sn ia clues from rates and the delay time distribution
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SN Ia clues from rates and the delay-time distribution Dani Maoz, Tel-Aviv University single degenerate ( SD ) (Whelan & Iben 1974) WD Main sequence, subgiant, red- giant, or helium star double degenerate

  1. SN Ia clues from rates and the delay-time distribution Dani Maoz, Tel-Aviv University

  2. “ single degenerate ” ( “ SD ” ) (Whelan & Iben 1974) WD Main sequence, subgiant, red- giant, or “ helium star ”

  3. “ double degenerate ” ( “ DD ” ) (Webbink 1984; Iben & Tutukov 1984)

  4. Also: “ collisional double degenerate ” (Benz+, Hawley+, Loren-Aguilar+, Raskin+, Rosswog+, Thompson, Katz & Dong, Kushnir+, Garcia-Senz+… )

  5. Also: “ core degenerate ” (Soker+) merger + spinup/spindown

  6. Measuring SN Rates Can give clues to progenitors

  7. SN Ia “ delay time distribution ” (DTD): = the hypothetical SN Ia rate vs. time following a short burst of star formation. Different progenitor scenarios predict different DTD Star formation rate SN DTD SN SFR Rate t=0 time t=0 time

  8. e.g., Double-Degenerate scenario. Consider population of binary WDs. Time until merger of each pair (gravitational wave losses): DTD ~ t -1 expected generically

  9. double-degenerate: DTD ~ t -1 expected generically

  10. similarly: single-degenerate: DTD cutoff at few Gyr MS secondaries M<2 Mo cannot transfer mass stably Decreasing secondary mass

  11. Recovering the delay time distribution (many different ways to do it) e.g. SN rates in galaxy clusters

  12. SDSS 1004+4112 z=0.68 Sharon et al. (2010)

  14. The SN rate vs. redshift in galaxy clusters B10 Cosmic time Maoz, Sharon, Gal-Yam (2010)

  15. Time-integrated # of SNe-Ia must produce observed mass of Fe in clusters (minus mass from CC-SNe) Maoz, Sharon, Gal-Yam (2010) SN rates in galaxy clusters + iron/star mass ratio

  16. Time-integrated # of SNe-Ia must produce observed mass of Fe in clusters t -1.1 t -1.3 Maoz, Sharon, Gal-Yam (2010) SN rates in galaxy clusters + iron/star mass ratio

  17. How to recover the delay time distribution or… volumetric SN rates vs. redshift in field, compared to cosmic SFH

  18. SN delay time Star-formation distribution (t) history (z) time * time = SN rate (z)

  19. SN rate SFH delay time dist.

  20. 
 SNSDF0806.50, z=1.66 Poznanski et al. 2007, Graur et al. 2011 SN rate vs. redshift
 e.g.: SN rate at high z from the Subaru Deep Field


  21. 
 SN rate vs. redshift
 e.g.: SN rate at high z from the Subaru Deep Field


  22. SN rates out to z=2 and beyond with HST CLASH/ CANDELS Graur + 2014, Rodney+2015

  24. Madau & Dickinson 14

  26. How to recover the delay time distribution or… SN Rates vs. individual galaxy star-formation histories

  27. SN rate SFH delay function True also in an individual galaxy! expect. value visibility time visibility time expec. value for # SNe in N = r ∙ t given galaxy

  28. Compare observed number of SNe (0 or 1) in each galaxy to expectation value for given model DTD 0 0 0 1 0 0 0 0 0 0 0 0 0 1 0 0 0 1 0 0 0 0 1 0 0 0 0 0 0 0 0 0 0 0 0 0 1 0 0 0

  29. t -1 Maoz, Brandt, Mannucci 2012 SDSS-II SNe Ia in Stripe 82 galaxies with SDSS spectra and SFHs

  30. t -1 Maoz+11, Maoz+12, Graur & Maoz 12

  31. A SN survey among 700,000 SDSS spectra: 90 SNe Ia (Graur & Maoz 12)

  32. How to recover the delay time distribution or even… SN remnants in the LMC+SMC, viewed as a SN survey

  34. Stellar age distributions in 1836 individual LMC/SMC “ cells ” , from resolved stellar populations. Harris & Zaritzky 2004, 2009

  35. Stellar age distributions in 1836 individual LMC/SMC “ cells ” , from resolved stellar populations. Harris & Zaritzky 2004, 2009

  36. Stellar age distributions in 1836 individual LMC/SMC “ cells ” , from resolved stellar populations. Harris & Zaritzky 2004, 2009

  37. Maoz & Badenes 2010 SN remnants in the Magellanic Clouds and SADs from resolved stellar populations

  38. A consistent picture: * Wide distribution of delay times, looks like ~ t -1 (DD?) Volumetric field rates Graur+11,14,..

  39. Madau & Dickinson 14

  41. Volumetric field rates Graur+11,14,..

  42. Time-integrated SFR now matches stellar density vs. z

  43. Core-collapse SNe: “ instantaneous ” after star formation � CC SN rate must track the cosmic SFR. For standard IMF: 0.01 SNe per formed Msun. Expected CC rate vs. z now matches observations Madau & Dickinson 14

  44. A consistent picture: * Wide distribution of delay times, looks like ~ t -1 (DD?) Volumetric field rates Graur+11,14,..

  47. Questions Can we find a progenitor channel(s) that: 1. makes things that look like normal Ia ’ s and 2. makes enough of them (while satisfying progenitor population observational constraints) and 3. gives them a 1/t DTD?

  48. CC iron yields are measurable directly from the SN light curves 0.2 Msun - � 0.02 Msun � Kushnir 15

  49. Ratio of 3:1 Types II to Ibc …. Most Type II are IIP Li+ 2011 Mean iron yield pr CC SN = ¾ * 0.02 + ¼ * 0.2 = 0.065 Msun

  50. Howell+09 0.7 Msun - �

  51. Cosmic iron accumulation history

  52. Cosmic iron accumulation history

  53. all SDSS spectra, incl. ~10,000 WDs, have spectra from multiple (2-3) epochs ΔRV

  54. Observed RV distribution discriminates among models: Maoz et al. (2012), Badenes & Maoz (2012): Best-fit model for binary parameter distribution implies total WD merger rate ~ 1x10 -13 yr -1 M 1 = SN Ia rate per stellar mass in Sbc galaxies (MW)!

  55. The bivariate distribution of SN delay and explosion energy: physical link between progenitor and explosion energy Ruiter+12 Ni 56 mass or SN luminosity or stretch

  56. ~ 3 - 7% ~(1-2)x10 -3 ~33 SN-Ia/Msun Msun

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