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Observations of Cosmic Dust Evolution Using GRB Afterglows : The 2175 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

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Observations of Cosmic Dust Evolution Using GRB Afterglows:

The 2175 Å Carrier at z~3 and Supernova Dust at z~5

Daniel Perley (UC Berkeley)

2009 年 04 月 22 日

Deciphering the Ancient Universe with Gamma-Ray Bursts

arXiv:0912.2229

ApJL 691:27 ApJ 701:63 ApJL 691:27 ApJ 701:63

GRB 080607 GRB 071025

京都 , 日本

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

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

  • bservational 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 = λβ)

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Curves

S M C L M C MW

( d i f f u s e I S M )

Starburst galaxies

  • p

t i c a l I R

UV

Introduction

Varying slopes (reddening per dimming) “2175 Å bump”: can be dominant

  • r totally absent

Aλ = 1.09 τ(λ)

  • Normalized to 5500Å

(AV)

  • Considerable local

variation, esp. in UV

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

GRB 080607

contributions from:

Jason X. Prochaska Yaron Sheffer Josh Bloom Adam Miller Adam Morgan Mo Ganeshalingam Weidong Li Adria Updike

(+ others)

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.

Keck PAIRITEL KAIT SuperLOTIS

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

A Phenomenal Burst

  • 15-150 keV fluence:

S = 2.32 × 10-5 erg/cm2 (7th highest of Swift mission)

  • z = 3.038!
  • Eiso = 1.87 × 1054 erg (highest of Swift mission?)
  • Liso,max = 2.27 × 1054 erg/s

(Konus-Wind, Golenetskii et al. GCN 7862)

GRB 080607

time (s)

40 80 120

BAT light curve

(from Swift burst analyzer)

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Afterglow

GRB 080607

K H J I clear V White

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Afterglow

GRB 080607

K H J I R V White

Peak observed magnitude: R~16, K~11.5

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Spectrum

Occurred during

  • ur Keck/LRIS

night (classical,

GRB host galaxies)

t = 20-120 min

low resolution, 3800-9200 Å

z = 3.036

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Ionic Lines

z = 3.036

Germanium Copper Sulfur Silicon Carbon Potassium Nickel Carbon GalliumLead Iron Cobalt Manganese Aluminum Titanium Zinc Nickel Silicon Hydrogen (Ly α) Magnesium Chlorine Phosphorous Chromium ??? ???

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Ionic Lines

z = 3.036

Germanium Copper Sulfur Silicon Carbon Potassium Nickel Carbon GalliumLead Iron Cobalt Manganese Aluminum Titanium Zinc Nickel Silicon Hydrogen (Ly α) Magnesium Chlorine Phosphorous Chromium ??? ???

GRB 080607

Z > solar Z > solar _ _

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Molecular Lines

z = 3.036

Germanium Copper Sulfur Silicon Carbon Potassium Nickel Carbon GalliumLead Iron Cobalt Manganese Aluminum Titanium Zinc Nickel Silicon Hydrogen (Ly α) Carbon Monoxide Magnesium Chlorine Molecular hydrogen (H2) Phosphorous Chromium ??? ??? Carbon Monoxide

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Vibrationally Excited H2

z = 3.036

Germanium Copper Sulfur Silicon Carbon Potassium Nickel Carbon GalliumLead Iron Cobalt Manganese Aluminum Titanium Zinc Nickel Silicon Hydrogen (Ly α) Carbon Monoxide Magnesium Chlorine Molecular hydrogen (H2) Phosphorous Chromium ??? ??? Carbon Monoxide

d = 230–940 pc d = 230–940 pc

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Curvature

z = 3.036

Germanium Copper Sulfur Silicon Carbon Potassium Nickel Carbon GalliumLead Iron Cobalt Manganese Aluminum Titanium Zinc Nickel Silicon Hydrogen (Ly α) Carbon Monoxide Magnesium Chlorine Molecular hydrogen (H2) Phosphorous Chromium ??? ??? Carbon Monoxide

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Spectral Energy Distribution

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Spectral Energy Distribution

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Modeling

SMC Calzetti

(starburst)

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Modeling

SMC Calzetti Milky Way LMC

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Modeling

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

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Law

GRB 080607

S M C L M C MW

( d i f f u s e I S M )

Starburst galaxies G R B 8 6 7

Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 c4 = 0.3 ± 0.1

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Law

GRB 080607

S M C L M C MW

( d i f f u s e I S M )

Starburst galaxies G R B 8 6 7

Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 c4 = 0.3 ± 0.1 ▪ Very large extinction column

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Law

GRB 080607

S M C L M C MW

( d i f f u s e I S M )

Starburst galaxies G R B 8 6 7

Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 c4 = 0.3 ± 0.1 ▪ Very large extinction column ▪ Relatively UV-grey (many large particles)

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Law

GRB 080607

S M C L M C MW

( d i f f u s e I S M )

Starburst galaxies G R B 8 6 7

Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 c4 = 0.3 ± 0.1 ▪ Very large extinction column ▪ Relatively UV-grey (many large particles) ▪ 2175 Å bump weak but present

G R B 8 6 7

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Law

GRB 080607

S M C L M C MW

( d i f f u s e I S M )

Starburst galaxies G R B 8 6 7

Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 c4 = 0.3 ± 0.1 ▪ Very large extinction column ▪ Relatively UV-grey (many large particles) ▪ 2175 Å bump weak but present

M W

(Rv ~ 5 molecular cloud)

Similar to Similar to Galactic Galactic molecular molecular cloud cloud sightlines. sightlines.

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Summary

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.

GRB 080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

GRB 080607

contributions from:

Christopher Klein Josh Bloom Stefano Covino Takeo Minezaki

  • P. Wozniak

Thomas Vestrand Grant Williams Thomas Kruhler Adria Updike

(+ others)

GRB 071025

Supporting Evidence for a Transition in Dust Properties in the first ~1 Gyr

MNRAS MNRAS in press (arXiv/0912.2999) in press (arXiv/0912.2999)

PAIRITEL REM MAGNUM RAPTOR Kuiper GROND

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Light Curve

GRB 071025

K H J I clear Y R XRT

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Spectral Energy Distribution

R-band faintness cannot be reproduced by any dust model: photometric redshift

z = 4.8 ± 0.4

GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Spectral Energy Distribution

R-band faintness cannot be reproduced by any dust model: photometric redshift

z = 4.8 ± 0.4

GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Spectral Energy Distribution

GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Spectral Energy Distribution

SED is inflected: flattens around λrest ~ 2000 Å I-band faintness is not due to DLA (HIRES spectrum) GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Modeling

Milky Way LMC

GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Modeling

Milky Way LMC SMC

GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Modeling

Milky Way LMC SMC Maiolino

Empirical law from a SDSS z=6.2 quasar: well fit by models of dust from Type II SNe

Av = 0.55 ± 0.1

GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction law

GRB 071025

S M C L M C MW

( d i f f u s e I S M )

Starburst galaxies Maiolino

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Is it real?

The significance of this critically depends on accurate calibration and understanding of systematic uncertainties!

e.g., GRB 050904: Stratta et al. : Maiolino dust Kann et al. : no dust Gou et al. : no dust Liang and Li : 2175 A bump? Zafar: no dust

GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Is it real?

The significance of this critically depends on accurate calibration and understanding of systematic uncertainties!

e.g., GRB 050904: Stratta et al. : Maiolino dust Kann et al. : no dust Gou et al. : no dust Liang and Li : 2175 A bump? Zafar: no dust

SED features do not change with time and are seen with multiple instruments in geographically different locations.

GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Is it real?

The significance of this critically depends on accurate calibration and understanding of systematic uncertainties!

e.g., GRB 050904: Stratta et al. : Maiolino dust Kann et al. : no dust Gou et al. : no dust Liang and Li : 2175 A bump?

SED features do not change with time and are seen with multiple instruments in geographically different locations.

GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Is it real?

The significance of this critically depends on accurate calibration and understanding of systematic uncertainties!

e.g., GRB 050904: Stratta et al. : Maiolino dust Kann et al. : no dust Gou et al. : no dust Liang and Li : 2175 A bump? Zafar: no dust

Examined: zeropoint uncertainty 2MASS survey systematic uncertainty instrumental color terms variable atmospheric absorption non-power law intrinsic spectrum strong DLA at z=5.2

none of these are significant enough to generate the observed effect. SED features do not change with time and are seen with multiple instruments in geographically different locations.

GRB 071025

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Dust Transition at High z?

z = 0 z = 2 z = 4 z = 6 Gray

Featureless, shallow Featureless, steep Shallow w/ 2175 Maiolino plateau Steep w/ 2175

Milky Way (mean) Milky Way (clouds) LMC SMC SDSS quasars GRB 061126 GRB 051111 GRB 071025 GRB 080607 AGN? BAL QSOs Nearby spirals SN hosts Lensing galaxies Nearby starbursts GRB 070802

Poznanski et al. 2009, Elias-Rosa et al. 2006 Calzetti et al. 1994 Butler et al. 2007

most GRBs

Schady et al. 2010, Kann et al. 2007 Perley et al. 2010 Maiolino et al. 2004 Perley et al. 2008 Hopkins et al. 2004 Gaskell et al. 2007 Prochaska et al. 2009 Eliasdottir et al. 2009 Falco et al. 2009 Keel & White 2001, Bianchi et al. 1996

Conclusions E x t i n c t i

  • n

L a w C l a s s Redshift

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Dust Transition at High z?

z = 0 z = 2 z = 4 z = 6 Gray

Featureless, shallow Featureless, steep Shallow w/ 2175 Maiolino plateau Steep w/ 2175

Milky Way (mean) Milky Way (clouds) LMC SMC SDSS quasars GRB 061126 GRB 051111 GRB 071025 GRB 080607 AGN? BAL QSOs Nearby spirals SN hosts Lensing galaxies Nearby starbursts GRB 070802

Poznanski et al. 2009, Elias-Rosa et al. 2006 Calzetti et al. 1994 Butler et al. 2007

most GRBs

Schady et al. 2010, Kann et al. 2007 Perley et al. 2010 Maiolino et al. 2004 Perley et al. 2008 Hopkins et al. 2004 Gaskell et al. 2007 Prochaska et al. 2009 Eliasdottir et al. 2009 Falco et al. 2009 Keel & White 2001, Bianchi et al. 1996

Conclusions E x t i n c t i

  • n

L a w C l a s s Redshift

t > 1 Gyr: z < 5 z < 5 Dust forms in AGB stars t < 1 Gyr: z > 5 Dust forms in SNe? Dust forms in SNe?

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Dust Transition at High z?

z = 0 z = 2 z = 4 z = 6 Gray

Featureless, shallow Featureless, steep Shallow w/ 2175 Maiolino plateau Steep w/ 2175

Milky Way (mean) Milky Way (clouds) LMC SMC SDSS quasars GRB 061126 GRB 051111 GRB 071025 GRB 080607 AGN? BAL QSOs Nearby spirals SN hosts Lensing galaxies Nearby starbursts GRB 070802

Poznanski et al. 2009, Elias-Rosa et al. 2006 Calzetti et al. 1994 Butler et al. 2007

most GRBs

Schady et al. 2010, Kann et al. 2007 Perley et al. 2010 Maiolino et al. 2004 Perley et al. 2008 Hopkins et al. 2004 Gaskell et al. 2007 Prochaska et al. 2009 Eliasdottir et al. 2009 Falco et al. 2009 Keel & White 2001, Bianchi et al. 1996

Conclusions E x t i n c t i

  • n

L a w C l a s s Redshift

t > 1 Gyr: z < 5 z < 5 Dust forms in AGB stars t < 1 Gyr: z > 5 Dust forms in SNe? Dust forms in SNe?

Too early to be sure, but trend is intriguing!

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Conclusions

  • Diffuse MW / LMC / SMC is not the whole story
  • 080607: Galactic-like molecular cloud at z=3

with weaker 2175 Å carrier

  • 071025: Plenty of dust at z=5, extinction law

resembles z>5 quasars and modeled dust from Type II Sne

  • SN → AGB production transition at z~5?

Conclusions

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Law

GRB 080607

S M C L M C MW

( d i f f u s e I S M )

Starburst galaxies G R B 8 6 7 M W

(Rv ~ 5 molecular cloud)

Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 c4 = 0.3 ± 0.1 c2 (UV steepness) c3 (2175 bump strength)

ONC diffuse diffuse MW MW LMC LMC SMC SMC

080607

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Observations of Cosmic Dust Evolution using GRBs Daniel Perley 2009 年 04 月 22 日

Extinction Law

GRB 080607

S M C L M C MW

( d i f f u s e I S M )

Starburst galaxies G R B 8 6 7 M W

(Rv ~ 5 molecular cloud)

Av = 3.2 ± 0.5 Rv = 4.0 ± 0.2 c3 = 1.3 ± 0.3 c4 = 0.3 ± 0.1 c2 (UV steepness) c3 (2175 bump strength)

ONC diffuse diffuse MW MW LMC LMC SMC SMC

080607

Typical MW-like values, Typical MW-like values, except: except: Large Rv: dense ISM Large Rv: dense ISM (like a molecular cloud!) (like a molecular cloud!) Low but Low but nonzero nonzero c3: c3: presence of 2175 presence of 2175 Å Å carrier carrier (graphite grains?) (graphite grains?)