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Spectroscopic signatures of SN Ia progenitors A talk not about the Palomar Transient Factory

Spectroscopic signatures of SN Ia progenitors A talk not about the Palomar Transient Factory . Avishay Gal-Yam, Weizmann Institute of Science Leiden workshop 2010. Preamble. Lots of time for questions What is a type Ia SN? . Not going to cover: CSM interaction, CSM absorption.

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Spectroscopic signatures of SN Ia progenitors A talk not about the Palomar Transient Factory

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  1. Spectroscopic signatures of SN Ia progenitorsA talk not about the Palomar Transient Factory Avishay Gal-Yam, Weizmann Institute of Science Leiden workshop 2010

  2. Preamble • Lots of time for questions • What is a type Ia SN? • Not going to cover: CSM interaction, CSM absorption

  3. The basics: data+models Sauer et al. 2008 • Chandrasekhar-mass C/O models fit the data well

  4. Progenitor signatures: 1 • Hydrogen and helium: no convincing evidence

  5. Progenitor signatures: 2 Tanaka et al. 2010 Howell et al. 2006 Mazzali 2001 • Carbon: evidence for C/O progenitor (not O/Ne) • Indicative of deflagration • Strong in super-C events (Howell)

  6. Progenitor signatures: 3 Tanaka et al. 2008 • Ca high-velocity features – CSM (SD)? • Or else, 3D effects?

  7. Faint events (1991bg-like) Mazzali et al. 1997 • High velocity oxygen shell • No outer He shell

  8. Interim summary • SNeIa are explosions of C/O WDs with mass ~MCh • How much C survives ? • There are no traces of H or He (no outer He shell) • H CSM may be indicated (SD) What are SNeIa? What can we learn from other SNe?

  9. Type Ib (UCB; CCCP) Graham & Li 2005 Shy cousins: SN 2005E LOSS discovery Member of the Ca-rich Subclass (Filippenko et al.) Hagai Perets, Nature, in press Dave Arnett, Paolo Mazzali, Daniel Kagan, UCB SN group, CCCP, Anderson & James, Ofek, Bildsten & Co., Quataert & Co.

  10. A massive star? No star formation to deep limits … unlikely also on theoretical grounds r<25.3 (25.9) at 3(2)  Perets et al. 2009

  11. 22.9 kpc 11.3 kpc A hyper-velocity SN (HVSN) ? Life in the fast lane? SN 2005E Not likely: chances to observe HVSNe with LOSS are < 1/100

  12. Mazzali So what, then? What will nebular spectra reveal? Peculiar abundances (C, O, Ca, Ni56) = (0.1 0.037 0.135 0.003) solar Total ejected mass is <0.3 solar !

  13. Not a single event! 6-10 additional siblings, additional early hosts

  14. What can it be? A double WD (O/Ne+He): accretion induced collapse ? Or else, CO/He DD merger (Waldman models)

  15. } Models by Arnett Nucleosynthesis Can you make so much Ca with no Si and S? (Ca/S >6) * No (if you burn C/O) * Yes (if you burn He) Confirmed by details models by Waldman et al.

  16. Can we start mapping? Normal SNeIa: SD? Faint SNeIa: CO/CO DD? SN 2005E CO/He DD?

  17. Thanks

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