Transient Sciencewith Wide Field Survey
and 3.8m Telescope- 広視野突発天体サーベイと3.8m望遠鏡によるサイエンス -Masaomi Tanaka
田中 雅臣(National Astronomical Observatory of Japan)
On behalf of KISS collaboration
Tomoki Morokuma (Univ. Tokyo)
Nozomu Tominaga, Kensho Mori (Konan Univ.)• Frontier of Transient Survey• KISS (Kiso Supernova Survey)

and Synergy with 3.8m Telescope• Future PlanStellar Evolution - Supernova

1

6.5
100

LBV

80

6.0
30

5.5

25

WR

log L/L60
5040

C: Ohio StateUniversity

20

5.0

16

4.5

1210

4.0
3.5
5.5

86

Smartt+09
5.0RSG4.5log Teff

4.0

3.5

Solar metallicity
LMC metallicity

08kr

93J11dhLuminosity

08cn

RSG
Maund+11

Temperature

Fig. 4.— Hertzsprung-Russell diagram showing the luminosities and temperatures of the progenitors of SNe 2011dh ( ), 1993J (⌅; Maund et al. 2004;
Aldering et al. 1994), 2008cn (•; Elias-Rosa et al. 2009), and 2009kr (N;Fraser et al. 2010b; Elias-Rosa et al. 2010). Overlaid are stars stellar evolu-Lewi
Li, W
X.
Li, W
Li, W
J.
Maı́z
MassScMattDa
Maun
Maun
Maun
G.
Menz
Mutc
Ab
Pasto—. 2Phill95
Reila
BuScheThe Astrophysical Journal, 757:31 (10pp), 2012 September 20

Adiabaticcooling

3 day

Bolometricradioactive
power
Bersten+12

Figure 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 l

Too late with typical 2-3 day cadence7.5 Shock Breakout

UV100

Apparent g’ magnitude [mag]SN shock breakout

progenitor starz=0.2 z=1.5 z=2.5
z=0.5 z=2 z=3z=1

22

24

Breakout

1 day !
26

28

00.5

1

1.5

> a few days

Days since bolometric peak (observer frame) [Days]
Figure from N. Tominaga

GALEX and SNLS observations (points, SNLS-04D2dc,51
erg reddened for the hosts = 20M! and E = 1.2 × 10mag (lines, Tominaga et al. 2009) (black and red: near UV,t enlarges the phase when the SN emitted UV light. (Right):
B magnitude system for a SN IIP model with Mms = 40M!

Star formation tracer
at high redshift

Figure from T. Morokuma

16Highcadence

Magnitude

18

ROTSE

20

KISS

22

iPTF

PTF

SDSS
Pan-STARRS

24

SNLS

26

HSTHSC

Deep

28
0.01

PTF

0.1

110
Cadence (days)

100• Frontier of Transient Survey• KISS (Kiso Supernova Survey)

and Synergy with 3.8m Telescope• Future Plan

KISS: KIso Supernova Survey• Extremely high cadence• 1-hr cadence• 4 deg FOV• 3 min exposure• ~ 21 mag in g-band• ~50-100 deg /day
• 100 day observations/yr (around new moon)• High SFR field (< 200 Mpc, 30-100 Msun/yr)
222012 Apr: Dry run 2012 Sep: Main survey -KISS 1st year
No of visits

Kiso observatory

Anywhere

KISS pipeline

cut-out images
Refstandard reduction

image subtraction
source detection< 10 min~ 50GB/day
cut-out images
RefNewSubNewSub

KISS databasesourceinfo

KISS interface

KISS databasesourceinfoAmateur astronomers

37 SN candidates
KISS12a

KISS12f

KISS12k

KISS13a

KISS12g

KISS12l

KISS13b

SN 2012cq
KISS12b

SN 2013ISN 2012cm
KISS12c

KISS12h

KISS12m

SN 2013JSN 2012ct
KISS12d

KISS13d

KISS12i

KISS12n

KISS13j
SN 2013Y

KISS12e

KISS12j

KISS12q

KISS13l
SN 2013??

NOT 2.5m (3)Kiso 1m

Hiroshima 1.5m (1)TNG 3.6m (3)Follow-up collaboration
Akeno 0.5m
HCT 2mWIYN 0.9m

Swope 1m

KISS collaboration• Survey members• Tomoki Morokuma (PI), Nozomu Tominaga, Masaomi Tanaka,Kensho Mori, Koji Kawabata, Yoshihiko Saito, Nobuharu Ukita,Michael Richmond, Yuji Urata• Indian Institute of Astrophysics• Devendra Sahu

• Carnegie Supernova Project (CSP)• Eric Hsiao, Maximilian Stritzinger, Mark Phillips, Nidia Morrell,
Carlos Contreras, Francesco Taddia• Telescopio Nazionale Galileo (TNG)• Paolo Mazzali, Emma Walker, Elena Pian

• SNFactory• Greg Aldering• Russian Institutes• Dmitry Tsvetkov, Nikolay Pavlyuk

Synergy with 3.8m Telescope• Rapid follow up• High speed pointing of 3.8m telescope iscritical (1 min, Nagata-san, Kurita-san)• Rapid communication (< 1 hr)

Target feed takes ~ 10-60 min• Automatic response• Low resolution spectroscopy(R~500, v~500 km/s)• IFU is preferred (Ota-san, Matsubayashi-san)confirmation image + spectroscopy
占有性•機動性が最も重要な要素

No Transient Left BehindBy-products fromhigh-cadence survey• Variable QSO

SDSS

g=22.6 mag• ~ 110• Variable stars

80• ~(HighGalactic latitude)• Rapid flare (< 1hr)•

~ 5 (after Maehara et al. ...)(High Galactic latitude)
Nogami-san’s talkSpectroscopy during the flare!?

21:01>20.8 mag

1hr
22:01

19.0 mag

1hr23:09>20.1 mag• Frontier of Transient Survey• KISS (Kiso Supernova Survey)

and Synergy with 3.8m Telescope• Future Plan

Gravitational Wave Electromagnetic Wave Astronomy• KAGRA 2017• Neutron star merger

C: KAGRA• 1-10 events / yr

• EM counterpart
Ota-san’s talk

C: NASAThe Astrophysical Journal, 746:48 (15pp), 2012 February 10with specific stellar populations). Because merger counterparts
are predicted to be faint, obtaining a spectroscopic redshift
is challenging (cf. Rowlinson et al. 2010), in which case
spectroscopy of the host galaxy is the most promising meansof obtaining the event redshift.
It is important to distinguish two general strategies for connecting EM and GW events. One approach is to search for aGW signal following an EM trigger, either in real time or ata post-processing stage (e.g., Finn et al. 1999; Mohanty et al.
2004). This is particularly promising for counterparts predicted
to occur in temporal coincidence with the GW chirp, such as
short-duration gamma-ray bursts (SGRBs). Unfortunately, mostother promising counterparts (none of which have yet been
independently identified) occur hours to months after coalescence.6 Thus, the predicted arrival time of the GW signal willremain uncertain, in which case the additional sensitivity gained
from this information is significantly reduced. For instance, if
the time of merger is known only to within an uncertainty of∼ hours (weeks), as we will show is the case for optical (radio)
counterparts, then the number of trial GW templates that must
be searched is larger by a factor ∼104 –106 than if the merger
time is known to within seconds, as in the case of SGRBs.
A second approach, which is the primary focus of this paper,
is EM follow-up of GW triggers. A potential advantage in thiscase is that counterpart searches are restricted to the nearby
universe, as determined by the ALIGO/Virgo sensitivity range(redshift z ! 0.05–0.1). On the other hand, the large error
regions are a significant challenge, which are estimated to betens of square degrees even for optimistic configurations of GW
detectors (e.g., Gürsel & Tinto 1989; Fairhurst 2009; Wen &Chen 2010; Nissanke et al. 2011). Although it has been argued
that this difficulty may be alleviated if the search is restricted
to galaxies within 200 Mpc (Nuttall & Sutton 2010), we stressthat the number of galaxies with L " 0.1 L∗ (typical of SGRB
host galaxies; Berger 2009, 2011) within an expected GW error

Metzger & Berger

EM signature from
NS-NS merger•

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

Ejecta ISM ShockRadio (years)

GRBobs(t ~ 0.1 1 s)

Kilonova

Optical (t ~ 1 day)On-axis short GRBjMerger Ejecta
Tidal Tail & Disk Windv ~ 0.1 0.3 c• very rare

BH

• Off-axis radio emission

Metzger & Berger 2012,
Figure 1. Summary of potential electromagnetic counterparts of NS–NS/ApJ, 746, 48
NS–BH mergers discussed in this paper, as a function of the observer angle• delayed (~1 yr)• no guarantee of association

θobs . Following the merger a centrifugally supported disk (blue) remains aroundthe central compact object (usually a BH). Rapid accretion lasting !1 spowers a collimated relativistic jet, which produces a short-duration gamma
ray burst (Section 2). Due to relativistic beaming, the gamma-ray emission
is restricted to observers with θobs ! θj , the half-opening angle of the jet
Non-thermal afterglow emission results from the interaction of the jet withthe surrounding circumburst medium (pink). Optical afterglow emission isobservable on timescales up to ∼ days–weeks by observers with viewing anglesof θobs ! 2θj (Section 3.1). Radio afterglow emission is observable from alviewing angles (isotropic) once the jet decelerates to mildly relativistic speeds
on a timescale of weeks–months, and can also be produced on timescales oyears from sub-relativistic ejecta (Section 3.2). Short-lived isotropic optica
emission lasting ∼few days (kilonova; yellow) can also accompany the merger
powered by the radioactive decay of heavy elements synthesized in the ejecta(Section 4).
(A color version of this figure is available in the online journal.)• “kilonova” (macronova)• could be common if r-process occurs

Neutron star merger @ 200 Mpc
17KISS

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Magnitude

192021Soft EOS

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q=0.9

24 Realistic simulation
25by MT, Hotokezaka+

0.1

1Days after the explosion

10

2 deg

GW alert error box
10 deg x 10 deg(for example)

6 deg

Localization with
Schmidt telescope
Spectroscopy with
3.8m telescope

2 deg

25 pointing=> 2-3 hr
0.3 deg

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Transient Science with 3.8m Telescope• (Need wide field survey) Kambe-sanfollow up for• Rapid
high-cadence transient survey• Shock breakout of supernovae• Rapid flare• Critical role in GW-EM astronomy• 3.8m Telescope + 1m Schmidt (wide field)• Hope for 3.8m Telescope• Low resolution spectroscopy (R~500)• IFU (image and spec, reducing time loss)• Rapid communication/automatic response