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The First Cosmic Explosions Daniel Whalen McWilliams Fellow Carnegie Mellon University Chris Fryer, Lucy Frey LANL Candace Joggerst UCSC/LANL QuickTime™ and a TIFF(Uncompressed) decompressor are needed to see this pi cture. QuickT i me™ and a T IFF (Uncompressed) decom pressor are needed to see this picture. ~ 200 pc Cosmological Halo z ~ 20 Transformation of the Halo Whalen, Abel & Norman 2004, ApJ, 610, 14 QuickTime™ and a YUV420 codec decompressor are needed to see this picture. Chemical Mixing Prior to Breakout Core Collapse SN PISN Joggerst, Whalen, et al 2010, ApJ, 709, 11 Joggerst & Whalen 2010, ApJ in prep Primordial SNe in Relic H II Regions Whalen, Van Veelen, O’Shea & Norman ApJ 2008, 682,49 Reverse Shock Collision with the Shell Primordial SNe in Neutral Halos Late Radiative Phase Fallback 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 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 Post Processing Includes Detailed LANL Opacities but the atomic levels are assumed to be in equilibrium, a clear approximation PISN Shock Breakout • X-rays (< 1 keV) • transient (a few hours in the local frame) Spectra at Breakout The spectra evolve rapidly as the front cools Long-Term Light Curve Evolution 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 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 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)