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
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/21214
Ver los metadatos del registro completo
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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 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
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publishedVersion |
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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 |
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eng |
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eng |
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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 |
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info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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openAccess |
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EDP Sciences |
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EDP Sciences |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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