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The First Cosmic Explosions

The First Cosmic Explosions. Daniel Whalen McWilliams Fellow Carnegie Mellon University Chris Fryer, Lucy Frey LANL Candace Joggerst UCSC/LANL. ~ 200 pc. Cosmological Halo z ~ 20. Transformation of the Halo Whalen, Abel & Norman 2004, ApJ, 610, 14. Chemical Mixing Prior to Breakout.

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The First Cosmic Explosions

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  1. The First Cosmic Explosions Daniel Whalen McWilliams Fellow Carnegie Mellon University Chris Fryer, Lucy Frey LANL Candace Joggerst UCSC/LANL

  2. ~ 200 pc Cosmological Halo z ~ 20

  3. Transformation of the Halo Whalen, Abel & Norman 2004, ApJ, 610, 14

  4. Chemical Mixing Prior to Breakout Core Collapse SN PISN Joggerst, Whalen, et al 2010, ApJ, 709, 11 Joggerst & Whalen 2010, ApJ in prep

  5. Primordial SNe in Relic H II Regions Whalen, Van Veelen, O’Shea & Norman ApJ 2008, 682,49 Reverse Shock Collision with the Shell

  6. Primordial SNe in Neutral Halos Late Radiative Phase Fallback

  7. Conclusions I • elemental yields of primordial SNe depend on both explosive • nucleosynthesis and mixing and fallback within the star • metals mix with primordial gas on 3 characteristic spatial • scales in primordial SNe (inside the star, 10 - 15 pc and 100 - • 200 pc) • Salpeter-type IMF averages of 15 - 40 solar mass Pop III • core-collapse SNe are the best fit to EMP star abundances • thus far, although considerable work remains • metal and dust cooling in Pop III SNe remnants may lead to • prompt second star formation

  8. LANL Pop III Supernova Light Curve Effort Whalen, Fryer & Frey, ApJ 2010a,b, in prep • LANL ASC code RAGE (Radiation Adaptive Grid Eulerian) • 1D RTP AMR radiation hydrodynamics with grey/multigroup • FLD and Implicit Monte Carlo transport • 2T models (radiation and matter not assumed to be at the same • temperature) • PISN, core-collapse, and hypernova models • post process rad hydro profiles to obtain spectra and light curves

  9. Post Processing Includes Detailed LANL Opacities but the atomic levels are assumed to be in equilibrium, a clear approximation

  10. PISN Shock Breakout • X-rays (< 1 keV) • transient (a few • hours in the local • frame)

  11. Spectra at Breakout The spectra evolve rapidly as the front cools

  12. Long-Term Light Curve Evolution

  13. Late Time Spectra spectral features after breakout may enable us to distinguish between PISN and CC SNe larger parameter study with well-resolved photospheres is now in progress

  14. Roadmap Ahead • current models are grey FLD; next step is • multigroup FLD and then multigroup IMC • advance from 1D RTP AMR calculations • to 2D cartesian AMR grids • incorporate mixing from 2D models to • simulate core-collapse SNe (15 - 40 solar • mass stars, hypernovae) • implement non-equilibrium opacities • investigate progenitor environments on • LC and spectra (LBV brightening?) • explore asymmetric explosion mechanisms • evolve toward 2D AMR IMC rad hydro • with thousands of frequency bins -- eliminate • post processing

  15. Conclusions II • PISN will be visible to JWST out to z ~ 10 - 15; strong lensing may • enable their detection out to z ~ 20 (Holz, Whalen & Fryer 2010 • ApJ in prep) • dedicated ground-based followup with 30-meter class telescopes • for primordial SNe spectroscopy • discrimination between Pop III PISN and Pop III CC SNe will be • challenging but offers the first direct constraints on the Pop III IMF • complementary detection of Pop III PISN remnants by the SZ effect • may be possible (Whalen, Bhattacharya & Holz 2010, ApJ in prep)

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