heavy elements and reddening in gamma ray bursts
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Heavy elements and reddening in Gamma Ray Bursts. Sandra Savaglio Johns Hopkins University In collaboration with Mike Fall (STScI) & Fabrizio Fiore (Rome Obs). Heavy elements and reddening in Gamma Ray Bursts. Sandra Savaglio Johns Hopkins University - PowerPoint PPT PresentationTRANSCRIPT
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Heavy elements and reddening in Gamma Ray Bursts
Sandra SavaglioJohns Hopkins University
In collaboration with Mike Fall (STScI) & Fabrizio Fiore (Rome Obs)
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Heavy elements and reddening in Gamma Ray Bursts
Sandra SavaglioJohns Hopkins University
In collaboration with Mike Fall (STScI) & Fabrizio Fiore (Rome Obs)
Optical spectra of GRB afterglows GRB–DLAs vs. QSO–DLAs Heavy elements and dust
Outline
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Heavy elements and reddening in Gamma Ray Bursts
Acknowledgements
Daniela Calzetti – STScIFiona Harrison – CalTechTim Heckman – JHUJulian Krolik – JHUNicola Masetti – CNR, BolognaEliana Palazzi – CNR BolognaNino Panagia – STScI James Rhoads – STScI Ken Sembach – STScI
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Introduction
GRB GRB X-ray position Error Instrument X-ray Afterglow Optical Transient Radio Afterglow z
020405 13h58m10s -31° 23' 15'*5' Uly/MO/SAX y y 0.69
011211 11h15m16s -21° 56' 1' SAX/WFC y y 2.14
011121 11h34m25s -76° 02' 2' SAX/WFC y y y 0.36
010921 22h55m35s +40° 56' 20*15' HE/Uly/SAX y 0.45
010222 14h52m12s +43° 01' 2.5' SAX/WFC y y y 1.477
000926 17h04m15s +51° 46' 3'*10' Uly/Ko/NE y y y 2.066
000418 12h25m21s +20° 05' 4'*8' Uly/KO/NE y y 1.118
000301C 16h20m22s +29° 25' 6'*8' ASM/Uly y y 2.03
000131 06h13m33s -51° 56' 3.5'*16' Uly/KO/NE y 4.5
991208 16h33m55s +46° 26' 14*1' Uly/KO/NE y y 0.706
990712 22h31m50s -73° 24' 2' SAX/WFC y n 0.434
990705 05h09m32s -72° 09' 6' SAX/WFC y y n 0.86
990510 13h38m06s -80° 30' 3' SAX/WFC y y y 1.619
990506 11h54m41s -26° 45' 7' BAT/PCA y y 1.3
990123 15h25m29s +44° 45' 2' SAX/WFC y y y 1.60
980703 23h59m07s +08° 35.6' 4' RXTE/ASM y y y 0.966
980613 10h17m46s +71° 29.9' 4' SAX/WFC y y n 1.096
980425 19h34m54s -52° 49.9' 8' SAX/WFC y SN y 0.0085
971214 11h56m30s +65° 12.0' 4' SAX/WFC y y n 3.42
970828 18h08m29s +59° 18.0' 2.5'*1' RXTE/ASM y n y 0.9578
970508 06h53m28s +79° 17.4' 3' SAX/WFC y y y 0.835
970228 05h01m57s +11° 46.4' 3' SAX/WFC y y n 0.695
This list URL: http://www.aip.de/ jcg/grbgen.html
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Introduction
GRBs vs. QSOs redshift distribution
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Introduction
0.5 daysmR=20.32
1.5 daysmR=21.11
0.7 daysmR=20.65
GRB 990712 zGRB=1.475
(Vreeswijk et al., 2001)
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IntroductionThis list URL: http://www.aip.de/ jcg/grbgen.html
GRB GRB X-ray position Error Instrument X-ray Afterglow Optical Transient Radio Afterglow z
020405 13h58m10s -31° 23' 15'*5' Uly/MO/SAX y y 0.69
011211 11h15m16s -21° 56' 1' SAX/WFC y y 2.14
011121 11h34m25s -76° 02' 2' SAX/WFC y y y 0.36
010921 22h55m35s +40° 56' 20*15' HE/Uly/SAX y 0.45
010222 14h52m12s +43° 01' 2.5' SAX/WFC y y y 1.477
000926 17h04m15s +51° 46' 3'*10' Uly/Ko/NE y y y 2.066
000418 12h25m21s +20° 05' 4'*8' Uly/KO/NE y y 1.118
000301C 16h20m22s +29° 25' 6'*8' ASM/Uly y y 2.03
000131 06h13m33s -51° 56' 3.5'*16' Uly/KO/NE y 4.5
991208 16h33m55s +46° 26' 14*1' Uly/KO/NE y y 0.706
990712 22h31m50s -73° 24' 2' SAX/WFC y n 0.434
990705 05h09m32s -72° 09' 6' SAX/WFC y y n 0.86
990510 13h38m06s -80° 30' 3' SAX/WFC y y y 1.619
990506 11h54m41s -26° 45' 7' BAT/PCA y y 1.3
990123 15h25m29s +44° 45' 2' SAX/WFC y y y 1.60
980703 23h59m07s +08° 35.6' 4' RXTE/ASM y y y 0.966
980613 10h17m46s +71° 29.9' 4' SAX/WFC y y n 1.096
980425 19h34m54s -52° 49.9' 8' SAX/WFC y SN y 0.0085
971214 11h56m30s +65° 12.0' 4' SAX/WFC y y n 3.42
970828 18h08m29s +59° 18.0' 2.5'*1' RXTE/ASM y n y 0.9578
970508 06h53m28s +79° 17.4' 3' SAX/WFC y y y 0.835
970228 05h01m57s +11° 46.4' 3' SAX/WFC y y n 0.695
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Introduction
Redshift FWHM (Ǻ) References
GRB 990123 1.6004 11.6 Kulkarni et al., 1999
GRB 990510 1.619 30 Vreeswijk, et al., 2001
GRB 000926 2.038 1.12 Castro et al., 2001
GRB 010222 1.475 6 / 4.8 / 3.3–5.8 Jha et al., 2001
Masetti et al 2001
Salamanca et al., 2001
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GRB010222 zGRB = 1.475 mV 20.2
Introduction
(Masetti et al., 2001)
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Introduction
GRB 000926 zGRB = 2.0379
(Castro et al., 2001)
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Introduction
GRB 000926 zGRB = 2.0379
NHI 21021 cm–2
(Fynbo et al., 2001)
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Introduction
Ly
NHI=2.3x10²º cmˉ ²
5”
Z QSO = 1.41
Wavelength (Å)
QSO Damped Lyman Alpha (DLA) systems
QSO EX0302-223 zDLA = 1.01mV 16.4
(Le Brun et al., 1998)
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[X/H] = log (NXi /NHI)– log (X/H)
(Pettini et al., 2000)
Ion log N [X/H]
HI 20.67±0.03 ….
ZnII 12.33±0.11 – 0.99±0.11
SiII 15.45±0.11 – 0.77±0.11
CrII 13.49±0.04 – 0.89±0.05
FeII 15.17±0.04 – 1.01±0.05
MnII 12.91±0.04 – 1.15±0.05
Introduction
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IntroductionMetallicity redshift evolution QSO DLAs
(Savaglio, 2000)
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QSO–DLA 0454+39 z = 0.8591FWHM = 7 km s–1
GRB–DLA 010222 zGRB = 1.475FWHM = 200 – 400 km s–1
velocity (km s–1 )velocity (km s–1 )
GRB–DLAs and QSO–DLAs
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1.4 minutes
14.4 minutes
2.4 hours
(Fruchter et al., 1999)
GRB 990123 zGRB = 1.6004
GRB–DLAs and QSO–DLAs
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760 km s–1
(Castro et al., 2001)
GRB000926zGRB = 2.0379Keck/ESIFWHM 80 km s–1
GRB–DLAs and QSO–DLAs
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Heavy element column densities in GRB–DLAs
Equivalent Widths of absorption lines
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Heavy element column densities in GRB–DLAs
Curve of growth (Spitzer, 1978)
Linear part: log Wr / = log (N f ) – 4.053
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Heavy element column densities in GRB–DLAs
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Heavy element column densities in GRB–DLAs
Curve of growth (Spitzer, 1978)
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Heavy element column densities in GRB–DLAs
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Heavy element column densities in GRB–DLAs
Comparison with QSO–DLAs
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Heavy element column densities in GRB–DLAs
Comparison with QSO–DLAs
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Heavy element abundances in GRB–DLAs
Relative abundances and comparison with QSO–DLAs
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Heavy element abundances in GRB–DLAs
Relative abundances and comparison with QSO–DLAs
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Heavy element abundances in GRB–DLAs
Relative abundances and comparison with QSO–DLAs
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Heavy element abundances in GRB–DLAs
Relative abundances and comparison with QSO–DLAs
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Dust depletion correction
Heavy element abundances in the Galactic ISM
(Savage & Sembach 1996)
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Dust depletion correction
(Savaglio 2000)
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Dust depletion correction
GRB 000926
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Dust depletion correction
GRB 010222 GRB 990123
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Dust extinction
Optical extinction in solar neighborhood
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Dust extinction
Optical extinction in solar neighborhood
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Dust extinction
AV
GRB 990123 1.1
GRB 000926 0.9
GRB 010222 0.6
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Dust extinction
GRB 000926 zGRB = 2.0379
(Fynbo et al., 2001)
UK
AV=0.270.12AV=0.180.06
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Dust extinction
Grey dust extinction in Active Nuclei
(Maiolino, Marconi & Oliva, 2001)
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Dust extinction
(Fruchter, Krolik & Rohads, 2001)
Large dust grains might be destroyed first
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• Absorption lines in 3 GRB –DLAs indicate column densities of metals are larger than in QSO–DLAs
• [Fe/Zn] indicates high dust depletion
• Low observed reddening in GRBs can be explained if grey extinction is assumed
• High extinction might party explain low fraction (30 – 35 %) of optical GRB afterglow detections
This talk URL: http://www.pha.jhu/˜savaglio/grb/grb.ppt
Conclusions