High-Cadence Transient Survey with
Kiso/Tomo-e Gozen and Spectroscopic
Follow-up with Seimei/KOOLS-IFU

諸隈 智貴 (東京大学) ==> 田中 雅臣 (東北大学)
Tomoki Morokuma (Univ. of Tokyo/IoA)==> Masaomi Tanaka (Tohoku Univ.)

Contents
New Parameter Space: High Cadence Transient Surveys
Kiso Schmidt telescope & Tomo-e Gozen
Northern Sky Transient Survey w/ Tomo-e Gozen
Survey Design
Follow-up Scheme
Survey So Far
Summary

High-Cadence Transient Survey with Kiso/Tomo-e Gozen & Spectroscopic Follow-up with Seimei/KOOLS-IFU

せいめいUM・光赤外UM

2019/08/07-08

2

−24

45

Luminous Supernovae
SCP06F6
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−22

44

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Supernovae

43

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39

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2019/08/07-08

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−18
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]

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Peak Luminosity [M ]Vsubmitted

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ality between
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the electromagnetic
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SN2008ha
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4110
−14
41
41
41
41
−14 ) &"
−14
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P60−M82OT−081119
complete inventoryoftransients
in
the
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38 38
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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(denotedgrayIn
sixby grayyears,
searches,
we onlyweknew only
about three classes(denoted about
by gray bands).three
In the past sixclasses
years,
we onlysystematic
knew about
searches,
three classes (denotedbyby graybands). Inbands).
the past six years,
we onlysystematic
knew theaboutsearches,
threepastclasses (denotedbands). In thesystematic
past six years, systematic searches,

we only
knew
about
three
classes(denotedby gray
bands).
In theInpast
six
systematic
searches,
2019/08/07-08
we
only
knew
about
three
classes(denotedby gray
bands).
theせいめいUM・光赤外UM
pastyears,
six years,
systematic
searches,
High-Cadence Transient
Surveywith
Kiso/Tomo-e
Gozen& Spectroscopic
Follow-up
withSeimei/KOOLS-IFU

5

“Moment” of Supernova Explosion
Supernova Shock Breakout
before

after

days

hours

High-Cadence Transient Survey with Kiso/Tomo-e Gozen & Spectroscopic Follow-up with Seimei/KOOLS-IFU

shock breakout

せいめいUM・光赤外UM

2019/08/07-08

6

Very Early Phases of Core-Collapse Supernovae
Discovered by Victor Buso@Argentine, 16-inch telescope
SN 2016gkg@NGC 613
Bersten+2018, Nature

possible detection with Gaia (Garnavich+2016, Rubin+2016)
serendipitous detections with Swift/XRT (SN 2008D; Soderberg+2008),
GALEX (Schawinski+2008)
High-Cadence Transient Survey with Kiso/Tomo-e Gozen & Spectroscopic Follow-up with Seimei/KOOLS-IFU

せいめいUM・光赤外UM

2019/08/07-08

7

105cm Kiso Schmidt Telescope@Nagano, Kiso
105 cm Schmidt telescope (4th largest)
since 1974
open-use ==> collaboration basis (2018-)

High-Cadence Transient Survey with Kiso/Tomo-e Gozen & Spectroscopic Follow-up with Seimei/KOOLS-IFU

せいめいUM・光赤外UM

2019/08/07-08

8

Tomo-e Gozen April 2019 completed
84 CMOS sensors
low dark current, readout noise
operated in room temp. (no cooler)effective area: 20 deg2 (9 deg in diameter)
1k x 2k ~ 20 x 40 arcmin2
no filter (gri, Ha, … sometimes)
2 Hz readout (nominal): up to ~200 Hz

High-Cadence Transient Survey with Kiso/Tomo-e Gozen & Spectroscopic Follow-up with Seimei/KOOLS-IFU

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

せいめいUM・光赤外UM

2019/08/07-08

9

Northern Sky Transient Survey w/ Tomo-e Gozen
7,000 deg2 - 2 hr cadence - 18 mag depth
7,000 deg2 - 1 day cadence - 19 mag depth
no filter: effectively g+r bands
1 visit
6 sec exposure: [0.5 sec exposure] x 12
~18-19 mag
2x3 or 2x2 dithering~8% missed~60 deg2 (partially vignetted by ~30%)
cadence: ~2 hours
survey area / 2 hrs: ~7,000 deg2, EL>40 deg
2-4 times visits per night~19 mag for daily stacked data (not yet implemented)
survey simulation (Joao, Ikeda+)
reference: PS1 r-band
High-Cadence Transient Survey with Kiso/Tomo-e Gozen & Spectroscopic Follow-up with Seimei/KOOLS-IFU

せいめいUM・光赤外UM

2019/08/07-08

10

Tomo-e Gozen Survey Power

Yasuda+2019, in press

Tomo-e Gozen

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Survey Statistics (as of 2019/07/05)
equatorial

ecliptic

red: tonight
blue: previously observed(thicker, more visits)
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First Discovery of A Supernova (SN 2019cxx)
April 2019
Type Ia supernova@z=0.025
follow-up observations
Spectroscopy
Gemini-N/GMOS (Tanaka+)
Seimei/KOOLS-IFU (Maeda+)
Kanata/HOWPol
Imaging
Kanata/HOWPol

3 daysTomo-ePS1[Tomo-e] - [PS1]

Kanata/HONIR

http://www.ioa.s.u-tokyo.ac.jp/kisohp/NEWS/SN2019cxx/index.html
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Follow-up Scheme

After discovering transient candidates…
spectroscopic identification
flash spectroscopy w/ Seimei/KOOLS-IFU
multi-band light curves
KISS w/ KWFC: KISS international collaboration + OISTER# of spectroscopic observations (29 spec-ID+) limited: too faintTM+2014, Tanaka+2014, TM+2017, Gabanyi+2018, Kokubo+2019
Tomo-e Gozen survey: bright enough for OISTER domestic telescopes
discovery ==> follow-up within the same night
Approved programs
Seimei/KOOLS-IFU
Gemini-N/GMOS
KISS (w/ KWFC)
Kyoto/Seimei(Kanata, MITSuME)KOOLS-IFU
optical imaging

opticalspectroscopy

Tomo-e SN Survey
High-Cadence Transient Survey with Kiso/Tomo-e Gozen & Spectroscopic Follow-up with Seimei/KOOLS-IFU©Sako

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Proposed Observations for Seimei/KOOLS-IFU~15 candidates w/ ~> 1 mag day-1 (up to 150 Mpc)
“flash spectroscopy” (<1 day after Tomo-e discovery)~4 objects
more (~4 more times) follow-up w/ Seimei/KOOLS-IFU
more follow-up w/ Kanata, MITSuME, …
Discoveries, identification, & characterization of a few rapidly
evolving transients

Figure 4 The first supernova discovered
Tomo-e Gozen.
This supernova was spe
scopically observed with Seimei/KOOLS-IFU
Gemini-N/GMOS and identified as a Typez = 0.025. From left to right, 6-second T
e Gozen discovery image, PS1 reference im
Figure 3 Light curves of rapid transients withsubtracted image (Tomo-e−PS1), and follo
planned epochs of KOOLS-IFU spectroscopy. @Our proposal(from Tanaka+2016)
Kanata/HOWPol
IC -band image.
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High-Cadence Transient Survey with Kiso/Tomo-e Gozen & Spectroscopic Follow-up with Seimei/KOOLS-IFU

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Data Products
after image subtraction: being developed
Subtracted images relative to PS1 r-band
CNN ==> automatic alert for bright transients
photometry@subtracted images
before image subtraction for variable stars etc.
photometry & light curves
motion detection
NEO searchDiscovery of 2019 FA
size: ~8m (http://www.ioa.s.u-tokyo.ac.jp/kisohp/NEWS/2019FA/2019FA.html)

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Summary
Let’s catch supernovae (and other transient phenomena) in early-phase (rightafter explosions).
Tomo-e Gozen was completed in April 2019.
Northern Sky Transient Survey has been started since Nov. 2018 (w/ Q1).
Fully ready this fall.
2x2 dithering, 7,000 deg / 2 hours, 18 mag depth
2-4 visits / nightEffective survey by simulation (Joao, Ikeda et al. in prep.)
additionally consider weather conditions (avoid cloudy region andchoose clear sky region) <== ongoing
Development of automatic data reduction pipeline & website I/F: almost done.
Machine-learning technique (CNN) to pick up only real sources: being
developed
Automatic alert (to ourselves): being tested
First SN (Type Ia) was successfully discovered & identified.
quick follow-up observations w/ Seimei, Kanata, Gemini, …
“flash” spectroscopy w/ KOOLS-IFU

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