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GRBs, Dust, and the High-Redshift Universe

GRBs, Dust, and the High-Redshift Universe. Daniel Perley (Hubble Fellow, Caltech). GRBs: Massive Stellar Core Collapse. Extremely Luminous Transients. GRBs as Probes. GRB 050904 (z=6.295). Kawai+2006. GRB Populations as SFR Tracers. Kistler et al. 2008. Robertson & Ellis 2011. GRBs.

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GRBs, Dust, and the High-Redshift Universe

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  1. GRBs, Dust, and the High-Redshift Universe Daniel Perley (Hubble Fellow, Caltech)

  2. GRBs: Massive Stellar Core Collapse

  3. Extremely Luminous Transients

  4. GRBs as Probes GRB 050904 (z=6.295) Kawai+2006

  5. GRB Populations as SFR Tracers Kistler et al. 2008 Robertson & Ellis 2011 GRBs Behroozi et al. 2011

  6. GRB Populations as SFR Tracers Kistler et al. 2008 Robertson & Ellis 2011 GRBs Behroozi et al. 2011

  7. GRB hosts vs. SN hosts GRB host galaxies (irregular, young) SN host galaxies (spiral, mature) Fruchter+ 2006

  8. Heavily Obscured GRB 080607 Modified MW-like dust Av,rest = 3.3 ± 0.4 magAR,obs = 5.8 ± 0.7 mag z = 3.036 Perley et al. 2010b

  9. Dark GRBs ~25% of GRBs are dark: No optical afterglow, even with early follow-up. • Can't identify host without X-ray or radio follow-up. • Can't measure redshift without large ground-based telescopes. Palomar 60-inch follow-up of GRB 061222A ~10 minutes after burst

  10. Hosts of Dust-Obscured GRBs

  11. GRB hosts vs. Field Galaxies GRBs sample “all” types of star-forming galaxies, and dusty GRBs prefer dustier, more massive, more star-forming hosts... Grey points: K-selected field galaxies (Kajisawa et al. 2011) “ordinary” mildly obscured GRBs heavily obscured GRBs Extinction Stellar Mass SFR

  12. GRB hosts vs. Field Galaxies GRBs overall still strongly trend towards low-mass, low-dust, high-sSFR systems. expected population median as a function of redshift for a uniform SFR-tracer Extinction Stellar Mass SFR

  13. Moving to Higher Redshifts Improvement at higher redshifts, but a preference for the faintest and bluest galaxies persists. (Consistent with metallicity evolution?)

  14. Other Interests... Understanding the deviation: metallicity or something else? Constraints on the progenitor? Can we correct GRB rates → SFR calibrations? Effects of types of dust. (Origin of 2175 Angstrom absorption feature?) Multiwavelength view: abundance of submillimeter hosts Links to other extreme transients (luminous SNe)

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