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Supernovae and GRB Connection

Supernovae and GRB Connection. Ken’ichi Nomoto (Univ. of Tokyo). MAGNUM (U. Tokyo). Supernova Spectra (Maximum Light). log(Flux). l (Å). SN 1998bw. Hypernova Candidates E kinetic > (5-10) × 10 51 ergs. GRB 980425. Spectra of Supernovae & Hypernovae. Ic : no H, no strong He,

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Supernovae and GRB Connection

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  1. Supernovae and GRB Connection Ken’ichi Nomoto (Univ. of Tokyo) MAGNUM (U. Tokyo)

  2. Supernova Spectra (Maximum Light) log(Flux) l(Å)

  3. SN 1998bw Hypernova CandidatesEkinetic > (5-10)×1051ergs GRB 980425

  4. Spectra of Supernovae & Hypernovae Ic: no H, no strong He, no strong Si SiII Ia O Ca He Ib Hypernovae： broad features blended lines 　　“Large mass at high velocities” Ic 94I 97ef Hyper-novae 98bw

  5. Core Collapse SNe Mass loss • ＩＩ-P • Single RG • ＩＩn, ＩＩ-L, ＩＩb • Close Binaries? • Ｉb, Ｉc • Single WR • Close Binaries • Hypernovae (Ｉc) ↔ Gamma-Ray Bursts • Rotating Single WR? (Helium) • Close Binary Mergers?(Mass of SN ejecta: Mej ?)

  6. SN2003dh SN2003lw SN1998bw SN2006aj SN1997ef SN2002ap SN1994I

  7. 56Co-decay

  8. CO Star Models for SNeIc H-rich He ５６Fe C+O 56Co MC+O Si 56Ni Fe Collapse • ~ [dyn• diffusion]1/2 ~• 1/2  Mej R V R c Parameters [Mej, E, M(56Ni)] Light Curve Spectra E  Mej  ½Mej¾E -¼ ５６Ni E  Mej3

  9. Jet-like explosion Tominaga et al. 2005

  10. M=25M, E=3×1050erg [Fe/H]=－5.3 Log X 56Fe He O 0 C H 58Ni －1 C Ne －2 Mg O Ti －3 N －4 2 4 6 8 Mr (M) MBH~6M ejecta Fallback Mixing Umeda & Nomoto (2003)

  11. Spectral Fitting: SN1997ef Iwamoto et al. (2000) Too Narrow Features E51=E/1051 erg Normal SN (E51=1) Small Mej Hypernova (E51=20) Large Mej at High Vel. Broad Features

  12. Light curves of Hypernovae & SNeIc log L (erg/s) Radioactive Decay 56Ni 56Co 56Fe 43 98bw 42 97ef 41 94I 0 50 100 t (days)

  13. SN 2003dh /GRB 030329

  14. GRB 030329 / SN 2003dh Hjorth et al (2003)

  15. SN2003dh / GRB030329 Deng et al. (2005)

  16. SN2003lw / GRB031203 Deng et al. (2005)

  17. Supernova – GRB Connection Three GRB－SNe = all Type Ic Hypernovae E > 1052 erg (～10×normal SN) Large Mms→Black Hole Forming SNe Aspherical

  18. Type II-P SN 1997D Very narrow lines. V < 1000 km s-1. EK=1-4×1050ergs. V~1000km s-1 2002gd, 1999br Faint M(56Ni)~0.002M (Turatto, Mazzali, Young, Nomoto 2002)

  19. Turatto, Mazzali, Young, Nomoto, Iwamoto et al. (1998) SNⅡ 1997D:Faint SN m－M=30.64 (NGC1536) 1987A LBOL 1997D Mms~20M M(56Ni) 0.07M 0.002M 1987A 1997D Mms~ 25－30MR ≤ 300R E~4×1050erg narrow lines

  20. Hypernovae/Faint SNe GRB-SN EK Failed SN? 13M ☉ ~15M☉ Nomoto et al. (2003)

  21. Hypernovae/Faint SNe (56Ni mass) Nomoto et al. (astro-ph/0308136) GRB-SN

  22. Non-GRB Hypernovae SNe 1997ef, 1999as, 2002ap, 2003jd MAGNUM (U. Tokyo)

  23. Brightest Hypernova: 1999as @z=0.127 (Knop et al.) E ~ 3×1052erg Mms ~ 60M MCO ~ 20MM(56Ni) ~ 5.4M mag SN 1999as (Deng et al. )

  24. SN2003dh SN2003lw SN2006aj SN1998bw SN1997ef SN2002ap SN1994I

  25. SN 2003jd SN 1983V SN 2003jd SN 2002ap SN 1998bw

  26. Spectra of SN2002ap 4M8 C+O star (Mms ~ 25) (E = 4e51 erg) Mazzali et al. 2002

  27. XRF060218SN2006SN2006aj 200602

  28. SN2003dh SN2003lw SN2006aj SN1998bw SN1997ef SN2002ap SN1994I

  29. 3 days since the explosion FeIII, FeII OI 7774

  30. 16 days since the explosion SiII OI 7774 CaII IR triplet

  31. Comparison with 02ap SN 2006aj (21 Feb 2006) Model2Msun Model4Msun SN 2002ap at z=0.033 OI 7774

  32. SN 2006aj 13 days after the explosion (3 Mar 2006) CrII, TiII Model 2 Msun 4 Msun OI 7774 SiII 6355 FeII, FeIII CaII IR triplet

  33. SN 2006aj

  34. XRF 060218/ SN 2006aj • Small Oxygen Mass < 1.3 M8 • Mej ~ 2 M8 (Mms ~ 20 M8) • E ~ 2 x 1051 erg • M(56Ni)~0.21M8 • Neutron Star forming SN ? • Magnetar-driven XRF ? • Mass Loss Rate ? Shell ? • Cas A – connection ?

  35. Non-GRB, peculiar SN Ib 2005bf MAGNUM (U. Tokyo)

  36. SN Ib 2005bf: Spectra H feature He Tominaga et al. 2005

  37. SN 2005bf: Observed Light Curves Tominaga et al. 2005 Folatelli et a. 2006 Modjaz et al. 2006

  38. Comparison with other SN Ib/c

  39. SN 2005bf: Abundance Distribution X(56Ni)=0.44 X(He)=0.44 Mass Fraction Si, O, C He H,He X(56Ni)=0.03 Ni X(56Ni)=0.013 1,600 3,900 5,400 13,000 Velocity [km/s]

  40. Type Ib SN 2005bf • Peculiar Light Curve • Double peaks : M(56Ni)~0.3M8 • Slow rise to the 2nd peak (~40 days) • Rapid decline • Mej ~ 6 – 7 M8 (Mms ~ 25 – 30 M8) • E ~ 1.3 x 1051 erg • Explosion of a WN star He, H features

  41. Subaru FOCAS Obs. of SN 2005bf He indicated by [OＩ] ~10 days after the 2nd peak. [CaＩＩ] [FeＩＩ]?? H

  42. Unipolar Ejection of 56Ni(Fe)? [OI] 6300 [FeII] 7150 [CaII] 7300 sym. axis sym. axis Ca O Fe

  43. SN 2005bf: Light Curve @ Late Phases

  44. Type Ib SN 2005bf • Nebula Spectrum • [FeII], [CaII],[OI] : Blue shifted by ~1500 km/s • [OI] : Double peaks • Unipolar Jet ? • Kick ? (v ~ 200 – 600 km/s ?) • Neutron Star Forming SN ?? - normal E, small mass cut, large M(Ni) Rapid decline of LC:56Ni decay ?? - Magnetar?? GRB connection??

  45. First Star – Hypernova Connection: Abundance Patterns of Extremely Metal-Poor Stars

  46. Metal Poor Stars • Mega Metal Poor (MMP): [Fe/H] < -6 • Hyper Metal Poor (HMP): [Fe/H] < -5 • Ultra Metal Poor (UMP): [Fe/H] < -4 • Extremely Metal Poor(EMP) : [Fe/H] < -3 • Very Metal Poor (VMP): [Fe/H] < -2 • Metal Poor (MP) : [Fe/H] < -1 • Solar: [Fe/H] ~ 0 • Super Metal Rich(SMR): [Fe/H] > +0.5 [Fe/H]=log(Fe/H)-log(Fe/H) (Beers & Christlieb 2005)

  47. McWilliam, Ryan Co Cr trend [Fe/H] [Fe/H] Mn Zn

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