Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4
- Autores
- Hägele, Guillermo Federico; García Benito, Rubén; Pérez Montero, Enrique; Díaz, Ángeles I.; Cardaci, Monica 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 10 400Å of three star-forming regions in the HII 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 2.5×10^10Msun is derived from the rotation curve.
Fil: Hägele, Guillermo Federico. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: García Benito, Rubén. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Peking University/kavli Inst. Of Astronomy And Astroph.; China
Fil: Pérez Montero, Enrique. Inst. de Astrofísica de Andalucía; España
Fil: Díaz, Ángeles I.. Universidad Autónoma de Madrid. Facultad de Ciencias; España
Fil: Cardaci, Monica Viviana. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Firpo, Verónica. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Terlevich, Elena. Instituto Nacional de Astrofísica, Óptica y Electrónica; México
Fil: Terlevich, Roberto. Instituto Nacional de Astrofísica, Óptica y Electrónica; México - Materia
-
ISM: abundances
HII regions
galaxies: abundances
galaxies: fundamental parameters
galaxies: starburst
galaxies: stellar content - 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:11336/138714
Ver los metadatos del registro completo
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Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4Hägele, Guillermo FedericoGarcía Benito, RubénPérez Montero, EnriqueDíaz, Ángeles I.Cardaci, Monica VivianaFirpo, VerónicaTerlevich, ElenaTerlevich, RobertoISM: abundancesHII regionsgalaxies: abundancesgalaxies: fundamental parametersgalaxies: starburstgalaxies: stellar contenthttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We analyse high signal-to-noise ratio spectrophotometric observations acquired simultaneously with TWIN, a double-arm spectrograph, from 3400 to 10 400Å of three star-forming regions in the HII 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 2.5×10^10Msun is derived from the rotation curve.Fil: Hägele, Guillermo Federico. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: García Benito, Rubén. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Peking University/kavli Inst. Of Astronomy And Astroph.; ChinaFil: Pérez Montero, Enrique. Inst. de Astrofísica de Andalucía; EspañaFil: Díaz, Ángeles I.. Universidad Autónoma de Madrid. Facultad de Ciencias; EspañaFil: Cardaci, Monica Viviana. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Firpo, Verónica. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Terlevich, Elena. Instituto Nacional de Astrofísica, Óptica y Electrónica; MéxicoFil: Terlevich, Roberto. Instituto Nacional de Astrofísica, Óptica y Electrónica; MéxicoWiley Blackwell Publishing, Inc2011-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/138714Hägele, Guillermo Federico; García Benito, Rubén; Pérez Montero, Enrique; Díaz, Ángeles I. ; Cardaci, Monica Viviana; et al.; Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 414; 1; 1-2011; 1-170035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.18389.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/414/1/272/1089522info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:39:23Zoai:ri.conicet.gov.ar:11336/138714instacron: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:34982025-09-29 10:39:23.679CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4 |
| title |
Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4 |
| spellingShingle |
Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4 Hägele, Guillermo Federico ISM: abundances HII regions galaxies: abundances galaxies: fundamental parameters galaxies: starburst galaxies: stellar content |
| title_short |
Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4 |
| title_full |
Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4 |
| title_fullStr |
Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4 |
| title_full_unstemmed |
Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4 |
| title_sort |
Abundance determination of multiple star-forming regions in the HII 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, Monica 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, Monica Viviana Firpo, Verónica Terlevich, Elena Terlevich, Roberto |
| author_role |
author |
| author2 |
García Benito, Rubén Pérez Montero, Enrique Díaz, Ángeles I. Cardaci, Monica Viviana Firpo, Verónica Terlevich, Elena Terlevich, Roberto |
| author2_role |
author author author author author author author |
| dc.subject.none.fl_str_mv |
ISM: abundances HII regions galaxies: abundances galaxies: fundamental parameters galaxies: starburst galaxies: stellar content |
| topic |
ISM: abundances HII regions galaxies: abundances galaxies: fundamental parameters galaxies: starburst galaxies: stellar content |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| 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 10 400Å of three star-forming regions in the HII 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 2.5×10^10Msun is derived from the rotation curve. Fil: Hägele, Guillermo Federico. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: García Benito, Rubén. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Peking University/kavli Inst. Of Astronomy And Astroph.; China Fil: Pérez Montero, Enrique. Inst. de Astrofísica de Andalucía; España Fil: Díaz, Ángeles I.. Universidad Autónoma de Madrid. Facultad de Ciencias; España Fil: Cardaci, Monica Viviana. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Universidad Autónoma de Madrid. Facultad de Ciencias; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Firpo, Verónica. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Terlevich, Elena. Instituto Nacional de Astrofísica, Óptica y Electrónica; México Fil: Terlevich, Roberto. Instituto Nacional de Astrofísica, Óptica y Electrónica; México |
| description |
We analyse high signal-to-noise ratio spectrophotometric observations acquired simultaneously with TWIN, a double-arm spectrograph, from 3400 to 10 400Å of three star-forming regions in the HII 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 2.5×10^10Msun is derived from the rotation curve. |
| publishDate |
2011 |
| dc.date.none.fl_str_mv |
2011-01 |
| 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 |
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article |
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publishedVersion |
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http://hdl.handle.net/11336/138714 Hägele, Guillermo Federico; García Benito, Rubén; Pérez Montero, Enrique; Díaz, Ángeles I. ; Cardaci, Monica Viviana; et al.; Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 414; 1; 1-2011; 1-17 0035-8711 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/138714 |
| identifier_str_mv |
Hägele, Guillermo Federico; García Benito, Rubén; Pérez Montero, Enrique; Díaz, Ángeles I. ; Cardaci, Monica Viviana; et al.; Abundance determination of multiple star-forming regions in the HII galaxy SDSS J165712.75+321141.4; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 414; 1; 1-2011; 1-17 0035-8711 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
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info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.18389.x info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/414/1/272/1089522 |
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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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https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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application/pdf application/pdf application/pdf application/pdf |
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Wiley Blackwell Publishing, Inc |
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Wiley Blackwell Publishing, Inc |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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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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