1 / 15

Finding the First Cosmic Explosions

Finding the First Cosmic Explosions. Daniel Whalen McWilliams Fellow Carnegie Mellon University. My Collaborators. Chris Fryer (LANL) Lucy Frey (LANL) Wes Even (LANL) Daniel Holz (University of Chicago) Massimo Stiavelli (STSci) Alexander Heger (University of Minnesota)

brandi
Télécharger la présentation

Finding the First Cosmic Explosions

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

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

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

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

  4. Disk Fragmentation Pop III Protostar

  5. Properties of the First Stars (?) • thought to be very massive (25 - 500 solar masses) • due to inefficient H2 cooling • form in isolation (one per halo or in binaries) or in • small multiples • 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

  6. The First H II Regions in the Universe Whalen, Abel & Norman 2004 ApJ, 610, 14 Whalen & Norman 2006 ApJS, 162, 281 Whalen & Norman 2008a, ApJ, 672, 287 Whalen & Norman 2008b, ApJ, 673, 664

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

  8. Mixing in Pop III Supernovae Joggerst, .., Whalen, et al 2010 ApJ 709, 11 Joggerst & Whalen 2011 ApJ, 728, 129

  9. LANL Pop III Supernova Light Curve Effort Whalen et al. ApJ 2012a,b,c,d in prep • begin with 1D Pop III 15 – 40 Msol CC SN and 150 – 250 Msol • KEPLER PI SN blast profiles • evolve PI SNe out to 3 yr in the LANL radiation hydro code RAGE • (Radiation Adaptive Grid Eulerian) • evolve CC SNe out to breakout in the CASTRO AMR code, port • to RAGE, and then run out to 8 months • post-process RAGE profiles with the LANL SPECTRUM code • to compute light curves and spectra

  10. Shock Breakout

  11. Light Curves u-series (red hypergiants) z-series (blue compact giants)

  12. Spectral Evolution: z250

  13. JWST NIRCam Light Curves

  14. Some Pop III Core-Collapse SN Light Curves z25B z25B z25D z25G

  15. Conclusions • preliminary indications are that Pop III PI SNe • will be visible to JWST and TMT out to z ~ 30 • without strong lensing • Pop III CC SNe may be visible out to z ~ 7 - 10 • detections of primordial SNe will be the first direct • probe of the Pop III IMF • Pop III CC SNe will reveal many protogalaxies • that would otherwise not be detected by next • generation observatories

More Related