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Finding the First Cosmic Explosions with JWST

Finding the First Cosmic Explosions with JWST. Daniel Whalen McWilliams Fellow Carnegie Mellon University. My Collaborators. Chris Fryer (LANL) Daniel Holz (LANL) Massimo Stiavelli (STSci) Alexander Heger (University of Minnesota) Candace Joggerst (LANL) Catherine Lovekin (LANL)

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Finding the First Cosmic Explosions with JWST

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  1. Finding the First Cosmic Explosions with JWST Daniel Whalen McWilliams Fellow Carnegie Mellon University

  2. My Collaborators • Chris Fryer (LANL) • Daniel Holz (LANL) • Massimo Stiavelli (STSci) • Alexander Heger (University of Minnesota) • Candace Joggerst (LANL) • Catherine Lovekin (LANL) • Lucy Frey (LANL)

  3. Birthplaces of Primordial Stars ~ 200 pc 105 - 106 Msol halos at z ~ 20

  4. Properties of the First Stars • thought to be very massive (25 - 500 solar masses) • due to inefficient H2 cooling • form in isolation (either one per halo or in binaries) • Tsurface ~ 100,000 K • extremely luminous sources of ionizing and LW photons • (> 1050 photons s-1) • 2 - 3 Myr lifetimes • no known mechanisms for mass loss -- no line-driven winds

  5. Photoevaporation of a Halo by a Pop III Star Whalen, Abel & Norman 2004, ApJ, 610, 14

  6. Primordial Ionization Front Instabilities Whalen & Norman 2008, ApJ, 675, 644

  7. Final Fates of the First Stars Heger & Woosley 2002, ApJ 567, 532

  8. Mixing & Fallback in 15 – 40 Msol Pop III SNe Joggerst, .., Whalen, et al 2010 ApJ 709, 11

  9. Mixing in 150 – 250 Msol Pop III PI SNe Joggerst & Whalen 2011, ApJ, 728, 129

  10. LANL Pop III Supernova Light Curve Effort Whalen et al. ApJ 2010a,b,c in prep • begin with 1D Pop III 15 – 40 Msol CC SN and 150 – 250 Msol • PI SN blast profiles • evolve these explosions through breakout from the surface of • the star out to 6 mo (CC SNe) or 3 yr (PI SNe) in the LANL • radiation hydro code RAGE (Radiation Adaptive Grid Eulerian) • post-process RAGE profiles with the LANL SPECTRUM code • to compute LCs and spectra • perform MC Monte Carlo models of strong GL of z ~ 20 SNe to • calculate flux boosts • convolve boosted spectra with models for absorption by the Lyman • alpha forest and JWST instrument response to determine • detection thresholds in redshift

  11. Post Processing Includes Detailed LANL Opacities atomic levels are assumed to be in equilibrium: an approximation

  12. Our Grid of Pop III SN Light Curve Models • 150, 175, 200, 225, and 250 Msol PI SN explosions, • blue and red progenitors, in modest winds and in • diffuse relic H II regions (18 models) • 15, 25, and 40 Msol CC SN explosions, red and blue • progenitors, three explosion energies in relic H II • regions only • red and blue progenitors span the range of expected • stellar structures for Pop III stars • core-collapse KEPLER blast profiles are evolved in 2D • in the CASTRO AMR code first up to shock breakout to • capture internal mixing—these profiles are then spherically • averaged and evolved in RAGE to compute LCs

  13. u150 u175 u200 u225

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

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

  16. Long-Term Light Curve Evolution

  17. Late Time Spectra spectral features after breakout may enable us to distinguish between PISN and CC SNe

  18. Conclusions • PISN will be visible to JWST out to z ~ 10 ; strong lensing may • enable their detection out to z ~ 15 (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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