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 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

Heavy elements and reddening in Gamma Ray Bursts Acknowledgements Daniela Calzetti – STScI Fiona Harrison – CalTech Tim Heckman – JHU Julian Krolik – JHU Nicola Masetti – CNR, Bologna Eliana Palazzi – CNR Bologna Nino Panagia – STScI James Rhoads – STScI Ken Sembach – STScI

Introduction GRBGRB X-ray positionErrorInstrumentX-ray AfterglowOptical TransientRadio Afterglowz h 58 m 10 s -31° 23'15'*5'Uly/MO/SAX yy h 15 m 16 s -21° 56'1'SAX/WFCyy h 34 m 25 s -76° 02'2'SAX/WFCyyy h 55 m 35 s +40° 56'20*15'HE/Uly/SAX y h 52 m 12 s +43° 01'2.5'SAX/WFCyyy h 04 m 15 s +51° 46'3'*10'Uly/Ko/NEyyy h 25 m 21 s +20° 05'4'*8'Uly/KO/NE yy C16 h 20 m 22 s +29° 25'6'*8'ASM/Uly yy h 13 m 33 s -51° 56'3.5'*16'Uly/KO/NE y h 33 m 55 s +46° 26'14*1'Uly/KO/NE yy h 31 m 50 s -73° 24'2'SAX/WFC yn h 09 m 32 s -72° 09'6'SAX/WFCyyn h 38 m 06 s -80° 30'3'SAX/WFCyyy h 54 m 41 s -26° 45'7'BAT/PCAy y h 25 m 29 s +44° 45'2'SAX/WFCyyy h 59 m 07 s +08° 35.6'4'RXTE/ASMyyy h 17 m 46 s +71° 29.9'4'SAX/WFCyyn h 34 m 54 s -52° 49.9'8'SAX/WFCySNy h 56 m 30 s +65° 12.0'4'SAX/WFCyyn h 08 m 29 s +59° 18.0'2.5'*1'RXTE/ASMyny h 53 m 28 s +79° 17.4'3'SAX/WFCyyy h 01 m 57 s +11° 46.4'3'SAX/WFCyyn0.695 This list URL: ˜ jcg/grbgen.html

Introduction GRBs vs. QSOs redshift distribution

Introduction 0.5 days m R = days m R = days m R =20.65 GRB z GRB =1.475 (Vreeswijk et al., 2001)

Introduction This list URL: ˜ jcg/grbgen.html GRBGRB X-ray positionErrorInstrumentX-ray AfterglowOptical TransientRadio Afterglowz h 58 m 10 s -31° 23'15'*5'Uly/MO/SAX yy h 15 m 16 s -21° 56'1'SAX/WFCyy h 34 m 25 s -76° 02'2'SAX/WFCyyy h 55 m 35 s +40° 56'20*15'HE/Uly/SAX y h 52 m 12 s +43° 01'2.5'SAX/WFCyyy h 04 m 15 s +51° 46'3'*10'Uly/Ko/NEyyy h 25 m 21 s +20° 05'4'*8'Uly/KO/NE yy C16 h 20 m 22 s +29° 25'6'*8'ASM/Uly yy h 13 m 33 s -51° 56'3.5'*16'Uly/KO/NE y h 33 m 55 s +46° 26'14*1'Uly/KO/NE yy h 31 m 50 s -73° 24'2'SAX/WFC yn h 09 m 32 s -72° 09'6'SAX/WFCyyn h 38 m 06 s -80° 30'3'SAX/WFCyyy h 54 m 41 s -26° 45'7'BAT/PCAy y h 25 m 29 s +44° 45'2'SAX/WFCyyy h 59 m 07 s +08° 35.6'4'RXTE/ASMyyy h 17 m 46 s +71° 29.9'4'SAX/WFCyyn h 34 m 54 s -52° 49.9'8'SAX/WFCySNy h 56 m 30 s +65° 12.0'4'SAX/WFCyyn h 08 m 29 s +59° 18.0'2.5'*1'RXTE/ASMyny h 53 m 28 s +79° 17.4'3'SAX/WFCyyy h 01 m 57 s +11° 46.4'3'SAX/WFCyyn0.695

Introduction RedshiftFWHM (Ǻ)References GRB Kulkarni et al., 1999 GRB Vreeswijk, et al., 2001 GRB Castro et al., 2001 GRB / 4.8 / 3.3–5.8 Jha et al., 2001 Masetti et al 2001 Salamanca et al., 2001

GRB z GRB = m V  20.2 Introduction (Masetti et al., 2001)

Introduction GRB z GRB = (Castro et al., 2001)

Introduction GRB z GRB = N HI  2  cm –2 (Fynbo et al., 2001)

Introduction Ly  N HI =2.3x10²º cmˉ ² 5” Z QSO = 1.41 Wavelength (Å) QSO Damped Lyman Alpha (DLA) systems QSO EX z DLA = 1.01 m V  16.4 (Le Brun et al., 1998)

[X/H] = log (N Xi /N HI )– log (X/H) (Pettini et al., 2000)  Ion log N [X/H] HI20.67±0.03 …. ZnII12.33±0.11– 0.99±0.11 SiII15.45±0.11– 0.77±0.11 CrII13.49±0.04– 0.89±0.05 FeII15.17±0.04– 1.01±0.05 MnII12.91±0.04– 1.15±0.05 Introduction

Metallicity redshift evolution QSO DLAs (Savaglio, 2000)

QSO–DLA z = FWHM = 7 km s –1 GRB–DLA z GRB = FWHM = 200 – 400 km s –1 velocity (km s –1 ) GRB–DLAs and QSO–DLAs

1.4 minutes 14.4 minutes 2.4 hours (Fruchter et al., 1999) GRB z GRB = GRB–DLAs and QSO–DLAs

760 km s –1 (Castro et al., 2001) GRB z GRB = Keck/ESI FWHM  80 km s –1 GRB–DLAs and QSO–DLAs

Heavy element column densities in GRB–DLAs Equivalent Widths of absorption lines

Heavy element column densities in GRB–DLAs Curve of growth (Spitzer, 1978) Linear part: log W r / = log (N f ) – 4.053

Heavy element column densities in GRB–DLAs

Curve of growth (Spitzer, 1978)

Heavy element column densities in GRB–DLAs

Comparison with QSO–DLAs

Heavy element column densities in GRB–DLAs Comparison with QSO–DLAs

Heavy element abundances in GRB–DLAs Relative abundances and comparison with QSO–DLAs

Heavy element abundances in GRB–DLAs Relative abundances and comparison with QSO–DLAs

Heavy element abundances in GRB–DLAs Relative abundances and comparison with QSO–DLAs

Heavy element abundances in GRB–DLAs Relative abundances and comparison with QSO–DLAs

Dust depletion correction Heavy element abundances in the Galactic ISM (Savage & Sembach 1996)

Dust depletion correction (Savaglio 2000)

Dust depletion correction GRB

Dust depletion correction GRB GRB

Dust extinction Optical extinction in solar neighborhood

Dust extinction Optical extinction in solar neighborhood

Dust extinction A V GRB GRB GRB

Dust extinction GRB z GRB = (Fynbo et al., 2001) U K A V =0.27  0.12 A V =0.18  0.06

Dust extinction Grey dust extinction in Active Nuclei (Maiolino, Marconi & Oliva, 2001)

Dust extinction (Fruchter, Krolik & Rohads, 2001) Large dust grains might be destroyed first

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: Conclusions