Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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:0912.2229ApJL 691:27 ApJ 701:63ApJL 691:27 ApJ 701:63

GRB 080607 GRB 071025

京都 , 日本

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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

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 = λβ)

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction Curves

SMC

LMC M

W

(diff

use

ISM

)

Starburst galaxies

opt

ica

l

IR

UV

Introduction

Varying slopes (reddening per dimming)

“2175 Å bump”: can be dominant or totally absent

Aλ = 1.09 τ(λ)

- Normalized to 5500Å (A

V)

- Considerable local variation, esp. in UV

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

GRB 080607

contributions from:

Jason X. Prochaska Yaron Sheffer Josh BloomAdam MillerAdam MorganMo GaneshalingamWeidong LiAdria Updike(+ others)

GRB 080607

An Ultra-Energetic Burst Piercing a Milky Way-like Molecular Cloud 2 Billion Years after the Big Bang

•• ApJL 691:27ApJL 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

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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)0 40 80 120

BAT light curve (from Swift burst analyzer)

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

AfterglowGRB 080607

K

H

JI

clearV

White

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

AfterglowGRB 080607

K

H

J

IR

V

White

Peak observed magnitude:

R~16, K~11.5

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Spectrum

Occurred during our Keck/LRIS night (classical, GRB host galaxies)

t = 20-120 min

low resolution, 3800-9200 Å

z = 3.036

GRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Ionic Lines

z = 3.036

Germanium

Copper

Sulfur

Silicon

Carbon

Potassium

Nickel

Carbon

GalliumLeadIron

Cobalt

Manganese

Aluminum

Titanium Zinc

Nickel

Silicon

Hydrogen (Ly α)

Magnesium

Chlorine

Phosphorous

Chromium

???

???

GRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Ionic Lines

z = 3.036

Germanium

Copper

Sulfur

Silicon

Carbon

Potassium

Nickel

Carbon

GalliumLeadIron

Cobalt

Manganese

Aluminum

Titanium Zinc

Nickel

Silicon

Hydrogen (Ly α)

Magnesium

Chlorine

Phosphorous

Chromium

???

???

GRB 080607

Z > solarZ > solar__

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Molecular Lines

z = 3.036

Germanium

Copper

Sulfur

Silicon

Carbon

Potassium

Nickel

Carbon

GalliumLeadIron

Cobalt

Manganese

Aluminum

Titanium Zinc

Nickel

Silicon

Hydrogen (Ly α)

Carbon Monoxide

Magnesium

Chlorine

Molecular hydrogen

(H2)

Phosphorous

Chromium

???

???

Carbon Monoxide

GRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Vibrationally Excited H2

z = 3.036

Germanium

Copper

Sulfur

Silicon

Carbon

Potassium

Nickel

Carbon

GalliumLeadIron

Cobalt

Manganese

Aluminum

Titanium Zinc

Nickel

Silicon

Hydrogen (Ly α)

Carbon Monoxide

Magnesium

Chlorine

Molecular hydrogen

(H2)

Phosphorous

Chromium

???

???

Carbon Monoxide

d = 230–940 pcd = 230–940 pc

GRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Curvature

z = 3.036

Germanium

Copper

Sulfur

Silicon

Carbon

Potassium

Nickel

Carbon

GalliumLeadIron

Cobalt

Manganese

Aluminum

Titanium Zinc

Nickel

Silicon

Hydrogen (Ly α)

Carbon Monoxide

Magnesium

Chlorine

Molecular hydrogen

(H2)

Phosphorous

Chromium

???

???

Carbon Monoxide

GRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Spectral Energy DistributionGRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Spectral Energy DistributionGRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction Modeling

SMC

Calzetti(starburst)

GRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction Modeling

SMC

Calzetti

Milky Way

LMC

GRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction Modeling

SMC

Calzetti

Milky Way

LMC

Solve for extinction law using general Fitzpatrick parameters:

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

GRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction LawGRB 080607

SMC

LMC M

W

(diff

use

ISM

)

Starburst galaxies

GRB 080607

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

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction LawGRB 080607

SMC

LMC M

W

(diff

use

ISM

)

Starburst galaxies

GRB 080607

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

▪ Very large extinction column

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction LawGRB 080607

SMC

LMC M

W

(diff

use

ISM

)

Starburst galaxies

GRB 080607

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

▪ Very large extinction column

▪ Relatively UV-grey (many large particles)

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction LawGRB 080607

SMC

LMC M

W

(diff

use

ISM

)

Starburst galaxies

GRB 080607

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

▪ Very large extinction column

▪ Relatively UV-grey (many large particles)

▪ 2175 Å bump weak but present

GRB 080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction LawGRB 080607

SMC

LMC M

W

(diff

use

ISM

)

Starburst galaxies

GRB 080607

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

▪ Very large extinction column

▪ Relatively UV-grey (many large particles)

▪ 2175 Å bump weak but present

MW

(Rv

~ 5

mole

cula

r

cloud)

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

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

GRB 080607

contributions from:

Christopher Klein Josh BloomStefano CovinoTakeo MinezakiP. WozniakThomas VestrandGrant WilliamsThomas KruhlerAdria Updike(+ others)

GRB 071025

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

MNRASMNRAS in press (arXiv/0912.2999) in press (arXiv/0912.2999)

PAIRITEL

REM

MAGNUM

RAPTOR

Kuiper

GROND

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Light CurveGRB 071025

KHJ

Iclear

Y

R

XRT

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Spectral Energy Distribution

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

photometric redshiftz = 4.8 ± 0.4

GRB 071025

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Spectral Energy Distribution

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

photometric redshiftz = 4.8 ± 0.4

GRB 071025

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Spectral Energy DistributionGRB 071025

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Spectral Energy Distribution

SED is inflected: flattens around λ

rest ~ 2000 Å

I-band faintness is not due to DLA (HIRES spectrum)

GRB 071025

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction Modeling

Milky Way

LMC

GRB 071025

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction Modeling

Milky Way

LMC

SMC

GRB 071025

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction Modeling

Milky Way

LMC

SMC

MaiolinoEmpirical 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

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction lawGRB 071025

SMC

LMC

MW

(d

iffus

e IS

M)

Starburst galaxies

Maiolino

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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 dustKann et al. : no dustGou et al. : no dustLiang and Li : 2175 A bump?

Zafar: no dust

GRB 071025

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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 dustKann et al. : no dustGou et al. : no dustLiang 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

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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 dustKann et al. : no dustGou et al. : no dustLiang and Li : 2175 A bump?

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

GRB 071025

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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 dustKann et al. : no dustGou et al. : no dustLiang and Li : 2175 A bump?

Zafar: no dust

Examined:zeropoint uncertainty2MASS survey systematic uncertaintyinstrumental color termsvariable atmospheric absorptionnon-power law intrinsic spectrumstrong 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

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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

SMCSDSS

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 GRBsSchady 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. 2009Keel & White 2001, Bianchi et al. 1996

ConclusionsE

xtin

cti

on

Law

Cla

ss

Redshift

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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

SMCSDSS

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 GRBsSchady 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. 2009Keel & White 2001, Bianchi et al. 1996

ConclusionsE

xtin

cti

on

Law

Cla

ss

Redshift

t > 1 Gyr: z < 5z < 5

Dust forms in AGB stars

t < 1 Gyr: z > 5

Dust forms in SNe?Dust forms in SNe?

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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

SMCSDSS

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 GRBsSchady 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. 2009Keel & White 2001, Bianchi et al. 1996

ConclusionsE

xtin

cti

on

Law

Cla

ss

Redshift

t > 1 Gyr: z < 5z < 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!

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 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

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction LawGRB 080607

SMC

LMC M

W

(diff

use

ISM

)

Starburst galaxies

GRB 080607

MW

(Rv

~ 5

mole

cula

r

cloud)

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

c2 (UV steepness)

c3 (

2175

bum

p st

reng

th)

ON

C

diffuse diffuse MWMW

LMCLMC

SMCSMC080607

Observations of Cosmic Dust Evolution using GRBsDaniel Perley2009 年 04 月 22 日

Extinction LawGRB 080607

SMC

LMC M

W

(diff

use

ISM

)

Starburst galaxies

GRB 080607

MW

(Rv

~ 5

mole

cula

r

cloud)

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

c2 (UV steepness)

c3 (

2175

bum

p st

reng

th)

ON

C

diffuse diffuse MWMW

LMCLMC

SMCSMC080607

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 nonzerononzero c3: c3: presence of 2175 presence of 2175 ÅÅ carrier carrier (graphite grains?) (graphite grains?)