Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4

Autores
Hägele, Guillermo Federico; García Benito, Rubén; Pérez Montero, Enrique; Díaz, Ángeles I.; Cardaci, Mónica Viviana; Firpo, Verónica; Terlevich, Elena; Terlevich, Roberto
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We analyse high signal-to-noise ratio spectrophotometric observations acquired simultaneously with TWIN, a double-arm spectrograph, from 3400 to 10400 Å of three star-forming regions in the H II galaxy SDSS J165712.75+321141.4. We have measured four line temperatures -Te([O III]), Te([S III]), Te([O II]) and Te([S II]) - with high-precision, rms errors of the order of 2, 5, 6 and 6 per cent, respectively, for the brightest region, and slightly worse for the other two. The temperature measurements allowed the direct derivation of ionic abundances of oxygen, sulphur, nitrogen, neon and argon. We have computed cloudy tailor-made models which reproduce the O2+-measured thermal and ionic structures within the errors in the three knots, with deviations of only 0.1 dex in the case of O+ and S2+ ionic abundances. In the case of the electron temperature and the ionic abundances of S+/H+, we find major discrepancies which could be the consequence of the presence of colder diffuse gas. The star formation history derived using starlight shows a similar age distribution of the ionizing population among the three star-forming regions. This fact suggests a similar evolutionary history which is probably related to the process of interaction with a companion galaxy that triggered the star formation in the different regions almost at the same time. The hardness of the radiation field mapped through the use of the softness parameter η is the same within the observational errors for all three regions, implying that the equivalent effective temperatures of the radiation fields are very similar for all the studied regions of the galaxy, in spite of some small differences in the ionization state of different elements. Regarding the kinematics of the galaxy, the gas rotation curve shows a deviation from the circular motion probably due either to an interaction process or to an expanding bubble or shell of the ionized gas approaching us. A dynamical mass of 2.5×1010M⊙ is derived from the rotation curve.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Galaxies: abundances
Galaxies: fundamental parameters
Galaxies: starburst
Galaxies: stellar content
H II regions
ISM: abundances
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/84005

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/84005
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4Hägele, Guillermo FedericoGarcía Benito, RubénPérez Montero, EnriqueDíaz, Ángeles I.Cardaci, Mónica VivianaFirpo, VerónicaTerlevich, ElenaTerlevich, RobertoCiencias AstronómicasGalaxies: abundancesGalaxies: fundamental parametersGalaxies: starburstGalaxies: stellar contentH II regionsISM: abundancesWe analyse high signal-to-noise ratio spectrophotometric observations acquired simultaneously with TWIN, a double-arm spectrograph, from 3400 to 10400 Å of three star-forming regions in the H II galaxy SDSS J165712.75+321141.4. We have measured four line temperatures -Te([O III]), Te([S III]), Te([O II]) and Te([S II]) - with high-precision, rms errors of the order of 2, 5, 6 and 6 per cent, respectively, for the brightest region, and slightly worse for the other two. The temperature measurements allowed the direct derivation of ionic abundances of oxygen, sulphur, nitrogen, neon and argon. We have computed cloudy tailor-made models which reproduce the O<SUP>2+</SUP>-measured thermal and ionic structures within the errors in the three knots, with deviations of only 0.1 dex in the case of O<SUP>+</SUP> and S<SUP>2+</SUP> ionic abundances. In the case of the electron temperature and the ionic abundances of S<SUP>+</SUP>/H<SUP>+</SUP>, we find major discrepancies which could be the consequence of the presence of colder diffuse gas. The star formation history derived using starlight shows a similar age distribution of the ionizing population among the three star-forming regions. This fact suggests a similar evolutionary history which is probably related to the process of interaction with a companion galaxy that triggered the star formation in the different regions almost at the same time. The hardness of the radiation field mapped through the use of the softness parameter η is the same within the observational errors for all three regions, implying that the equivalent effective temperatures of the radiation fields are very similar for all the studied regions of the galaxy, in spite of some small differences in the ionization state of different elements. Regarding the kinematics of the galaxy, the gas rotation curve shows a deviation from the circular motion probably due either to an interaction process or to an expanding bubble or shell of the ionized gas approaching us. A dynamical mass of 2.5×10<SUP>10</SUP>M⊙ is derived from the rotation curve.Facultad de Ciencias Astronómicas y Geofísicas2011info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf272-288http://sedici.unlp.edu.ar/handle/10915/84005enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.18389.xinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:10Zoai:sedici.unlp.edu.ar:10915/84005Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:10.266SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4
title Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4
spellingShingle Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4
Hägele, Guillermo Federico
Ciencias Astronómicas
Galaxies: abundances
Galaxies: fundamental parameters
Galaxies: starburst
Galaxies: stellar content
H II regions
ISM: abundances
title_short Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4
title_full Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4
title_fullStr Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4
title_full_unstemmed Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4
title_sort Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4
dc.creator.none.fl_str_mv Hägele, Guillermo Federico
García Benito, Rubén
Pérez Montero, Enrique
Díaz, Ángeles I.
Cardaci, Mónica Viviana
Firpo, Verónica
Terlevich, Elena
Terlevich, Roberto
author Hägele, Guillermo Federico
author_facet Hägele, Guillermo Federico
García Benito, Rubén
Pérez Montero, Enrique
Díaz, Ángeles I.
Cardaci, Mónica Viviana
Firpo, Verónica
Terlevich, Elena
Terlevich, Roberto
author_role author
author2 García Benito, Rubén
Pérez Montero, Enrique
Díaz, Ángeles I.
Cardaci, Mónica Viviana
Firpo, Verónica
Terlevich, Elena
Terlevich, Roberto
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Galaxies: abundances
Galaxies: fundamental parameters
Galaxies: starburst
Galaxies: stellar content
H II regions
ISM: abundances
topic Ciencias Astronómicas
Galaxies: abundances
Galaxies: fundamental parameters
Galaxies: starburst
Galaxies: stellar content
H II regions
ISM: abundances
dc.description.none.fl_txt_mv We analyse high signal-to-noise ratio spectrophotometric observations acquired simultaneously with TWIN, a double-arm spectrograph, from 3400 to 10400 Å of three star-forming regions in the H II galaxy SDSS J165712.75+321141.4. We have measured four line temperatures -Te([O III]), Te([S III]), Te([O II]) and Te([S II]) - with high-precision, rms errors of the order of 2, 5, 6 and 6 per cent, respectively, for the brightest region, and slightly worse for the other two. The temperature measurements allowed the direct derivation of ionic abundances of oxygen, sulphur, nitrogen, neon and argon. We have computed cloudy tailor-made models which reproduce the O<SUP>2+</SUP>-measured thermal and ionic structures within the errors in the three knots, with deviations of only 0.1 dex in the case of O<SUP>+</SUP> and S<SUP>2+</SUP> ionic abundances. In the case of the electron temperature and the ionic abundances of S<SUP>+</SUP>/H<SUP>+</SUP>, we find major discrepancies which could be the consequence of the presence of colder diffuse gas. The star formation history derived using starlight shows a similar age distribution of the ionizing population among the three star-forming regions. This fact suggests a similar evolutionary history which is probably related to the process of interaction with a companion galaxy that triggered the star formation in the different regions almost at the same time. The hardness of the radiation field mapped through the use of the softness parameter η is the same within the observational errors for all three regions, implying that the equivalent effective temperatures of the radiation fields are very similar for all the studied regions of the galaxy, in spite of some small differences in the ionization state of different elements. Regarding the kinematics of the galaxy, the gas rotation curve shows a deviation from the circular motion probably due either to an interaction process or to an expanding bubble or shell of the ionized gas approaching us. A dynamical mass of 2.5×10<SUP>10</SUP>M⊙ is derived from the rotation curve.
Facultad de Ciencias Astronómicas y Geofísicas
description We analyse high signal-to-noise ratio spectrophotometric observations acquired simultaneously with TWIN, a double-arm spectrograph, from 3400 to 10400 Å of three star-forming regions in the H II galaxy SDSS J165712.75+321141.4. We have measured four line temperatures -Te([O III]), Te([S III]), Te([O II]) and Te([S II]) - with high-precision, rms errors of the order of 2, 5, 6 and 6 per cent, respectively, for the brightest region, and slightly worse for the other two. The temperature measurements allowed the direct derivation of ionic abundances of oxygen, sulphur, nitrogen, neon and argon. We have computed cloudy tailor-made models which reproduce the O<SUP>2+</SUP>-measured thermal and ionic structures within the errors in the three knots, with deviations of only 0.1 dex in the case of O<SUP>+</SUP> and S<SUP>2+</SUP> ionic abundances. In the case of the electron temperature and the ionic abundances of S<SUP>+</SUP>/H<SUP>+</SUP>, we find major discrepancies which could be the consequence of the presence of colder diffuse gas. The star formation history derived using starlight shows a similar age distribution of the ionizing population among the three star-forming regions. This fact suggests a similar evolutionary history which is probably related to the process of interaction with a companion galaxy that triggered the star formation in the different regions almost at the same time. The hardness of the radiation field mapped through the use of the softness parameter η is the same within the observational errors for all three regions, implying that the equivalent effective temperatures of the radiation fields are very similar for all the studied regions of the galaxy, in spite of some small differences in the ionization state of different elements. Regarding the kinematics of the galaxy, the gas rotation curve shows a deviation from the circular motion probably due either to an interaction process or to an expanding bubble or shell of the ionized gas approaching us. A dynamical mass of 2.5×10<SUP>10</SUP>M⊙ is derived from the rotation curve.
publishDate 2011
dc.date.none.fl_str_mv 2011
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
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info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/84005
url http://sedici.unlp.edu.ar/handle/10915/84005
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0035-8711
info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.18389.x
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
272-288
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instname:Universidad Nacional de La Plata
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