Presentation is loading. Please wait.

Presentation is loading. Please wait.

Nozomu Tominaga (Konan University/Kavli IPMU U. Tokyo)

Similar presentations

Presentation on theme: "Nozomu Tominaga (Konan University/Kavli IPMU U. Tokyo)"— Presentation transcript:

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

Download ppt "Nozomu Tominaga (Konan University/Kavli IPMU U. Tokyo)"

Similar presentations

Ads by Google