1. Nozomu Tominaga (Konan University/Kavli IPMU U. Tokyo)
Supernova shock breakout at high redshift and wide-field transient survey
Nozomu Tominaga
(Konan University/Kavli IPMU U. Tokyo)
23rd Jul 2013
DARK MATTER, DARK ENERGY AND THEIR DETECTION

2. Outline What are supernovae? Cosmology with transients
Issues to be addressed
Ongoing/future transient surveys
Kiso Supernova Survey (KISS)
Subaru/Hyper Suprime-Cam survey
Reference
NT et al. ApJ L10
NT et al. in prep.

3. 56Ni-56Co radioactive decay
Supernovae
SN1987A
Very bright
L~1042erg/s~109L8
Energy source
Shock heating
56Ni-56Co radioactive decay
Huge energy
EK~1051erg
Gravitational energy
GM28/RNS~1053erg
Nuclear energy
D(12C56Ni)M8~1051erg

4. Two types of supernovae
Core-collapse SNe (CCSNe)
Explosions of massive stars
Gravitational energy
Type Ia SNe (SNe Ia)
Explosions of low-mass stars
Nuclear energy
©MPA

5. Type Ia supernovae (SNe Ia)
“for the discovery of the accelerating expansion of the Universe through observations of distant supernovae”

6. Cosmology with CCSNe -Gamma-ray bursts-
A part of CCSNe accompany Gamma-ray bursts (GRBs).
GRBs can be observed up to z~8.
z=8.2
(Salvaterra + 09; Tanvir+09)
© Masaomi Tanaka

7. High-z cosmology with Gamma-ray bursts
GRBs could be a standard candle with Amati (Ep-Eiso) and Yonetoku (Ep-Lp) relations.
Current
Expected
Amati+08;Tsutsui+12

8. Issues to be uncovered Progenitor system
SNe Ia: white dwarf + main-sequence or redgiant stars
white dwarf + white dwarf
GRBs: rapidly rotating Wolf-Rayet star
a tiny fraction (10-5) of core-collapse SNe
Relativistic jets
Core collapse
Double degenerate
(White dwarf + white dwarf)
Single degenerate
(White dwarf + normal stars)
SNIa rate
CCSN rate
Hopkins & Beacom 06
CCSNe obs.
GRB obs.

9. To clarify them, SNe Ia: GRBs:
Early epoch observation
GRBs:
SLSN and Shock breakout connect CCSNe and GRBs
Kasen 10
1M8 Redgiant
6M8 Main-sequence
2M8 Main-sequence
No companion
3days
1days
NT+11
GRB B
Large
luminosity
gap
Superluminous supernova SN2006gy
Supernova shock breakout
SN1987A
e.g, SN2011fe (Li+11;Nugent+11)
We need observations with short cadence and continuous follow-up observations!!

10. Two optical transient surveys
Nearby supernova survey
Kiso Supernova Survey (KISS) from Apr 2012
Characteristics: high cadence
Aim: detailed studies of nearby objects
the progenitor system of Type Ia SNe
the nature of shock breakout
High-z supernova survey
Subaru/Hyper Suprime-Cam survey from Feb 2014
Characteristics: the deepest survey with wide FoV
Aim: detection of various high-z supernovae and GRBs
the cosmology with SNe Ia
the nature of GRBs

11. Nearby shock breakout survey -Kiso Supernova Survey-
Tominaga
PI: Moromuka
Tanaka
Mori
Matsumoto
Amateur collaborator
Tomoki Morokuma (Tokyo), Nozomu Tominaga (Konan), Masaomi Tanaka (NAOJ), Emiko Matsumoto (Konan), Kensho Mori (Hiroshima),
many other collaborators

12. Kiso Supernova Survey (KISS)
from Apr 2012
Kiso Wide-Field Camera (KWFC)
Diameter: 1.05m FoV: 4deg2
3min exposure (mlim,g~21mag) with ~1hr interval
2deg x 2deg
1.05m Schmidt telescope

13. Kiso Wide-Field Camera KWFC (Apr 2012 -)
One of the cameras with wide field-of-view
© Shigeyuki Sako

14. KISS strategy g-band observation of SDSS fields
~3min exposure with ~hour interval
observe the same field every night
Previous surveys observe a field every several days.
© Masaomi Tanaka

15. KISS collaboration Japan/Taiwan team
Kanata(1.5m)/HOWPol, MITSuME(0.5m), Lulin(1m)
Rochester Institute of Technology (KPNO 0.9-m)
Michael W. Richmond
Indian Institute of Astrophysics (HCT)
Devendra Sahu
Carnegie Supernova Project (CSP; NOT)
Eric Hsiao, Maximilian Stritzinger, Mark Phillips, Nidia Contreras, Francesco Taddia Morrell, Carlos Contreras
Telescopio Nazionale Galileo (TNG/DOLORES; 3.5m)
Paolo Mazzali, Emma Walker, Elena Pian
SNFactory (UH88/SNIFT)
Greg Aldering
Sternberg Astronomical Institute (Crimea, Moscow)
Dmitry Tsvetkov, Nikolay Pavlyuk

16. Follow-up observation
We can obtain a light curve for 24 hours.
Google

17. Type Ia SN with KISS SN 2012cm z=0.0282 phase: -9days
© Tomoki Morokuma

18. Shock breakout with KISS -not discovered yet-
~3 shock breakout in the 3 year project
mplateau~20mag, mtail~22mag
It is easy to be followed up with other telescope.
Multicolor light curve, spectroscopy g u r i z
20M8 E51=1 z=0.05

19. HSC transient survey HSC-transient group
Tomoki Morokuma (Tokyo), Naoki Yasuda (Kavli IPMU), Yuji Urata (NCU, Taiwan), Kuiyun Huang (ASIAA), Masaomi Tanaka (NAOJ), Jun E. Okumura (Kyoto), Tomonori Totani (Kyoto), Nozomu Tominaga (Konan), Takashi J. Moriya (Kavli IPMU), Robert Quimby (Tokyo/Kavli IPMU), Keiichi Maeda (Kavli IPMU), Shigehiro Nagataki (Kyoto), Ching-Hsuan Shen (NCU, Taiwan), Cheng-Hsien Tang (NCU, Taiwan), Meng-Feng Tsai (NCU, Taiwan), Min-Feng Wang (NCU, Taiwan), Naoki Yoshida (Tokyo)

20. Hyper Suprime Cam on Subaru telescope
Hyper Suprime-Cam (HSC)
Diameter: 8.2m, FoV: 1.77deg2
mlim (5s) w/ 1hr: 27.5(g) 27.2(r) 26.7(i)
from Feb 2014
HSC
1.5deg
HST
Suprime-Cam

21. First image (M31) -1st Feb 2013-
i-band 2min exposure
©HSC blog

22. HSC strategic program Primary science 300nights/5yrs 3 layers
Weak lensing
Galaxy evolution
300nights/5yrs
3 layers
Wide, Deep, Ultradeep
Transient science is free!!

23. Objectives Type Ia SN Core-Collapse SN Shock Breakout Superluminous SN
GRB Orphan Afterglow
QSO

24. Type Ia SNe HSC-UD survey SDSS: 0.05 < z < 0.4
(deep)/UD
z=1.2
SDSS: 0.05 < z < 0.4
SNLS: 0.3 < z < 1.0
HST: z > 1.0
DES: 0.3 < z < 1.0
~5000 SN Ia
SN Ia at z > 1 is still small number.
HSC-UD survey
~130 SN (~60 at z > 1) for S/N>5
~80 SN (~20 at z > 1) for S/N>10 (3 bands detection)

25. Type Ia SNe -cosmology-
Suzuki et al. (2011)
If we can use all S/N>5 sample in addition to UNION2 sample, error on ΩM and w will be decreased by a factor of 2.

26. Core-collapse SNe Available for free with SNe Ia cadence (deep)/UD
Survey
Tel.
Redshift
# of SNe
SNLS
CFHT
~0.3
120
GOODS
HST 45
HSC-UD
Subaru
~165

27. Shock breakout -detectable up to z>1.4-
g-band limiting
mag. w/ 10min
exposure 1%
10%
50%
90%
50% of detection is at z>0.7 and 10% is at z>1.4.
NT+11

28. Super Luminous Supernova
deep/UD
Super Luminous Supernova
Rare extremely bright SNe
CCSN z~4
Gal-Yam+12
Slow follow-up obs.
Spectroscopic follow-up is possible even at half a year after the detection

29. No GRB, but an optical flare.
GRB orphan afterglow
Direct evidence that GRB consists of relativistic jets
GRB!
Redshift range: 0.5<z<3
No GRB, but an optical flare.
Granot+02

30. SN rate history with HSC
HSC CCSNe
CCSN rate
HSC SN shock breakout
HSC SLSNe
HSC GRB orphan AG
SNIa rate
GRBs
HSC SNe Ia
Hopkins & Beacom 06 and references therein

31. Summary
Supernovae and gamma-ray bursts are bright so as to be useful for cosmology.
However, the progenitor systems are still unclear. To address them, we perform two optical surveys.
KISS: the progenitor of Type Ia SNe
the nature of shock breakout
HSC: the detection of high-z and/or rare transients
Many transient science cases are available with HSC strategic survey.
Cosmology with SNe Ia upto z~1.5
A ladder of CCSNe upto z~4 connecting to GRBs
Improvement of GRB cosmology