observations of cosmic dust evolution using grb …inoue/grb2010web/...2009 年 04 月 22 日 daniel...
TRANSCRIPT
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
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?)