1. Optical & Near-Infrared Observations of Peculiar Type Ia SNe with Domestic Collaborations in Japan Masayuki Yamanaka Konan Univ. Seminar at SAI on 2014 Nov. 21

2. Topics of my talk : Two Topics 1. EARLY PHASE OBSERVATIONS OF EXTREMELY LUMINOUS TYPE Ia SUPERNOVA 2009dc (Yamanaka et al. 2009, ApJ, 707, L118) 2. Early-Phase Opitcal & Near-Infrared Observations of Type Iax SN 2012Z with OISTER (Yamanaka et al. in prep) Seminar at SAI on 2014 Nov. 21

3. Type Ia SN : Distance Indicator We can estimate the distance from the light curves ⇒ Distant SNe Ia ⇒ Constraints on dark energy ⊿ m 15 (B) : the decline rate Strongly-correlated with luminosity Good indicators of distance apparent mag days since max 15 day after max ⊿ m 15 (B) max Light curve Correlations between ⊿ m 15 (B) and absolute magnitudes Seminar at SAI on 2014 Nov. 21

4. The luminosity is too high to explain with non-rotating white dwarf in the “single degenerate scenario. On the other hand, there is no “double- degenerate” explosion model to reproduce the luminosity. Seminar at SAI on 2014 Nov. 21 Super-Chandrasekhar (SC) SN Single Degenerate Double Degenerate ? Howell et al. 2006, Nature, 443, 308

5. SuperNova 2009dc Discovered at 16.5 mag on Apr. 9.31( Ｕ Ｔ ). Distance to UGC 10064 is 89.3Mpc (CBET 1762) Spectroscopy at Apr.16 The spectrum is very similar to that of a previous super-Chandrasekhar SN Ia. Show the CII absorption (CBET 1768) 。 Really Super-Chandrasekhar SNe ? Closer than other super-Chandrasekhar events Seminar at SAI on 2014 Nov. 21

6. Observations in Domestic Collaborators Early-phase (until 100 days from discovery) 1.5m Kanata + HOWPol (imaging) (Configurations Dedicated for Transients) +1.5m@Gunma + GLOWS (Spectroscopy) 、 1.88m@OAO + ISLE (NIR imaging) 0.5m-MITSuME@OAO 、 1.0m@Kagoshima We successfully started the observations of 09dc at a day after the report 1.5m Kanata Telescope Multi-Mode Observations performed by Various Telescopes Seminar at SAI on 2014 Nov. 21 Map of Japan Gunma Hiroshima

7. What we can know from SNe observations ? Outer inner 56 Ni 56 Co 56 Fe γ γ, e + wavelength flux λ λ0λ0 λλ0λ0 P Cygni profile observer Ejecta interact with gamma-ray from 56Ni decay ⇒ Thermarised ejecta, the radiation peaked in optical wavelength Spectra Line velocity 8.8 days 111 days 56 Ni 56 Co 30day luminosity Days since explosion Diffusion time : depended on M, E Seminar at SAI on 2014 Nov. 21

8. Decline rate indicates the luminosity ⇒ SN 2009dc is expected to be intrinsically extremely luminous Very slow decline ● 09dc × 06gz － 05cf B V Rc Ic ⊿ m15(B) : magnitude difference between the peak and 15 days after its peak. Optical Light Curves ID ⊿ m 15 (B) SN 2009dc0.65+/-0.03 SN 2006gz0.69+/-0.05 SN 2005cf1.05 09dc(0.65) 03fg 06gz Seminar at SAI on 2014 Nov. 21

9. Abs.Mv No-19.90+/-0.05 Yes-20.32+/-0.19 06gz : Mv=-19.90+/-0.21 If we ignore the extinction, SN 2009dc is one of the most luminous Type Ia SN. Galaxy host 09dc(0.65) Corrections of host extinction ⇒ intrinsic luminosity Absolute magnitude 06gz 03fg Seminar at SAI on 2014 Nov. 21

10. ● 09dc(Abs.) × 09dc(No abs.) ― 06gz -- 05cf Assumption ： optical flux is 60%.of total (c.f.Stritzinger et al. 2006) Rising-time is 23 day (Silverman et al. 2010) No extinction : 56 Ni mass is estimated to be 1.3 +/- 0.3 M  Extinction : 2.0+/- 0.5 M  c.f. typical SN 2005cf : 0.8 M  Ever largest 56 Ni mass in SNe Ia Yamanaka et al. 2009 56 Ni mass is strongly related to the luminosity Quasi-Bolometric luminosity and 56 Ni mass Seminar at SAI on 2014 Nov. 21

11. Yamanaka et al. 2009 SNphase SN 2009dc5.6d after max SN 2006gz11d before max SN 2003du (typical)unseen CII is see until 5.6d ⇒ very thick C layer C : direct origin of WD ⇒ very massive WD Spectra : remarkable CII Typical SN Ia Si,S,Ca Ni,Fe C SN 2009dc Seminar at SAI on 2014 Nov. 21

12. Extremely luminous 、 very slow light curves ： rich 56 Ni(Fe) layer Low polarization ： almostly spherical symmetry (Tanaka et al.) Deep absorption of CII ： thick C layer ⇒ very massive WD (c.f. 2.4M  in standard model) ⇒ SN 2009dc could be a Super-Chandrasekhar SN CO Ni(Fe) Si,S,Ca,etc (burnt material) Carbon (unburnt material) normal 06gz 09dc Pictures of the whole ejecta of SN 2009dc Seminar at SAI on 2014 Nov. 21

13. Rapidly-rotating WDMerger in double ⇒ 56 Ni mass ~ 1.5M  、 total mass ~2.1M  Pfannes+ 2010 Pakmor+ 2010 ⇒ 56 Ni mass ~ 0.1M  、 total mass ~1.9M  SN 2009dc 56Ni mass ~ 2.0M , 2.4M  Rather well reproduce the properties of Faint Type SN Ia (Pakmor+) What is the nature of Progenitor for super-Chandra SN Ia? Seminar at SAI on 2014 Nov. 21

14. Next topic : Peculiar Type Ia SNe Seminar at SAI on 2014 Nov. 21 SNe Ia Progenitor ： WD in the close binary system -> Thermonuclear explosion -> Similar properties : distance indicator However, some peculiar SNe Ia do not obey Phillips (width-luminosity) relation (discovered by Li+ 2003) Prieto et al. 2006 More luminous, more slower -> Phillips relation The most faint peculiar SNe Ia was discovered in 2008. Its properties are rather similar to those of CC SNe. -> Too faint to be reproduced by thermonuclear explosion? luminosity decline rate Valenti et al. 2009, Nature Narayan et al. 2011

15. Progenitor detection : single degenerate Blue source was detected. It would be ‘He star’, which may be a companion star in close binary system, e.g., V445 Pup HeI emission lines are detected in late- phase (1yr) spectra : 07J (Foley et al. 2013) In recent binary model, the delay time is as long as 50-100Myr, whose age may be as young as that of a Type IIP SN. (Meng et al. 2014, Lyman et al. 2013, ) McCully et al. 2014, Nature, Seminar at SAI on 2014 Nov. 21

16. What is “OISTER” ? Seminar at SAI on 2014 Nov. 21 Optical and Infrared Synergetic Telescopes for Education and Research (“OISTER”) Domestic collaborations among Universities and NAOJ cooperated since 2011. Two strong points for SNe observations ① Canceling out the bad-condition weather, ② multi-band observations in the limited time -> Realized the high-cadence and multi-bands observations just after explosion date Permit us get the high-quality and large data set as good as those by other international collaborations

17. Do Deflagration models explain ? Seminar at SAI on 2014 Nov. 21 Phillips, Li, Frieman, Blinnikov et al. 2007, PASP Fink et al. 2014, MNRAS Bolometric light curves from ‘pure deflagration’ model Hydrodynamical studies with ‘failed deflagration’ ✔ Strong mixing ✔ faint luminosity ✔ a bit low metal environment ✔ compact remnant ? Foley et al. 2014, ApJ Significant detections of SN 2008ha indicate that the source is more luminous than SN at 1500days after max Input energy is smaller than the binding energy in WD

18. SUMMARY Seminar at SAI on 2014 Nov. 21 We present the optical and near-infrared studies of 2 peculiar SNe Ia with Dosmestic Collaborations in Japan. SN 2009dc has a extremely high luminosity and slow decline of the light curves. The strong CII absorption and low expansion velocity support that the ejected mass is much large. We conclude that SN 2009dc could be a super-Chandrasekhar SN. We also have obtained very high-cadence optical and NIR data set of Type Iax SN 2012Z with OISTER. We found that early-phase (outer layer) NIR properties are very similar to those of prototype SN 2005hk even including extremely faint SN 2008ha. We concluded that SNe Iax could have common origin.

19. Seminar at SAI on 2014 Nov. 21 Спасибо ！