Prompt follow-up observations of transients- Toward SN shock breakout detection 超新星爆発ショックブレイクアウトの検出に向けた突発天体の即時フォローアップ観測

Masaomi Tanaka (NAOJ)
on behalf of KISS collaboration
Tomoki Morokuma (U. Tokyo), Nozomu Tominaga (Konan),
Nobuharu Ukita (NAOJ), Emiko Matsumoto (Konan),
Katsutoshi Takaki (Hiroshima), Masayuki Yamanaka (Konan),and many collaborators

Bolo1042

3 -1
Bolometric luminosity[ergs ]
Photosphericvelocity [10km]

GA ET AL.

1010458104461043
41042
2

Bolometric luminosity [erg s-1]

1041045

1010510451044

44104301043

0.2Days

0.6
0.4Vol. 0.6705

Shock breakout

1044
10104350104100.41045

10500.201042

Color temperature [K]105ric velocity [103 km]

Color temperature [K]progenitor starTOMINAGAET AL.moment of SN explosion Vol. 705
The first

20

40

0.2
0.4
0.6
Tominaga+09

0.660

100

00.2

0.4

80

Supernova

emperature [K]> a few days
Figure10
3. Bolometric LC (top), color
temperature evolution (middle), and510- Probeof progenitor’sstellar
photospheric velocity
evolution (bottom)of the SN IIP model (lines).
The insets radius
6 panels enlarge the phase of shock breakout.
in the top and middle
30- Probe of high-z Universe
58Days since the peak (rest frame) [Days]

KISS: Kiso Supernova Survey(2012 Apr - 2015 Mar)

• 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
Expected number of detection ~1 / yr

16Magnitude

18ROTSE

20KISS 1m22

PTF 1m24PTF

PTFSDSS
Pan-STARRS
SNLS

26HSTHSCDeep

280.012013

Highcadence

0.1110Cadence (days)

100~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

NOT 2.5m

OAO 1.88m

Hiroshima 1.5m
TNG 3.6m

Spectroscopy in the same night!
NOTE: Non-ToO observation!
(we ALWAYS have SNe)
Weather is the major factor of success
WIYN 0.9m

Akeno 0.5m

HCT 2mSwope 1m

Lulin 1m

Status

13B: 4 nights(1-2 night/month)

2013/9 (2 nights)
Kiso

5OAO-

67891011

12

Pointing trouble (Kiso)--

Spectroscopy of 19-20 mag
SN candidates(not from KISS)=> 2 IAU/CBET circulars

GoodModerate

Bad

OAO SkyMonitor

OAO SkyMonitor

OAO SkyMonitor

Status

13B: 4 nights(1-2 night/month)

2013/9 (2 nights)
Kiso

5OAO-

6789101112

Pointing trouble (Kiso)--

Spectroscopy of 19-20 mag
SN candidates(not from KISS)=> 2 IAU/CBET circulars

67

2013/10 (1 night)
Kiso

30

1OAO--

234-

5-

-

2013/11 (1 night)
Kiso

30

31

OAO--

123456-

Spectroscopyon the discovery day(but unable to identify)

Status

14A: 13 nights (1-4 nights/month)

Good Moderate Bad
2014/1-2 (1 night)
Kiso

26

27

28

29

OAO

----

30

31

12--

3

4

Unable to identify
due to low S/N

2014/2-3 (3 nights)
Kiso

25

26

OAO--

27

28

12-

2014/3-4 (2 nights)
Kiso

28

2930

31

123OAO4-

2014/4 (4 nights)
Kiso

24

OAO

2014/5 (3 nights)

25

Kiso

24

25

OAO

--

26

26

27

27

28

28

29

30

1--

29

30

31---

Spectroscopyon the discovery day(but unable to identify)
1st identification of KISS SN(2 days after the discovery)

2nd identification of KISS SN(8 days after the discovery)15 IAU supernovae

KOOLS(g ~ 19 mag)Fig. 9. Identification
spectra for Tominaga,
the CBET-reported
KISS SNe
except for SN to2014U
which is shown inMorokuma,
MT+14,
submitted
PASJ
Figure 10. The flux density(fλ )survey
scale has arbitraryunits.
Observedandresults)
template spectra are shown in(KISSstrategy
andinitial

~80 SN candidates (as of 2014 May)
KISS12a

KISS12f

KISS12k

KISS13a

KISS12b

KISS12g

KISS12l

KISS13b

KISS12coN
KISS12d
KISS12etey
KISS12htuokaerbkcsho
KISS12m

KISS13d

KISS12i

KISS12n

KISS13j

KISS12j

KISS12q

KISS13l

Science under moderate weather condition- Tomography of SN ejecta SN 2014C in NGC 7331

4 days8 days17 days

Kanata~ 16 mag

Outerejecta(opt. thick)30 days
150 days
Takaki et al.

KOOLS~18 mag

Innerejecta(opt. thin)

Subaru300 days ~ 23 mag
Project led by Katsutoshi Takaki (Hiroshima)

Tanakaet al.
Tanakaet al.

SDSSSDSS

N

N

19.019.0

20032003 20142014

EE

19.519.5

Magnitude

Magnitude

KISS
KISS

1’gB

spectroscopy

20.020.01’

EpochEpochg
1 2 31 2 3B

x3

20.520.5
21.021.0
21.521.5

1 day

22.022.0
22.522.5

19.019.0

2003
2014
2003
2014

-10-10 1
1 22 3
MJD-56711.0(2014-02-23UT) UT)
MJD-56711.0(2014-02-2334

Tanaka et al.
Observed wavelength (A)
6000
7000
8000

Epoch 1
Epoch 2
Epoch 3Mg II

HβAGN!
3000[O III]HβHγ[Ne III][Ne III]

Mg II

02500

[Ne V]

5-3 -2 -1 0 1 2 3
3-1
Velocity (10 km s )[O II][O III]
5007

Flux fλ (103500
40004500
Rest wavelength (A)

5000

10I]

-17-2 -1-1erg cm s A )109000[O III]

5000

By
J110
poweemisstrengLabia
relateArcradioalogs
NLS
J110
loudnand Yfν (4rest fwherewavel(2008-10

123

MJD-56711.0 (2014-02-23 UT)

Follow-up observations: optical/radio/X-ray
19.0
2003

2014gB
Rc
J+2.0

19.5

Magnitude

20.0

Kanata/HONIRMITSuME

20.5
21.0

OAO/KOOLS

21.5
22.0
22.5
-50

5

10
15
2025
MJD-56711.0 (2014-02-23 UT)

30

3540

Extremely radio-loud AGNs with
- M ~ 10 -10 Msun
- L ~ LEdd
ge 2000). NLS1s=>
account
about 14 % of broad-line
radio-loudsources forSMBH
NLS1s is small, i.e., only 7
Relativistic
jetsin“growing”
Ns when AGN samples are selected with optical specNLS1s have R > 10 (2.5 % for R > 100) while aure 1. Upper left: Discovery image of SDSS J1100+4421 taken with Kiso/KWFC (stacked data on 2014 Feb 23 UT) compared
SDSS image taken in 2003. Upper right: Light curves of SDSS J1100+4421 around the discovery epoch. The vertical arrows inw the epochs of spectroscopic data. Lower: Long-term
multi-color (gBRc J) light curves of SDSS J1100+4421. In the light cu58
photometric data are comparedBHwith SDSS g-band magnitude and B- and Rc -band magnitudes estimated from SDSS magnitude
el and shaded region). Magnitudes are given in AB magnitudes for the SDSS g band and Vega magnitudes for the other bands.

copy MT,(ZhouMorokuma,et al. 2006). Theyshow
a lu20Saito% of broad-line
Seyfert1 galaxies haveR > 10 (Itoh,typically
Akitaya,Tominaga,et al. 2014,submittedto ApJ
osity close to the Eddington luminosity. It is now
for R > 100, Komossa et al. 2006). Thus, it had

Summary• KOOLS spectroscopy for KISS
• Observations on the same night• Identification of 2 KISS SNe (19-20 mag)
• No SN shock breakout yet• Ongoing work/Future plan
• Survey until 2015 Mar• 16.5 nights for 14B• Coordinated observations with Kanata/Subaru(4+13 nights in 13B/14A)* Morokuma+14, submitted to PASJ (KISS initial results)* MT+14, submitted to ApJ (flare in an unusual AGN)