grb absorption spectroscopy - Inaf

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CrII groud state line is decreasing in GRB 080310 log N epII (Cr II) = 13.07 ± 0.06 log N epIV (Cr II) = 12.37 ± 0.14 (De Cia et al. 2012) PHOTOIONIZATION IN ACTION
A NEW INSTRUMENT @ THE VLT: X-SHOOTER High efficiency spectrograph at the UT2 Cassegrain focus Intermediate resolution (R = 4000-14000) Wide spectral coverage (3000-25000Å) Three arms splitting: UVB, VIS, NIR First light: Nov 2008 In operation: Oct 2009 Suitable to: • spot GRBs up to z ~ 20 • study host metallicity in a wide redshift range • follow line variations with higher temporal resolution and longer times • collect good quality GRB spectra up to R ~ 21-21.5 (short GRBs)
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 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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