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

Autores
D'Elia, V.; Fiore, F.; Meurs, E. J. A.; Chincarini, G.; Melandri, A.; Norci, L.; Pellizza González, Leonardo Javier; 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.; Mirabel Miquele, Igor Felix
Año de publicación
2007
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
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 II*, O I* and Fe II* 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 C IV 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.
Fil: D'Elia, V.. Osservatorio Astronomico di Roma; Italia
Fil: Fiore, F.. Osservatorio Astronomico di Roma; Italia
Fil: Meurs, E. J. A.. Dunsink Observatory; Irlanda
Fil: Chincarini, G.. Osservatorio Astronomico di Brera,; Italia
Fil: Melandri, A.. Liverpool John Moores University; Reino Unido
Fil: Norci, L.. Dublin City University; Irlanda
Fil: Pellizza González, Leonardo Javier. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Perna, R.. State University Of Colorado Boulder; Estados Unidos
Fil: Piranomonte, S.. Osservatorio Astronomico di Roma; Italia
Fil: Sbordone, L.. Osservatorio Astronomico di Roma; Italia
Fil: Stella, L.. Osservatorio Astronomico di Roma; Italia
Fil: Tagliaferri, G.. Osservatorio Astronomico di Brera; Italia
Fil: Vergani, S. D.. Dublin City University; Irlanda
Fil: Ward, P.. Dunsink Observatory; Irlanda
Fil: Angelini, L.. National Aeronautics And Space Administration. Goddart Institute For Space Studies; Estados Unidos
Fil: Antonelli, L. A.. Osservatorio Astronomico di Roma; Italia
Fil: Burrows, D. N.. State University Of Pennsylvania; Estados Unidos
Fil: Campana, S.. Osservatorio Astronomico di Brera; Italia
Fil: Capalbi, M.. Science Data Center; Italia
Fil: Cimatti, A.. Osservatorio Astronomico di Arcetri,; Italia
Fil: Costa, E.. INAF; Italia
Fil: Cusumano, G.. Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo; Italia
Fil: Della Valle, M.. Osservatorio Astronomico di Arcetri; Italia
Fil: Filliatre, P.. Centre D; Francia
Fil: Fontana, A.. Osservatorio Astronomico di Roma; Italia
Fil: Frontera, F.. Universita; Italia
Fil: Fugazza, D.. Osservatorio Astronomico di Brera,; Italia
Fil: Gehrels, N.. National Aeronautics And Space Administration. Goddart Institute For Space Studies; Estados Unidos
Fil: Giannini, T.. Osservatorio Astronomico di Roma; Italia
Fil: Mirabel Miquele, Igor Felix. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Materia
GAMMA RAYS: BURSTS
COSMOLOGY: OBSERVATIONS
GALAXY: ABUNDANCES
GALAXIES: ISM
LINE: IDENTIFICATION
LINE: PROFILES
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/21214

id CONICETDig_edb7f52de3d3f0c2d8b335724b5daf86
oai_identifier_str oai:ri.conicet.gov.ar:11336/21214
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environmentD'Elia, V.Fiore, F.Meurs, E. J. A.Chincarini, G.Melandri, A.Norci, L.Pellizza González, Leonardo JavierPerna, 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.Mirabel Miquele, Igor FelixGAMMA RAYS: BURSTSCOSMOLOGY: OBSERVATIONSGALAXY: ABUNDANCESGALAXIES: ISMLINE: IDENTIFICATIONLINE: PROFILEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. 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 II*, O I* and Fe II* 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 C IV 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.Fil: D'Elia, V.. Osservatorio Astronomico di Roma; ItaliaFil: Fiore, F.. Osservatorio Astronomico di Roma; ItaliaFil: Meurs, E. J. A.. Dunsink Observatory; IrlandaFil: Chincarini, G.. Osservatorio Astronomico di Brera,; ItaliaFil: Melandri, A.. Liverpool John Moores University; Reino UnidoFil: Norci, L.. Dublin City University; IrlandaFil: Pellizza González, Leonardo Javier. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Perna, R.. State University Of Colorado Boulder; Estados UnidosFil: Piranomonte, S.. Osservatorio Astronomico di Roma; ItaliaFil: Sbordone, L.. Osservatorio Astronomico di Roma; ItaliaFil: Stella, L.. Osservatorio Astronomico di Roma; ItaliaFil: Tagliaferri, G.. Osservatorio Astronomico di Brera; ItaliaFil: Vergani, S. D.. Dublin City University; IrlandaFil: Ward, P.. Dunsink Observatory; IrlandaFil: Angelini, L.. National Aeronautics And Space Administration. Goddart Institute For Space Studies; Estados UnidosFil: Antonelli, L. A.. Osservatorio Astronomico di Roma; ItaliaFil: Burrows, D. N.. State University Of Pennsylvania; Estados UnidosFil: Campana, S.. Osservatorio Astronomico di Brera; ItaliaFil: Capalbi, M.. Science Data Center; ItaliaFil: Cimatti, A.. Osservatorio Astronomico di Arcetri,; ItaliaFil: Costa, E.. INAF; ItaliaFil: Cusumano, G.. Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo; ItaliaFil: Della Valle, M.. Osservatorio Astronomico di Arcetri; ItaliaFil: Filliatre, P.. Centre D; FranciaFil: Fontana, A.. Osservatorio Astronomico di Roma; ItaliaFil: Frontera, F.. Universita; ItaliaFil: Fugazza, D.. Osservatorio Astronomico di Brera,; ItaliaFil: Gehrels, N.. National Aeronautics And Space Administration. Goddart Institute For Space Studies; Estados UnidosFil: Giannini, T.. Osservatorio Astronomico di Roma; ItaliaFil: Mirabel Miquele, Igor Felix. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaEDP Sciences2007-05info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/21214D'Elia, V.; Fiore, F.; Meurs, E. J. A.; Chincarini, G.; Melandri, A.; et al.; UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment; EDP Sciences; Astronomy and Astrophysics; 467; 2; 5-2007; 629-6390004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066479info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2007/20/aa6479-06/aa6479-06.htmlinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/astro-ph/0609825info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:39:33Zoai:ri.conicet.gov.ar:11336/21214instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 11:39:33.353CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment
title UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment
spellingShingle UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment
D'Elia, V.
GAMMA RAYS: BURSTS
COSMOLOGY: OBSERVATIONS
GALAXY: ABUNDANCES
GALAXIES: ISM
LINE: IDENTIFICATION
LINE: PROFILES
title_short UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment
title_full UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment
title_fullStr UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment
title_full_unstemmed UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment
title_sort UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment
dc.creator.none.fl_str_mv D'Elia, V.
Fiore, F.
Meurs, E. J. A.
Chincarini, G.
Melandri, A.
Norci, L.
Pellizza González, Leonardo Javier
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.
Mirabel Miquele, Igor Felix
author D'Elia, V.
author_facet D'Elia, V.
Fiore, F.
Meurs, E. J. A.
Chincarini, G.
Melandri, A.
Norci, L.
Pellizza González, Leonardo Javier
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.
Mirabel Miquele, Igor Felix
author_role author
author2 Fiore, F.
Meurs, E. J. A.
Chincarini, G.
Melandri, A.
Norci, L.
Pellizza González, Leonardo Javier
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.
Mirabel Miquele, Igor Felix
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv GAMMA RAYS: BURSTS
COSMOLOGY: OBSERVATIONS
GALAXY: ABUNDANCES
GALAXIES: ISM
LINE: IDENTIFICATION
LINE: PROFILES
topic GAMMA RAYS: BURSTS
COSMOLOGY: OBSERVATIONS
GALAXY: ABUNDANCES
GALAXIES: ISM
LINE: IDENTIFICATION
LINE: PROFILES
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv 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 II*, O I* and Fe II* 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 C IV 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.
Fil: D'Elia, V.. Osservatorio Astronomico di Roma; Italia
Fil: Fiore, F.. Osservatorio Astronomico di Roma; Italia
Fil: Meurs, E. J. A.. Dunsink Observatory; Irlanda
Fil: Chincarini, G.. Osservatorio Astronomico di Brera,; Italia
Fil: Melandri, A.. Liverpool John Moores University; Reino Unido
Fil: Norci, L.. Dublin City University; Irlanda
Fil: Pellizza González, Leonardo Javier. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Perna, R.. State University Of Colorado Boulder; Estados Unidos
Fil: Piranomonte, S.. Osservatorio Astronomico di Roma; Italia
Fil: Sbordone, L.. Osservatorio Astronomico di Roma; Italia
Fil: Stella, L.. Osservatorio Astronomico di Roma; Italia
Fil: Tagliaferri, G.. Osservatorio Astronomico di Brera; Italia
Fil: Vergani, S. D.. Dublin City University; Irlanda
Fil: Ward, P.. Dunsink Observatory; Irlanda
Fil: Angelini, L.. National Aeronautics And Space Administration. Goddart Institute For Space Studies; Estados Unidos
Fil: Antonelli, L. A.. Osservatorio Astronomico di Roma; Italia
Fil: Burrows, D. N.. State University Of Pennsylvania; Estados Unidos
Fil: Campana, S.. Osservatorio Astronomico di Brera; Italia
Fil: Capalbi, M.. Science Data Center; Italia
Fil: Cimatti, A.. Osservatorio Astronomico di Arcetri,; Italia
Fil: Costa, E.. INAF; Italia
Fil: Cusumano, G.. Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo; Italia
Fil: Della Valle, M.. Osservatorio Astronomico di Arcetri; Italia
Fil: Filliatre, P.. Centre D; Francia
Fil: Fontana, A.. Osservatorio Astronomico di Roma; Italia
Fil: Frontera, F.. Universita; Italia
Fil: Fugazza, D.. Osservatorio Astronomico di Brera,; Italia
Fil: Gehrels, N.. National Aeronautics And Space Administration. Goddart Institute For Space Studies; Estados Unidos
Fil: Giannini, T.. Osservatorio Astronomico di Roma; Italia
Fil: Mirabel Miquele, Igor Felix. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
description 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 II*, O I* and Fe II* 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 C IV 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.
publishDate 2007
dc.date.none.fl_str_mv 2007-05
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/21214
D'Elia, V.; Fiore, F.; Meurs, E. J. A.; Chincarini, G.; Melandri, A.; et al.; UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment; EDP Sciences; Astronomy and Astrophysics; 467; 2; 5-2007; 629-639
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/21214
identifier_str_mv D'Elia, V.; Fiore, F.; Meurs, E. J. A.; Chincarini, G.; Melandri, A.; et al.; UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment; EDP Sciences; Astronomy and Astrophysics; 467; 2; 5-2007; 629-639
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066479
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2007/20/aa6479-06/aa6479-06.html
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/astro-ph/0609825
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
_version_ 1846782060589481984
score 12.982451