The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B

Autores
D'Elia, V.; Fiore, F.; Perna, R.; Krongold, Y.; Covino, S.; Fugazza, D.; Lazzati, D.; Nicastro, F.; Antonelli, L. A.; Campana, S.; Chincarini, G.; D´Avanzo, P.; Della Valle, M.; Goldoni, P.; Guetta, D.; Guidorzi, C,; Meuers, E. J. A.; Mirabel Miquele, Igor Felix; Molinari, E.; Norci, L.; Piranomonte, S.; Stella, L.; Stratta, G.; Tagliaferri, G.; Ward, P.
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
GRB080319B reached fifth optical magnitude during the burst prompt emission. Thanks to the Very Large Telescope (VLT)/Ultraviolet and Visual Echelle Spectrograph (UVES) rapid response mode, we observed its afterglow just 8m:30s after the gamma-ray burst (GRB) onset when the magnitude was R ~ 12. This allowed us to obtain the best signal-to-noise (S/N), high-resolution spectrum of a GRB afterglow ever (S/N per resolution element ~50). The spectrum is rich of absorption features belonging to the main system at z = 0.937, divided in at least six components spanning a total velocity range of 100 km s-1. The VLT/UVES observations caught the absorbing gas in a highly excited state, producing the strongest Fe II fine structure lines ever observed in a GRB. A few hours later, the optical depth of these lines was reduced by a factor of 4-20, and the optical/UV flux by a factor of ~60. This proves that the excitation of the observed fine structure lines is due to "pumping" by the GRB UV photons.  comparison of the observed ratio between the number of photons absorbed by the excited state and those in the Fe II ground state suggests that the six absorbers are ~2-6 kpc from the GRB site, with component I ~ 3 times closer to the GRB site than components III-VI. Component I is characterized also by the lack of Mg I absorption, unlike all other components. This may be both due to a closer distance and a lower density, suggesting a structured interstellar matter in this galaxy complex.
Fil: D'Elia, V.. Osservatorio Astronomico di Roma; Italia
Fil: Fiore, F.. Osservatorio Astronomico di Roma; Italia
Fil: Perna, R.. State University Of Colorado Boulder; Estados Unidos
Fil: Krongold, Y.. Universidad Nacional Autónoma de México; México
Fil: Covino, S.. Osservatorio Astronomico di Brera; Italia
Fil: Fugazza, D.. Osservatorio Astronomico di Brera; Italia
Fil: Lazzati, D.. State University Of Colorado Boulder; Estados Unidos
Fil: Nicastro, F.. Osservatorio Astronomico di Roma; Italia
Fil: Antonelli, L. A.. Osservatorio Astronomico di Roma; Italia
Fil: Campana, S.. Osservatorio Astronomico di Brera; Italia
Fil: Chincarini, G.. Osservatorio Astronomico di Brera; Italia
Fil: D´Avanzo, P.. Osservatorio Astronomico di Brera; Italia
Fil: Della Valle, M.. Osservatorio Astronomico di Capodimonte; Italia
Fil: Goldoni, P.. Centre D; Francia
Fil: Guetta, D.. Osservatorio Astronomico di Roma; Italia
Fil: Guidorzi, C,. Osservatorio Astronomico di Brera; Italia
Fil: Meuers, E. J. A.. School of Cosmic Physics; Irlanda
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
Fil: Molinari, E.. Osservatorio Astronomico di Brera; Italia
Fil: Norci, L.. School of Physical Sciences; Irlanda
Fil: Piranomonte, S.. Osservatorio Astronomico di Roma; Italia
Fil: Stella, L.. Osservatorio Astronomico di Roma; Italia
Fil: Stratta, G.. ASI Science Data Center; Italia
Fil: Tagliaferri, G.. Osservatorio Astronomico di Brera; Italia
Fil: Ward, P.. Mullard Space Science Laboratory; Reino Unido
Materia
gamma rays: bursts
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:11336/20569
Acceder
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network_name_str CONICET Digital (CONICET)
spelling The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319BD'Elia, V.Fiore, F.Perna, R.Krongold, Y.Covino, S.Fugazza, D.Lazzati, D.Nicastro, F.Antonelli, L. A.Campana, S.Chincarini, G.D´Avanzo, P.Della Valle, M.Goldoni, P.Guetta, D.Guidorzi, C,Meuers, E. J. A.Mirabel Miquele, Igor FelixMolinari, E.Norci, L.Piranomonte, S.Stella, L.Stratta, G.Tagliaferri, G.Ward, P.gamma rays: burstshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1GRB080319B reached fifth optical magnitude during the burst prompt emission. Thanks to the Very Large Telescope (VLT)/Ultraviolet and Visual Echelle Spectrograph (UVES) rapid response mode, we observed its afterglow just 8m:30s after the gamma-ray burst (GRB) onset when the magnitude was R ~ 12. This allowed us to obtain the best signal-to-noise (S/N), high-resolution spectrum of a GRB afterglow ever (S/N per resolution element ~50). The spectrum is rich of absorption features belonging to the main system at z = 0.937, divided in at least six components spanning a total velocity range of 100 km s<sup>-1</sup>. The VLT/UVES observations caught the absorbing gas in a highly excited state, producing the strongest Fe II fine structure lines ever observed in a GRB. A few hours later, the optical depth of these lines was reduced by a factor of 4-20, and the optical/UV flux by a factor of ~60. This proves that the excitation of the observed fine structure lines is due to "pumping" by the GRB UV photons.  comparison of the observed ratio between the number of photons absorbed by the excited state and those in the Fe II ground state suggests that the six absorbers are ~2-6 kpc from the GRB site, with component I ~ 3 times closer to the GRB site than components III-VI. Component I is characterized also by the lack of Mg I absorption, unlike all other components. This may be both due to a closer distance and a lower density, suggesting a structured interstellar matter in this galaxy complex.Fil: D'Elia, V.. Osservatorio Astronomico di Roma; ItaliaFil: Fiore, F.. Osservatorio Astronomico di Roma; ItaliaFil: Perna, R.. State University Of Colorado Boulder; Estados UnidosFil: Krongold, Y.. Universidad Nacional Autónoma de México; MéxicoFil: Covino, S.. Osservatorio Astronomico di Brera; ItaliaFil: Fugazza, D.. Osservatorio Astronomico di Brera; ItaliaFil: Lazzati, D.. State University Of Colorado Boulder; Estados UnidosFil: Nicastro, F.. Osservatorio Astronomico di Roma; ItaliaFil: Antonelli, L. A.. Osservatorio Astronomico di Roma; ItaliaFil: Campana, S.. Osservatorio Astronomico di Brera; ItaliaFil: Chincarini, G.. Osservatorio Astronomico di Brera; ItaliaFil: D´Avanzo, P.. Osservatorio Astronomico di Brera; ItaliaFil: Della Valle, M.. Osservatorio Astronomico di Capodimonte; ItaliaFil: Goldoni, P.. Centre D; FranciaFil: Guetta, D.. Osservatorio Astronomico di Roma; ItaliaFil: Guidorzi, C,. Osservatorio Astronomico di Brera; ItaliaFil: Meuers, E. J. A.. School of Cosmic Physics; IrlandaFil: 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; ArgentinaFil: Molinari, E.. Osservatorio Astronomico di Brera; ItaliaFil: Norci, L.. School of Physical Sciences; IrlandaFil: Piranomonte, S.. Osservatorio Astronomico di Roma; ItaliaFil: Stella, L.. Osservatorio Astronomico di Roma; ItaliaFil: Stratta, G.. ASI Science Data Center; ItaliaFil: Tagliaferri, G.. Osservatorio Astronomico di Brera; ItaliaFil: Ward, P.. Mullard Space Science Laboratory; Reino UnidoIOP Publishing2009-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/20569D'Elia, V.; Fiore, F.; Perna, R.; Krongold, Y.; Covino, S.; et al.; The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B; IOP Publishing; Astrophysical Journal; 694; 1; 3-2009; 332-3380004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/694/1/332info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/694/1/332info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/pdf/0804.2141.pdfinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-10T13:23:19Zoai:ri.conicet.gov.ar:11336/20569instacron: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:34982025-09-10 13:23:19.633CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B
title The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B
spellingShingle The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B
D'Elia, V.
gamma rays: bursts
title_short The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B
title_full The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B
title_fullStr The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B
title_full_unstemmed The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B
title_sort The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B
dc.creator.none.fl_str_mv D'Elia, V.
Fiore, F.
Perna, R.
Krongold, Y.
Covino, S.
Fugazza, D.
Lazzati, D.
Nicastro, F.
Antonelli, L. A.
Campana, S.
Chincarini, G.
D´Avanzo, P.
Della Valle, M.
Goldoni, P.
Guetta, D.
Guidorzi, C,
Meuers, E. J. A.
Mirabel Miquele, Igor Felix
Molinari, E.
Norci, L.
Piranomonte, S.
Stella, L.
Stratta, G.
Tagliaferri, G.
Ward, P.
author D'Elia, V.
author_facet D'Elia, V.
Fiore, F.
Perna, R.
Krongold, Y.
Covino, S.
Fugazza, D.
Lazzati, D.
Nicastro, F.
Antonelli, L. A.
Campana, S.
Chincarini, G.
D´Avanzo, P.
Della Valle, M.
Goldoni, P.
Guetta, D.
Guidorzi, C,
Meuers, E. J. A.
Mirabel Miquele, Igor Felix
Molinari, E.
Norci, L.
Piranomonte, S.
Stella, L.
Stratta, G.
Tagliaferri, G.
Ward, P.
author_role author
author2 Fiore, F.
Perna, R.
Krongold, Y.
Covino, S.
Fugazza, D.
Lazzati, D.
Nicastro, F.
Antonelli, L. A.
Campana, S.
Chincarini, G.
D´Avanzo, P.
Della Valle, M.
Goldoni, P.
Guetta, D.
Guidorzi, C,
Meuers, E. J. A.
Mirabel Miquele, Igor Felix
Molinari, E.
Norci, L.
Piranomonte, S.
Stella, L.
Stratta, G.
Tagliaferri, G.
Ward, P.
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
dc.subject.none.fl_str_mv gamma rays: bursts
topic gamma rays: bursts
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv GRB080319B reached fifth optical magnitude during the burst prompt emission. Thanks to the Very Large Telescope (VLT)/Ultraviolet and Visual Echelle Spectrograph (UVES) rapid response mode, we observed its afterglow just 8m:30s after the gamma-ray burst (GRB) onset when the magnitude was R ~ 12. This allowed us to obtain the best signal-to-noise (S/N), high-resolution spectrum of a GRB afterglow ever (S/N per resolution element ~50). The spectrum is rich of absorption features belonging to the main system at z = 0.937, divided in at least six components spanning a total velocity range of 100 km s<sup>-1</sup>. The VLT/UVES observations caught the absorbing gas in a highly excited state, producing the strongest Fe II fine structure lines ever observed in a GRB. A few hours later, the optical depth of these lines was reduced by a factor of 4-20, and the optical/UV flux by a factor of ~60. This proves that the excitation of the observed fine structure lines is due to "pumping" by the GRB UV photons.  comparison of the observed ratio between the number of photons absorbed by the excited state and those in the Fe II ground state suggests that the six absorbers are ~2-6 kpc from the GRB site, with component I ~ 3 times closer to the GRB site than components III-VI. Component I is characterized also by the lack of Mg I absorption, unlike all other components. This may be both due to a closer distance and a lower density, suggesting a structured interstellar matter in this galaxy complex.
Fil: D'Elia, V.. Osservatorio Astronomico di Roma; Italia
Fil: Fiore, F.. Osservatorio Astronomico di Roma; Italia
Fil: Perna, R.. State University Of Colorado Boulder; Estados Unidos
Fil: Krongold, Y.. Universidad Nacional Autónoma de México; México
Fil: Covino, S.. Osservatorio Astronomico di Brera; Italia
Fil: Fugazza, D.. Osservatorio Astronomico di Brera; Italia
Fil: Lazzati, D.. State University Of Colorado Boulder; Estados Unidos
Fil: Nicastro, F.. Osservatorio Astronomico di Roma; Italia
Fil: Antonelli, L. A.. Osservatorio Astronomico di Roma; Italia
Fil: Campana, S.. Osservatorio Astronomico di Brera; Italia
Fil: Chincarini, G.. Osservatorio Astronomico di Brera; Italia
Fil: D´Avanzo, P.. Osservatorio Astronomico di Brera; Italia
Fil: Della Valle, M.. Osservatorio Astronomico di Capodimonte; Italia
Fil: Goldoni, P.. Centre D; Francia
Fil: Guetta, D.. Osservatorio Astronomico di Roma; Italia
Fil: Guidorzi, C,. Osservatorio Astronomico di Brera; Italia
Fil: Meuers, E. J. A.. School of Cosmic Physics; Irlanda
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
Fil: Molinari, E.. Osservatorio Astronomico di Brera; Italia
Fil: Norci, L.. School of Physical Sciences; Irlanda
Fil: Piranomonte, S.. Osservatorio Astronomico di Roma; Italia
Fil: Stella, L.. Osservatorio Astronomico di Roma; Italia
Fil: Stratta, G.. ASI Science Data Center; Italia
Fil: Tagliaferri, G.. Osservatorio Astronomico di Brera; Italia
Fil: Ward, P.. Mullard Space Science Laboratory; Reino Unido
description GRB080319B reached fifth optical magnitude during the burst prompt emission. Thanks to the Very Large Telescope (VLT)/Ultraviolet and Visual Echelle Spectrograph (UVES) rapid response mode, we observed its afterglow just 8m:30s after the gamma-ray burst (GRB) onset when the magnitude was R ~ 12. This allowed us to obtain the best signal-to-noise (S/N), high-resolution spectrum of a GRB afterglow ever (S/N per resolution element ~50). The spectrum is rich of absorption features belonging to the main system at z = 0.937, divided in at least six components spanning a total velocity range of 100 km s<sup>-1</sup>. The VLT/UVES observations caught the absorbing gas in a highly excited state, producing the strongest Fe II fine structure lines ever observed in a GRB. A few hours later, the optical depth of these lines was reduced by a factor of 4-20, and the optical/UV flux by a factor of ~60. This proves that the excitation of the observed fine structure lines is due to "pumping" by the GRB UV photons.  comparison of the observed ratio between the number of photons absorbed by the excited state and those in the Fe II ground state suggests that the six absorbers are ~2-6 kpc from the GRB site, with component I ~ 3 times closer to the GRB site than components III-VI. Component I is characterized also by the lack of Mg I absorption, unlike all other components. This may be both due to a closer distance and a lower density, suggesting a structured interstellar matter in this galaxy complex.
publishDate 2009
dc.date.none.fl_str_mv 2009-03
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/11336/20569
D'Elia, V.; Fiore, F.; Perna, R.; Krongold, Y.; Covino, S.; et al.; The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B; IOP Publishing; Astrophysical Journal; 694; 1; 3-2009; 332-338
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/20569
identifier_str_mv D'Elia, V.; Fiore, F.; Perna, R.; Krongold, Y.; Covino, S.; et al.; The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B; IOP Publishing; Astrophysical Journal; 694; 1; 3-2009; 332-338
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/694/1/332
info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/694/1/332
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/pdf/0804.2141.pdf
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 IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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
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score 12.48226

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