 d>5d18 19
LOSS
CHASE

20

HSC
GOODS

21 22 23 24 25 26 27
Limiting magnitude (@6000A)

16Magnitude

18

ROTSE

20

KISS 1m

22

PTF 1m

24

PTF

PTF

SDSS
Pan-STARRS
SNLS

26

HST

HSC

Deep

28
0.01

2013

High
cadence

0.1

110Cadence (days)100

de from now, that we were not sufficiently imaginative.
Theoretically expected
Supernovae

Nova

2.

Figure from LSST Science Book
(afterPTF physicallycollaboration, Rau+09,Kasliwal+,Kulkarni+)
Theoreticalandplausible
candidates aremar

KISS: Kiso Supernova Survey• Extremely high cadence

Kiso 1.05m Schmidt telescope• 1-hr cadence <= 2-3 days
• 4 deg FOV (KWFC)• ~ 20-21 mag in g-band
2(3 min exposure)•~50-100 deg2 /day
(SDSS fields, high SFR)

• ~100 nights /yr• Automatic data reduction
Goal: Detection of shock breakout of supernovae

The Astrophysical Journal, 757:31 (10pp), 2012 September 20

Bolometricradioactive
power
Bersten+12Figure 10. Bolometric LCs (left panel) and g ′ -band LCs (right panel) for models with the same explosion
The observed bolometric LC (M. Ergon, in preparation) and g ′ -band LC (Arcavi et al. 2011) of SN 2011dherror bars indicate the size of the systematic uncertainty that corresponds to an uncertainty of 1 Mpc in theattaching essentially massless (<0.01 M⊙ ) envelopes to the He4 model. Larger radii produce higher early lat later times.
(Talks by Yamanaka-san and Maeda-san)(A color version of this figure is available in the online journal.)

The 1st day of the SN = memory of stellar radiusConnection between stellar evolution and SN

~80 SN candidates (as of 2014 May)
KISS12a

KISS12f

KISS12k

KISS13a

KISS12b

KISS12g

KISS12l

KISS13b

KISS12c

KISS12h

KISS12m

KISS13d

KISS12d

KISS12i

KISS12n

KISS13j

KISS12e

KISS12j

KISS12q

KISS13l

Follow up spectroscopy

No shock breakout yet(Success rate of spectroscopy ~ 25 %)Morokuma+14Fig. 10. Identification spectra for the CBET-reported KISS SNe except for SN 2014U which is shown inFigure 11. Flux density (fλ ) scale is in arbitrary unit. Observed and template spectra are shown in black

NOT 2.5m

OAO 1.88m

Hiroshima 1.5m
TNG 3.6mFollow up with 3.8m telescope
Spectroscopy with R ~ 500
for 20-21 mag(rapid response is a key)
WIYN 0.9m

Akeno 0.5m

HCT 2mSwope 1m

Lulin 1m

• Synergy with High-Cadence Survey• Synergy with Gravitational Astronomy- Low resolution spectrograph (ready to use anytime)- Flexible operation/instrument exchangeNew astronomy with gravitational waves
2017 - Advanced LIGO (US)- Advanced Virgo (Europe)- KAGRA (Japan)

KAGRA

NS-NS merger
with 200 Mpc~ 30 events/yr(~0.3-300)

C: NASA2 deg

Kiso 1m
Schmidt telescope(KWFC)~ 200 galaxies / 4deg2(< 200 Mpc)

GW alert error boxe.g. 6 deg x 6 deg~ 2000 galaxies(< 200 Mpc)

No electromagnetic counterpart
No gravitational wave astronomy

2 deg

Optical/Infrared emission from NS merger
Numerical relativity

Radiative transfer

Hotokezaka et al. 2013

MT & Hotokezaka 2013

18KISS19

NS merger @ 100 Mpc

Magnitude

2021

soft EOS

2223
24
25

stiff EOS
051015Time (days)

Best with red edge of optical (i band, 0.8um)

Bright models are consistent
with GRB 130603B

terglow21 and the host galaxy22 were

12110
X-ray

10–11

F606W
22F160W

AB magnitude

2310–122425
10–13

26

X-ray flux (erg s–1 cm–2)

f the merger of two neutron stars or athe production of a kilonova (some’ or an ‘r-process supernova’) due to
produced and initially ejected duringrds, an event similar to a faint, shortculations suggest that the spectra oftermined by the heavy r-process ionserial. Although these models10–13 area robust conclusion is that the opticaly line blanketing in the rapidly expanmerging instead in the near-infrareda longer timescale than would othervious NIR
limits on
early optical kilonova
sourceally, the NIR light curves are expecteda few days and lasting a week or moremodest redshift and intensive study of
didate for searching for such a kilonova.
he burst with the NASA/ESA Hubble
epochs, the first ,9 d after the burst
fter the burst (epoch 2). On each occas obtained in both the optical F606W
W filter (1.6 mm) (full details of the imagcussed here are given in Supplemenges are shown in Fig. 1; the key result isTime since GRB 130603B (d)

2728

10–14

29
104

105
106
Time since GRB 130603B (s)Figure 2 | Optical, NIR and X-ray light curves of GRB 130603B. Left axis,Tanvir+13
optical 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 Berger+13
band andVery red (R-H > 2.5 mag)r each15
ande thanWdeds
andrsionsarambabiligherLAL rameample
inningNFER
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mplete,showsmallr bothructed15maps
andoLatiW
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ample
ly tooNFER
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on,forshow
confismall-

50% CR 100 deg2
31%
37%
31%
72%
smaller than 200 deg2
Table
74% 1
80%
59%
90%
Summary of the 2015
listing
detectors,
500 anddeg22016 scenarios,
100%
100%the participating
99%
100%
BNS horizon distance,run2 duration, —and fractionsof events2%
localized within
5 deg
—
2%
2
5, 20,
100, 200, or 5002 deg . A dash (—) represents less than 1% of
fraction
20 deg——11%
14%
detections.
90% CR 100 deg2
2%4%
16%
32%
smaller than 200 deg2
9%
13%
21%
44%
Singer et al. 2014
2015
2016
500 deg2
42%
48%
38%
72%
Detectors
5 deg2
3% HL
4%
10%HLV 20%
fraction BNS range
54 Mpc 19%
108 Mpc 43%
20 deg2
14%
23%
searchedRun duration
23 months 54%
6 months 70%
100deg45%
45%
area smaller
No. detections
264%0.091 70%
62% 1.5 80%
than 200 deg
rapid
full89%PErapidfull92%PE
500 deg2287%82%(5 deg11%
14%222250%CR2 142 deg—
124 deg—
164 deg
43 deg20 deg
2%3%
16%
35%
2222
medianfraction
area
90%
CR2 573 deg
529 deg
646 deg
235 deg
50% CR 100 deg
31%
37%
31%
72%
2222
searched2 122 deg
88 deg
129 deg
32 degsmaller than 200 deg
74%
80%
59%
90%
500 deg2
100%
100%
99%
100%
Horizondistance~
50-100Mpc
2
5 degto following— up 9%— of all 2%2%that this corresponds
GW
detec211%2
Localization~
200degfraction
20deg
——
14%
tions. On the other hand,
one
might
decidetoalwayssearch
90% CR 100 deg2
4%
16%
32%
2 2%the smaller
most probable200degarea
forevery
GWevent,
correthan
200 deg2with 9%
13% telescopes
21%
44%
Widesurvey
1mclass
sponding to a different
confidence
level
for every
event. 72%In
500 deg2
42% 2
48%
38%
with
KISS)
2strategy
this case, (Similar
one would
2003%
deg ontheof
5 degfind
4% horizontal
10% axis20%
fractionarea histogram,2
the searched
and
find
that
thisstrategy
would
20
deg
14%
19%
23%
43%
Spectroscopy
with
3.8m
telescope
searched18
2
enclosethetruelocationoftheGW
source64%
ofthetime.
45%
54%
45%
70%
area smaller 100 deg2~panels500)
degof all (R64%70%
80%
The left-handaxes
fourof Figure62%
3 show thethan 200

Early observing runs of GW detectors## 2015-2016 ##2

Log flux (Fh) + constant

UBVRI
65

J

Type Ia

H
1.5 days
5.0 days10.0 days

43
2
15000

10000
15000
Wavelength (A)20000- Very red SED (peak at NIR)
- Extremely broad-line (feature-less) spectra
Spectroscopic identification is essential
Matsubayashi-san’s talk“Drill” with Fermi/GBM alert< 3 hr after the alert

12.5 deg

01122222212022

1

revised position
1(3.3 deg)

1alert position(2.7 deg)1< 1 hr after the alert

possiblecounterpart(by PTF)

by Tomoki Morokuma

Current Status of Conceptual
DesignStudy- Future -CMOS
for
Kiso
Schmidt
telescopest

The 1 generation wide-field CMOS camera• No need to cool
• Fast readout (30 Hz)

480 mm35mm Full HD CMOS sensor

x 84 chips
530 mm

KWFC
KWFC-CCD

Photo plate

190 Mpixels
Large FOV Ω
760 MB/exposure•Totalsky coverageobservation
20 degf• Efficient• High cadence2ĭ500 mm = ĭ8.7 deg
vignetting 0.44mag

ĭ225 mm = ĭ3.9 deg
vignetting free areasensor / package area = 0.3Survey power= fAΩ

Institute of Astronomy, The University of Tokyo

By courtesy of Shigeyuki Sako (PI),Soya Todo, Yuki Kikuchi, et al.

c.f. Zwicky Transient Factory (large format CCD)GW alert error box
e.g. 6 deg x 6 deg

Kiso/CMOS~9 deg
2 deg

Summary• High-cadence transient survey

with 1m telescopes• Survey=> Spectroscopy with 3.8m telescope• Gravitational wave astronomy• Identification of electromagnetic counterpart
observing runs => GW events @<100 Mpc• Early=> Spectroscopy with 3.8m telescope• Future

FOV, higher cadence,• Widerand more efficient observations- Low resolution spectrograph (ready to use anytime)- Flexible operation/instrument exchange