Observations of Cosmic Dust Evolution Using GRB Afterglows : The 2175 Å Carrier at z~3 and Supernova Dust at z~5 GRB 080607 GRB 071025 ApJL 691:27 ApJ 701:63 ApJL 691:27 ApJ 701:63 arXiv:0912.2229 Daniel Perley (UC Berkeley) 京都 , 日本 2009 年 04 月 22 日 Deciphering the Ancient Universe with Gamma-Ray Bursts 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Introduction ● How does high-z dust differ from local dust? – How much dust at z>3,4,5? (When did most of it form?) – Does it have the same composition, size distribution, and observational signatures as dust today? – What can it tell us about conditions in early galaxies? ● GRBs: excellent tools for probing high-z dust – Extremely luminous: visible to extreme redshifts – Occur in “typical” star-forming galaxies – Intrinsically simple spectrum (F = λ β ) 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Extinction Curves Introduction A λ = 1.09 τ (λ) UV - Normalized to 5500Å MW “2175 Å bump”: C e M s (A V ) can be dominant u S ) C f M f i M d S or totally absent ( - Considerable local I L variation, esp. in UV l a Starburst galaxies c R i t I p o Varying slopes (reddening per dimming) 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
GRB 080607 GRB 080607 An Ultra-Energetic Burst Piercing a Milky Way-like Molecular Cloud 2 Billion Years after the Big Bang • ApJL 691:27 ApJL 691:27 (arXiv/0901.0556) (arXiv/0901.0556) • • ApJ 701:63 ApJ 701:63 (arXiv/0907.1285) (arXiv/0907.1285) • • • Add'l work in prep. Add'l work in prep. contributions from: Jason X. Prochaska Yaron Sheffer Keck Josh Bloom PAIRITEL Adam Miller Adam Morgan KAIT Mo Ganeshalingam SuperLOTIS Weidong Li Adria Updike (+ others) 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
A Phenomenal Burst GRB 080607 ● 15-150 keV fluence: S = 2.32 × 10 -5 erg/cm 2 (7th highest of Swift mission) ● z = 3.038! ● E iso = 1.87 × 10 54 erg (highest of Swift mission?) ● L iso,max = 2.27 × 10 54 erg/s BAT light curve (from Swift burst analyzer) (Konus-Wind, Golenetskii et al. GCN 7862) 0 40 80 120 time (s) 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Afterglow GRB 080607 K H J I clear V White 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Afterglow GRB 080607 Peak observed magnitude: K R~16, K~11.5 H J I R V White 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Spectrum GRB 080607 Occurred during our Keck/LRIS z = 3.036 night (classical, GRB host galaxies) t = 20-120 min low resolution, 3800-9200 Å 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Ionic Lines GRB 080607 Carbon Chlorine Nickel Copper Potassium z = 3.036 Carbon Silicon Sulfur Hydrogen (Ly α) ??? GalliumLead Phosphorous Magnesium Aluminum Iron Germanium Silicon Chromium ??? Titanium Zinc Cobalt Nickel Manganese 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Ionic Lines GRB 080607 Carbon Chlorine Nickel Copper Potassium z = 3.036 Carbon Silicon Sulfur Hydrogen (Ly α) ??? GalliumLead Phosphorous Magnesium Aluminum Iron Germanium Silicon Chromium ??? Titanium Zinc Cobalt Nickel _ _ Z > solar Z > solar Manganese 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Molecular Lines GRB 080607 Carbon Chlorine Nickel Copper Potassium z = 3.036 Carbon Molecular hydrogen Silicon (H 2 ) Sulfur Hydrogen (Ly α) Carbon Monoxide ??? GalliumLead Phosphorous Magnesium Aluminum Iron Germanium Silicon Chromium ??? Titanium Zinc Cobalt Carbon Monoxide Nickel Manganese 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Vibrationally Excited H 2 GRB 080607 Carbon Chlorine Nickel Copper Potassium z = 3.036 Carbon Molecular hydrogen Silicon (H 2 ) Sulfur Hydrogen (Ly α) Carbon Monoxide ??? GalliumLead Phosphorous Magnesium Aluminum Iron Germanium Silicon Chromium ??? Titanium Zinc Cobalt Carbon Monoxide Nickel d = 230–940 pc d = 230–940 pc Manganese 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Curvature GRB 080607 Carbon Chlorine Nickel Copper Potassium z = 3.036 Carbon Molecular hydrogen Silicon (H 2 ) Sulfur Hydrogen (Ly α) Carbon Monoxide ??? GalliumLead Phosphorous Magnesium Aluminum Iron Germanium Silicon Chromium ??? Titanium Zinc Cobalt Carbon Monoxide Nickel Manganese 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Spectral Energy Distribution GRB 080607 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Spectral Energy Distribution GRB 080607 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Extinction Modeling GRB 080607 SMC Calzetti (starburst) 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Extinction Modeling GRB 080607 SMC Calzetti Milky Way LMC 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Extinction Modeling GRB 080607 SMC Calzetti Milky Way LMC Solve for extinction law using general Fitzpatrick parameters: Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 c4 = 0.3 ± 0.1 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Extinction Law GRB 080607 Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 MW C e c4 = 0.3 ± 0.1 M s u S ) C f M f i M d S ( I L Starburst galaxies 7 0 6 0 8 0 B R G 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Extinction Law GRB 080607 Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 MW C e c4 = 0.3 ± 0.1 M s u S ) C f M f i M d S ( I L ▪ Very large extinction column Starburst galaxies 7 0 6 0 8 0 B R G 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Extinction Law GRB 080607 Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 MW C e c4 = 0.3 ± 0.1 M s u S ) C f M f i M d S ( I L ▪ Very large extinction column Starburst galaxies ▪ Relatively UV-grey (many large 7 0 6 0 8 0 B R G particles) 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Extinction Law GRB 080607 Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 MW C e c4 = 0.3 ± 0.1 M s u S ) C f M f i M d S ( I L ▪ Very large extinction column Starburst galaxies ▪ Relatively UV-grey (many large 7 7 0 0 6 6 0 0 8 8 0 0 B B R R G G particles) ▪ 2175 Å bump weak but present 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Extinction Law GRB 080607 Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 MW C e c4 = 0.3 ± 0.1 M s u S ) C f M f i M d S ( I L ▪ Very large Similar to Similar to extinction Galactic Galactic column Starburst galaxies molecular molecular W (Rv ~ 5 ▪ Relatively molecular M cloud cloud UV-grey cloud) (many large 7 0 6 sightlines. 0 sightlines. 8 0 B R G particles) ▪ 2175 Å bump weak but present 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Summary GRB 080607 GRB 080607: ● Large dust column in star-forming galaxy at z>3 ● Probing sightline through molecular cloud ● Solar metallicity, dust resembles MW, LMC but not SMC, suggesting similar conditions to now: mature, dusty star-forming galaxy? ● Highest-redshift detection of 2175Å feature: carrier was formed (in part) by t = 2 Gyr. 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
GRB 080607 GRB 071025 Supporting Evidence for a Transition in Dust Properties in the first ~1 Gyr MNRAS in press (arXiv/0912.2999) in press (arXiv/0912.2999) MNRAS contributions from: Christopher Klein PAIRITEL Josh Bloom REM Stefano Covino Takeo Minezaki MAGNUM P. Wozniak RAPTOR Thomas Vestrand Grant Williams Kuiper Thomas Kruhler GROND Adria Updike (+ others) 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Light Curve GRB 071025 XRT K H J clear I Y R 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Spectral Energy Distribution GRB 071025 R-band faintness cannot be reproduced by any dust model: photometric redshift z = 4.8 ± 0.4 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Spectral Energy Distribution GRB 071025 R-band faintness cannot be reproduced by any dust model: photometric redshift z = 4.8 ± 0.4 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
Spectral Energy Distribution GRB 071025 2009 年 04 月 22 日 Daniel Perley Observations of Cosmic Dust Evolution using GRBs
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