grb absorption spectroscopy - Inaf

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LOW – RES GRBs GRBs represent a new tool to study high-z galaxies The ISM gives us precious information on the metal enrichment history of the galaxies, which in turn is linked to the mass function evolution. In the past, metal enrichment in galaxies at high z has been studied using: • Lyman Break Galaxies • Galaxies along the line of sight of quasars (Damped Lyman-α systems) The first class cannot be representative of the true galaxy population The second one is entangled by selection effects: the radiation from the QSOs probes preferentially the halos of the galaxies.
LOW – RES GRBs GRBs provide an independent way of studing the metal enrichment of galaxies at z > 1. Advantages: • Probing central galaxy regions • No luminosity bias • ISM can be studied up to higher redshift than DLA systems. GRB-DLAs appear to be more metal rich than QSO-DLAs (Savaglio 2005 and 2010; Prochaska et al. 2007) Savaglio 2010
Page 1 and 2: Absorption studies of GRB afterglow
Page 3: Suitable to: GRB ABSORPTION SPECTRO
Page 7 and 8: Advantages: Piranomonte et al. 2008
Page 9 and 10: FINE STRUCTURE FEATURES The gross s
Page 11: GRB 060418: VARIABILITY Fine struct
Page 14 and 15: CrII groud state line is decreasing
Page 18 and 19: OVI Lyβ SII NiII NV NiII Lyα OI/S
Page 20 and 21: MAIN SYSTEM METALLICITY Ly_α Missi
Page 26 and 27: CONCLUSIONS GRBs are a new tool to
Page 28 and 29: GRB explosion site Host gas far awa
Page 32 and 33: GRB 050730 The main system presents
Page 34 and 35: GRB 050730 Fine structure transitio
Page 36: GRB 050730 Second component: UV pum
Page 39 and 40: GRB080319B - MAIN SYSTEM: COMPONENT
Page 41 and 42: GRB080319B - MAIN SYSTEM: COMPONENT
Page 43 and 44: FINE STRUCTURE LINE VARIABILITY Fin
Page 45: GRB080319B - TIME DEPENDENT MODELIN
Page 48 and 49: GRB080330 - MAIN SYSTEM: COMPONENTS
Page 51 and 52: INTERVENING ABSORBERS GRB Strong Mg
Page 53 and 54: FINE STRUCTURE AND EXCITED LINES Id

grb absorption spectroscopy - Inaf

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