Tomo-e Gozenによる高頻度突発天体探査観測諸隈 智貴(東京大学・天文学教育研究センター)
Tomo-e Gozen Survey

第9回光赤外線天文学大学間連携ワークショップ@埼玉大学, 2018/12/25,26

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Contents
Kiso Schmidt Telescope & Tomo-e Gozen
All-Sky Survey w/ Tomo-e Gozen
Survey Statistics
Data Products
Follow-Up Observations
Summary

Tomo-e Gozen Survey

第9回光赤外線天文学大学間連携ワークショップ@埼玉大学, 2018/12/25,262

Kiso Schmidt Telescope@Nagano, Kiso
105 cm Schmidt telescope(4th largest)
since 1974

Tomo-e Gozen
84 CMOS sensors
9 deg in diameter
effective area: 20 deg2
1k x 2k ~ 20 x 40 arcmin2
no filtergri, Ha, … sometimes
2 Hz readout (nominal)
up to ~200 Hz (wide-fieldpulsar survey by M. Ichiki)Tomo-e Gozen Survey

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Tomo-e Gozen Field-of-View
Q1

Q2

Q3
Tomo-e Gozen Survey

Q4
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Tomo-e Gozen: 4 same components (Q1-4)
Q1: completed
Q3: under modification
Q2, Q4: under development. coming in a few months

Q1 commissioning data (2018/02)

Tomo-e Gozen Survey©S. Sako 5

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Q1+Q3 on focal plane

Q1Q3

Tomo-e Gozen Survey

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Tomo-e Gozen Transient Survey

started on Nov. 8, 2018 w/ Q1 (5 deg2)

10,000 deg2 - 2 hr cadence - 18 mag depth(10,000 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
fully utilize 2 Hz data in (near-)future~60 deg2 (partially vignetted by ~30%@FoV edge)
cadence: 2 hours
survey area (per 2 hours): ~10,000 deg2 (EL>30-35 deg)
3-5 times visits per night~5 “early” supernovae / year
supernova, nova, pulsar, (GW), neutrino, comet, asteroid, meteor,occultation, NEO, debri, super-flare, dwarf star flare, CV, “Tomo-eFlash” , YSO, Ultra-Long GRB, Fast Radio Burst, AGN, X-ray
transient (MAXI, NICER, etc…), UV transient (Hibari), “Rare EventSurvey”, polarization survey, unknown unknown??
9Tomo-e Gozen Survey

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Very Early Phases of Core-Collapse Supernovae
beforeafter~days~hours
Shock Breakout
Tomo-e Gozen Survey

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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)
Tomo-e Gozen Survey

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the light curves at t ! 2 day. However, in all
X-ray burst should be bright. Proposed X-r

Very Early Phases of Type Ia Supernovae
doi:10.1038/nature23908

va with an early flash
l detonation

absolute magnitude

single degenerate (SD) vs -20
double degenerate (DD) -19-18-19-17

geyama4, Ken’ichi Nomoto3, Naoki Yasuda3, Saurabh W. Jha6,-18, Željko Ivezić9, Pilar Ruiz-Lapuente10,11, Maximilian D. Stritzinger12,etrich Baade16, Nao Suzuki3, Andrew J. Connolly9,nes19,20, Hisanori Furusawa7 & Satoshi Miyazaki7,21-17

yeriseralapparent g-band magnitude of 25.14 ± 0.15 on 4.345 April ut (modified-16
Julian date 57482.345). One day later, MUSSES1604D brightened
rapidly to about 23.1 mag and 23.0 mag in the g- and r-bands, respec0
tively. More surprisingly, the g-band observation on 6 April indicates-16bolometric
5

1015

-19

–18
g+1

–16
–16.5

–14–15
HSC r

–13.5
–12
0
0

10

1

2
20

-18
20

-17-16
22

22-15

23

24

24-14
0

25

26

-15
-14
0

5

1015

©Yamanaka,
M.
-18
-17
Apparent magnitude

absolute magnitude

rKasen+2007
ultraviolet
model

-19

18

i–1

–20

Absolute magnitudeofeulesofnaneutant
lhedd,
af,shnory

1 MO• RG
6 MO• MS2 MO• MS
no companion-16

B-band510
days since explosion

15-15-140V-band
510
days since explosion

15Figure
HSC3.g Signatures of companion interaction in the early broadband light curves of Type Ia supernovae. We model three different progencompanion at26a = 2 × 1013 cm (green lines), a 6 M⊙ MS companion at a = 2 × 1012 cm (blue lines), and a 2 M⊙ MS companion at a = 5 × 10
345ultraviolet
light curves are constructed by integrating the flux in the region 1000–3000 Å and converting to the AB magnitude system. For all li◦viewingangle
30
40 is θ =50 0 .
60

Days since explosion (3 April)

Jiang+2017, Nature, @z=0.117

Figure 1 | The multi-band light curve of MUSSES1604D. The figure
shows photometric data from the g-, r- and i-bands (from the observer’sframe of reference), in the AB-magnitude system. Error bars denote 1σTomo-eGozenSurvey
第9回光赤外線天文学大学間連携ワークショップ@埼玉大学,
2018/12/25,26
uncertainties.
The dashedlines show
the best-fitting lightcurves derivedSN 2012ht@d~20 Mpc 12

Transient Surveys
OISTER spectroscopy

Tomo-e Gozen Survey

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Transient Surveys
OISTER spectroscopy

Tomo-e Gozen Survey

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Tomo-e Gozen Q1 Survey Observations
Started on Nov. 8, 2018
Q1: 5 deg2 FoV
remote observations
from “Kiso Observing Room” (tentative) @UT/IoA/Mitaka
Observers:
students: Y. Kojima (NEO), N. Arima (SN Ia), M. Ichiki (pulsar),
M. Morita (blazar), R. Hamasaki (SN, Konan), J. Jiang (SN Ia)
staffs: S. Sako, R. Ohsawa, Y. Niino (GW, FRB), TM (SN)
daytime work: T. Aoki, T. Soyano, K. Tarusawa, Y. Mori, S. Sako,R. Ohsawa, N. Takahashi, …
queue system“recipe” files made bysurvey simulation
Dome is closed automaticallywhen the weather gets bad.
objectives: NEO, supernovae
Tomo-e Gozen Survey

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Tomo-e Gozen Survey Simulation (by TM)
Requirements
maximize survey area with>=3 times visits with >1.5hour intervals.
minimize telescope motion.
minimize dome motion.
EL > 35 deg, higher isbetter.
(avoid Galactic Plane)
collaboration w/ Ikeda-san@ISM& his collaborators ongoing…

Tomo-e Gozen Survey

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Q1 (5 deg2) Data
9 deg

Tomo-e Gozen Survey

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Survey Statistics (2018/11,12)17.4 magdark: 18.2
bright: 16.6

S/N=10 depth
25.0 magtransparency
4.5 arcsec

bad in winterseeing7x105 fits
11/8

11/18

Tomo-e Gozen Survey

11/28

12/8

12/18

~10,000deg2
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2018/12/25,26

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Data Products

bias subtraction, dark
subtraction, flat-field,
astrometry

subtracted images (reference: PS1 r-band)
light curves of transients@subtracted
stacked images
0.5 sec x 12 frames = 6 sec exposure
simple photometry
free from cosmic rays
(zeromag, limiting
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simple photometry: 2x10 records
magnitude), image(for ~1.5 months, Q1, …)
subtraction, transient
light curves of all detected objects ???
detection
dep
external dataloevedgni
in other wavelength and/or with other telescopes be
optical, UV, IR: SDSS, PS1, GALEX, WISE, AKARI, …
X-ray: ROSAT, XMM-Newton, Chandra, …
radio: FIRST, NVSS, TGSS
object catalogs
SDSS (BAL) quasars
TNS transient objects
MPChecker asteroids
and more?
Tomo-e Gozen Survey

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Dedicated DB / Website being prepared©N. Tominaga, M. Tanaka, J. Jiang, R. Ohsawa, S. Sako, TM
developed based on KISS (Kiso/KWFC) & Subaru/HSC DB/Website
almost the same people involved
tentative DB almost completed.
updated in a few months based on this DB
Website can be browsed only via VPN. (only for developers now)functionsdata list w/ data reduction statustransient sources from subtracted images
transient sources from stacked images (?)

Tomo-e Gozen Survey

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still under development
tagdatecoordinate

Tomo-e Gozen Survey

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TXS 0506+056 = IceCube-170922A

46 records
for 35 days

Tomo-e Gozen Survey

第9回光赤外線天文学大学間連携ワークショップ@埼玉大学, 2018/12/25,2622

Follow-Up ObservationsOISTER facilities
J-GEM facilities (not involved in OISTER)
Gemini-N/GMOS (M. Tanaka+, S19A, 2019/02-07)(KISS collaboration)other wavelengths

Tomo-e Gozen Survey

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Working Groups
tomoe-gw: gravitational wave follow-up
tomoe-sn: supernova
tomoe-ps: planetary science (debri, meteor, NEO, comet, asteroid,TNO, YSO, exoplanet)
tomoe-agn: AGN (incl. blazar)
tomoe-star: nova, stellar flare, late-type star
tomoe-cobj: compact object (black hole, neutron star, pulsar,magnetor, white dwarf, GRB, FRB), high-energy transient event
tomoe-data: data science
Ryou Ohsawa (ohsawa@ioa.s.u-tokyo.ac.jp)
Tomoki Morokuma (tmorokuma@ioa.s.u-tokyo.ac.jp)
Shigeyuki Sako (sako@ioa.s.u-tokyo.ac.jp)

Tomo-e Gozen Survey

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SummaryTomo-e Gozen is a ultra-wide-field imaging instrument for the
1.05-m Kiso Schmidt telescope.
Q1(+Q3) (10 deg2 in total) were almost completed.
Q2 (February, 2019) & Q4 (April, 2019) coming soon.
will be almost ready for GW follow-up before O3 starts.
We have started an all-sky survey since Nov. 8, 2018.
2Hz x 12 exposures ==> 6 sec per visit
no filterStatistics
depth: 17.4 mag (all), 18.2 (dark), 16.6 (bright)
seeing: 4.4 arcsec seeing (bad in winter)
Data products will be available for anyone being interested inthem.
Transient detection in subtracted images are almost ready.
Light curves with simple photometry…?

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