UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: Probing the features of the GRB environment

V. D'Elia, F. Fiore, E. J.A. Meurs, G. Chincarini, A. Melandri, L. Nord, L. Pellizza, R. Perna, S. Piranomonte, L. Sbordone, L. Stella, G. Tagliaferri, S. D. Vergani, P. Ward, L. Angelini, L. A. Antonelli, D. N. Burrows, S. Campana, M. Capalbi, A. CimattiE. Costa, G. Cusumano, M. Della Valle, P. Filliatre, A. Fontana, F. Frontera, D. Fugazza, N. Gehrels, T. Giannini, P. Giommi, P. Goldoni, D. Guetta, G. Israel, D. Lazzati, D. Malesani, G. Marconi, K. Mason, S. Mereghetti, F. Mirabel, E. Molinari, A. Moretti, J. Nousek, M. Perri, L. Piro, G. Stratta, V. Testa, M. Vietri

Research output: Contribution to journalArticle

40 Citations (Scopus)

Abstract

Aims. The aim of this paper is to study the Gamma Ray Burst (GRB) environment through the analysis of the optical absorption features due to the gas surrounding the GRB. Methods. To this purpose we analyze high resolution spectroscopic observations (R = 20 000-45 000, corresponding to 14 km s -1 at 4200 Å and 6.6 km s-1 at 9000 Å) of the optical afterglow of GRB050730, obtained with UVES@VLT ∼4 h after the GRB trigger. Results. The spectrum shows that the ISM of the GRB host galaxy at z = 3.967 is complex, with at least five components contributing to the main absorption system. We detect strong C II*, Si IIz.ast;, O Iz.ast; and Fe IIz.ast; fine structure absorption lines associated to the second and third component. Conclusions. For the first three components we derive information on the relative distance from the site of the GRB explosion. Component 1, which has the longest wavelength, highest positive velocity shift, does not present any fine structure nor low ionization lines; it only shows very high ionization features, such as CIV and O VI, suggesting that this component is very close to the GRB site. From the analysis of low and high ionization lines and fine structure lines, we find evidences that the distance of component 2 from the site of the GRB explosion is 10-100 times smaller than that of component 3. We evaluated the mean metallicity of the z = 3.967 system obtaining values ≈10-2 of the solar metallicity or less. However, this should not be taken as representative of the circumburst medium, since the main contribution to the hydrogen column density comes from the outer regions of the galaxy while that of the other elements presumably comes from the ISM closer to the GRB site. Furthermore, difficulties in evaluating dust depletion correction can modify significantly these values. The mean [C/Fe] ratio agrees well with that expected by single star-formation event models. Interestingly the [C/Fe] of component 2 is smaller than that of component 3, in agreement with GRB dust destruction scenarios, if component 2 is closer than component 3 to the GRB site.

Original languageEnglish (US)
Pages (from-to)629-639
Number of pages11
JournalAstronomy and Astrophysics
Volume467
Issue number2
DOIs
StatePublished - May 1 2007

Fingerprint

afterglows
gamma ray bursts
ionization
spectroscopy
explosion
high resolution
dust
hydrogen
wavelength
fine structure
metallicity
gas
explosions
galaxies
analysis
destruction
star formation
depletion
optical absorption
actuators

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

D'Elia, V., Fiore, F., Meurs, E. J. A., Chincarini, G., Melandri, A., Nord, L., ... Vietri, M. (2007). UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: Probing the features of the GRB environment. Astronomy and Astrophysics, 467(2), 629-639. https://doi.org/10.1051/0004-6361:20066479
D'Elia, V. ; Fiore, F. ; Meurs, E. J.A. ; Chincarini, G. ; Melandri, A. ; Nord, L. ; Pellizza, L. ; Perna, R. ; Piranomonte, S. ; Sbordone, L. ; Stella, L. ; Tagliaferri, G. ; Vergani, S. D. ; Ward, P. ; Angelini, L. ; Antonelli, L. A. ; Burrows, D. N. ; Campana, S. ; Capalbi, M. ; Cimatti, A. ; Costa, E. ; Cusumano, G. ; Della Valle, M. ; Filliatre, P. ; Fontana, A. ; Frontera, F. ; Fugazza, D. ; Gehrels, N. ; Giannini, T. ; Giommi, P. ; Goldoni, P. ; Guetta, D. ; Israel, G. ; Lazzati, D. ; Malesani, D. ; Marconi, G. ; Mason, K. ; Mereghetti, S. ; Mirabel, F. ; Molinari, E. ; Moretti, A. ; Nousek, J. ; Perri, M. ; Piro, L. ; Stratta, G. ; Testa, V. ; Vietri, M. / UVES/VLT high resolution spectroscopy of GRB 050730 afterglow : Probing the features of the GRB environment. In: Astronomy and Astrophysics. 2007 ; Vol. 467, No. 2. pp. 629-639.
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abstract = "Aims. The aim of this paper is to study the Gamma Ray Burst (GRB) environment through the analysis of the optical absorption features due to the gas surrounding the GRB. Methods. To this purpose we analyze high resolution spectroscopic observations (R = 20 000-45 000, corresponding to 14 km s -1 at 4200 {\AA} and 6.6 km s-1 at 9000 {\AA}) of the optical afterglow of GRB050730, obtained with UVES@VLT ∼4 h after the GRB trigger. Results. The spectrum shows that the ISM of the GRB host galaxy at z = 3.967 is complex, with at least five components contributing to the main absorption system. We detect strong C II*, Si IIz.ast;, O Iz.ast; and Fe IIz.ast; fine structure absorption lines associated to the second and third component. Conclusions. For the first three components we derive information on the relative distance from the site of the GRB explosion. Component 1, which has the longest wavelength, highest positive velocity shift, does not present any fine structure nor low ionization lines; it only shows very high ionization features, such as CIV and O VI, suggesting that this component is very close to the GRB site. From the analysis of low and high ionization lines and fine structure lines, we find evidences that the distance of component 2 from the site of the GRB explosion is 10-100 times smaller than that of component 3. We evaluated the mean metallicity of the z = 3.967 system obtaining values ≈10-2 of the solar metallicity or less. However, this should not be taken as representative of the circumburst medium, since the main contribution to the hydrogen column density comes from the outer regions of the galaxy while that of the other elements presumably comes from the ISM closer to the GRB site. Furthermore, difficulties in evaluating dust depletion correction can modify significantly these values. The mean [C/Fe] ratio agrees well with that expected by single star-formation event models. Interestingly the [C/Fe] of component 2 is smaller than that of component 3, in agreement with GRB dust destruction scenarios, if component 2 is closer than component 3 to the GRB site.",
author = "V. D'Elia and F. Fiore and Meurs, {E. J.A.} and G. Chincarini and A. Melandri and L. Nord and L. Pellizza and R. Perna and S. Piranomonte and L. Sbordone and L. Stella and G. Tagliaferri and Vergani, {S. D.} and P. Ward and L. Angelini and Antonelli, {L. A.} and Burrows, {D. N.} and S. Campana and M. Capalbi and A. Cimatti and E. Costa and G. Cusumano and {Della Valle}, M. and P. Filliatre and A. Fontana and F. Frontera and D. Fugazza and N. Gehrels and T. Giannini and P. Giommi and P. Goldoni and D. Guetta and G. Israel and D. Lazzati and D. Malesani and G. Marconi and K. Mason and S. Mereghetti and F. Mirabel and E. Molinari and A. Moretti and J. Nousek and M. Perri and L. Piro and G. Stratta and V. Testa and M. Vietri",
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D'Elia, V, Fiore, F, Meurs, EJA, Chincarini, G, Melandri, A, Nord, L, Pellizza, L, Perna, R, Piranomonte, S, Sbordone, L, Stella, L, Tagliaferri, G, Vergani, SD, Ward, P, Angelini, L, Antonelli, LA, Burrows, DN, Campana, S, Capalbi, M, Cimatti, A, Costa, E, Cusumano, G, Della Valle, M, Filliatre, P, Fontana, A, Frontera, F, Fugazza, D, Gehrels, N, Giannini, T, Giommi, P, Goldoni, P, Guetta, D, Israel, G, Lazzati, D, Malesani, D, Marconi, G, Mason, K, Mereghetti, S, Mirabel, F, Molinari, E, Moretti, A, Nousek, J, Perri, M, Piro, L, Stratta, G, Testa, V & Vietri, M 2007, 'UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: Probing the features of the GRB environment', Astronomy and Astrophysics, vol. 467, no. 2, pp. 629-639. https://doi.org/10.1051/0004-6361:20066479

UVES/VLT high resolution spectroscopy of GRB 050730 afterglow : Probing the features of the GRB environment. / D'Elia, V.; Fiore, F.; Meurs, E. J.A.; Chincarini, G.; Melandri, A.; Nord, L.; Pellizza, L.; Perna, R.; Piranomonte, S.; Sbordone, L.; Stella, L.; Tagliaferri, G.; Vergani, S. D.; Ward, P.; Angelini, L.; Antonelli, L. A.; Burrows, D. N.; Campana, S.; Capalbi, M.; Cimatti, A.; Costa, E.; Cusumano, G.; Della Valle, M.; Filliatre, P.; Fontana, A.; Frontera, F.; Fugazza, D.; Gehrels, N.; Giannini, T.; Giommi, P.; Goldoni, P.; Guetta, D.; Israel, G.; Lazzati, D.; Malesani, D.; Marconi, G.; Mason, K.; Mereghetti, S.; Mirabel, F.; Molinari, E.; Moretti, A.; Nousek, J.; Perri, M.; Piro, L.; Stratta, G.; Testa, V.; Vietri, M.

In: Astronomy and Astrophysics, Vol. 467, No. 2, 01.05.2007, p. 629-639.

Research output: Contribution to journalArticle

TY - JOUR

T1 - UVES/VLT high resolution spectroscopy of GRB 050730 afterglow

T2 - Probing the features of the GRB environment

AU - D'Elia, V.

AU - Fiore, F.

AU - Meurs, E. J.A.

AU - Chincarini, G.

AU - Melandri, A.

AU - Nord, L.

AU - Pellizza, L.

AU - Perna, R.

AU - Piranomonte, S.

AU - Sbordone, L.

AU - Stella, L.

AU - Tagliaferri, G.

AU - Vergani, S. D.

AU - Ward, P.

AU - Angelini, L.

AU - Antonelli, L. A.

AU - Burrows, D. N.

AU - Campana, S.

AU - Capalbi, M.

AU - Cimatti, A.

AU - Costa, E.

AU - Cusumano, G.

AU - Della Valle, M.

AU - Filliatre, P.

AU - Fontana, A.

AU - Frontera, F.

AU - Fugazza, D.

AU - Gehrels, N.

AU - Giannini, T.

AU - Giommi, P.

AU - Goldoni, P.

AU - Guetta, D.

AU - Israel, G.

AU - Lazzati, D.

AU - Malesani, D.

AU - Marconi, G.

AU - Mason, K.

AU - Mereghetti, S.

AU - Mirabel, F.

AU - Molinari, E.

AU - Moretti, A.

AU - Nousek, J.

AU - Perri, M.

AU - Piro, L.

AU - Stratta, G.

AU - Testa, V.

AU - Vietri, M.

PY - 2007/5/1

Y1 - 2007/5/1

N2 - Aims. The aim of this paper is to study the Gamma Ray Burst (GRB) environment through the analysis of the optical absorption features due to the gas surrounding the GRB. Methods. To this purpose we analyze high resolution spectroscopic observations (R = 20 000-45 000, corresponding to 14 km s -1 at 4200 Å and 6.6 km s-1 at 9000 Å) of the optical afterglow of GRB050730, obtained with UVES@VLT ∼4 h after the GRB trigger. Results. The spectrum shows that the ISM of the GRB host galaxy at z = 3.967 is complex, with at least five components contributing to the main absorption system. We detect strong C II*, Si IIz.ast;, O Iz.ast; and Fe IIz.ast; fine structure absorption lines associated to the second and third component. Conclusions. For the first three components we derive information on the relative distance from the site of the GRB explosion. Component 1, which has the longest wavelength, highest positive velocity shift, does not present any fine structure nor low ionization lines; it only shows very high ionization features, such as CIV and O VI, suggesting that this component is very close to the GRB site. From the analysis of low and high ionization lines and fine structure lines, we find evidences that the distance of component 2 from the site of the GRB explosion is 10-100 times smaller than that of component 3. We evaluated the mean metallicity of the z = 3.967 system obtaining values ≈10-2 of the solar metallicity or less. However, this should not be taken as representative of the circumburst medium, since the main contribution to the hydrogen column density comes from the outer regions of the galaxy while that of the other elements presumably comes from the ISM closer to the GRB site. Furthermore, difficulties in evaluating dust depletion correction can modify significantly these values. The mean [C/Fe] ratio agrees well with that expected by single star-formation event models. Interestingly the [C/Fe] of component 2 is smaller than that of component 3, in agreement with GRB dust destruction scenarios, if component 2 is closer than component 3 to the GRB site.

AB - Aims. The aim of this paper is to study the Gamma Ray Burst (GRB) environment through the analysis of the optical absorption features due to the gas surrounding the GRB. Methods. To this purpose we analyze high resolution spectroscopic observations (R = 20 000-45 000, corresponding to 14 km s -1 at 4200 Å and 6.6 km s-1 at 9000 Å) of the optical afterglow of GRB050730, obtained with UVES@VLT ∼4 h after the GRB trigger. Results. The spectrum shows that the ISM of the GRB host galaxy at z = 3.967 is complex, with at least five components contributing to the main absorption system. We detect strong C II*, Si IIz.ast;, O Iz.ast; and Fe IIz.ast; fine structure absorption lines associated to the second and third component. Conclusions. For the first three components we derive information on the relative distance from the site of the GRB explosion. Component 1, which has the longest wavelength, highest positive velocity shift, does not present any fine structure nor low ionization lines; it only shows very high ionization features, such as CIV and O VI, suggesting that this component is very close to the GRB site. From the analysis of low and high ionization lines and fine structure lines, we find evidences that the distance of component 2 from the site of the GRB explosion is 10-100 times smaller than that of component 3. We evaluated the mean metallicity of the z = 3.967 system obtaining values ≈10-2 of the solar metallicity or less. However, this should not be taken as representative of the circumburst medium, since the main contribution to the hydrogen column density comes from the outer regions of the galaxy while that of the other elements presumably comes from the ISM closer to the GRB site. Furthermore, difficulties in evaluating dust depletion correction can modify significantly these values. The mean [C/Fe] ratio agrees well with that expected by single star-formation event models. Interestingly the [C/Fe] of component 2 is smaller than that of component 3, in agreement with GRB dust destruction scenarios, if component 2 is closer than component 3 to the GRB site.

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U2 - 10.1051/0004-6361:20066479

DO - 10.1051/0004-6361:20066479

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