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 surveyNozomu Tominaga(Konan University/Kavli IPMU U. Tokyo)23rd Jul 2013DARK MATTER, DARK ENERGY AND THEIR DETECTION
2 Outline What are supernovae? Cosmology with transients Issues to be addressedOngoing/future transient surveysKiso Supernova Survey (KISS)Subaru/Hyper Suprime-Cam surveyReferenceNT et al. ApJ L10NT et al. in prep.
7 High-z cosmology with Gamma-ray bursts GRBs could be a standard candle with Amati (Ep-Eiso) and Yonetoku (Ep-Lp) relations.CurrentExpectedAmati+08;Tsutsui+12
8 Issues to be uncovered Progenitor system SNe Ia: white dwarf + main-sequence or redgiant starswhite dwarf + white dwarfGRBs: rapidly rotating Wolf-Rayet stara tiny fraction (10-5) of core-collapse SNeRelativistic jetsCore collapseDouble degenerate(White dwarf + white dwarf)Single degenerate(White dwarf + normal stars)SNIa rateCCSN rateHopkins & Beacom 06CCSNe obs.GRB obs.
9 To clarify them, SNe Ia: GRBs: Early epoch observationGRBs:SLSN and Shock breakout connect CCSNe and GRBsKasen 101M8 Redgiant6M8 Main-sequence2M8 Main-sequenceNo companion3days1daysNT+11GRB BLargeluminositygapSuperluminous supernova SN2006gySupernova shock breakoutSN1987Ae.g, SN2011fe (Li+11;Nugent+11)We need observations with short cadence and continuous follow-up observations!!
10 Two optical transient surveys Nearby supernova surveyKiso Supernova Survey (KISS) from Apr 2012Characteristics: high cadenceAim: detailed studies of nearby objectsthe progenitor system of Type Ia SNethe nature of shock breakoutHigh-z supernova surveySubaru/Hyper Suprime-Cam survey from Feb 2014Characteristics: the deepest survey with wide FoVAim: detection of various high-z supernovae and GRBsthe cosmology with SNe Iathe nature of GRBs
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. RichmondIndian Institute of Astrophysics (HCT)Devendra SahuCarnegie Supernova Project (CSP; NOT)Eric Hsiao, Maximilian Stritzinger, Mark Phillips, Nidia Contreras, Francesco Taddia Morrell, Carlos ContrerasTelescopio Nazionale Galileo (TNG/DOLORES; 3.5m)Paolo Mazzali, Emma Walker, Elena PianSNFactory (UH88/SNIFT)Greg AlderingSternberg Astronomical Institute (Crimea, Moscow)Dmitry Tsvetkov, Nikolay Pavlyuk
16 Follow-up observation We can obtain a light curve for 24 hours.Google
18 Shock breakout with KISS -not discovered yet- ~3 shock breakout in the 3 year projectmplateau~20mag, mtail~22magIt is easy to be followed up with other telescope.Multicolor light curve, spectroscopyguriz20M8 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)
22 HSC strategic program Primary science 300nights/5yrs 3 layers Weak lensingGalaxy evolution300nights/5yrs3 layersWide, Deep, UltradeepTransient science is free!!
23 Objectives Type Ia SN Core-Collapse SN Shock Breakout Superluminous SN GRB Orphan AfterglowQSO
24 Type Ia SNe HSC-UD survey SDSS: 0.05 < z < 0.4 (deep)/UDz=1.2SDSS: 0.05 < z < 0.4SNLS: 0.3 < z < 1.0HST: z > 1.0DES: 0.3 < z < 1.0~5000 SN IaSN 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 SurveyTel.Redshift# of SNeSNLSCFHT~0.3120GOODSHST45HSC-UDSubaru~165
27 Shock breakout -detectable up to z>1.4- g-band limitingmag. w/ 10minexposure1%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/UDSuper Luminous SupernovaRare extremely bright SNeCCSN z~4Gal-Yam+12Slow 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 afterglowDirect evidence that GRB consists of relativistic jetsGRB!Redshift range: 0.5<z<3No GRB, but an optical flare.Granot+02
30 SN rate history with HSC HSC CCSNeCCSN rateHSC SN shock breakoutHSC SLSNeHSC GRB orphan AGSNIa rateGRBsHSC SNe IaHopkins & Beacom 06 and references therein
31 SummarySupernovae 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 SNethe nature of shock breakoutHSC: the detection of high-z and/or rare transientsMany transient science cases are available with HSC strategic survey.Cosmology with SNe Ia upto z~1.5A ladder of CCSNe upto z~4 connecting to GRBsImprovement of GRB cosmology