grb absorption spectroscopy - Inaf

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GRB080319B - FINE STRUCTURE LINE VARIABILITY Fine structure lines nearly disappear in less than 2 hours (less than 1h rest frame at z=0.937)! Fe II* 2396 Ground state lines remain constant (slight increment compatible with the decreasing of the excited levels) The strongest fine structure line variation ever found (optical depth reduced by a factor of 4 – 20) Fe II 2374
FINE STRUCTURE LINE VARIABILITY Fine structure of components III and IV drops faster than that of component I Explanation: Component I experiences higher fluxes for longer times, i.e., is the closest component to the GRB. I III+IV
Page 1 and 2: Absorption studies of GRB afterglow
Page 3 and 4: Suitable to: GRB ABSORPTION SPECTRO
Page 5 and 6: LOW - RES GRBs GRBs provide an inde
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: GRB080319B - MAIN SYSTEM: COMPONENT
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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