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dc.date.accessioned | 2019-10-24T16:43:34Z | |
dc.date.available | 2019-10-24T16:43:34Z | |
dc.date.issued | 2011 | |
dc.identifier.uri | http://sedici.unlp.edu.ar/handle/10915/84005 | |
dc.description.abstract | 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. | en |
dc.format.extent | 272-288 | es |
dc.language | en | es |
dc.subject | Galaxies: abundances | es |
dc.subject | Galaxies: fundamental parameters | es |
dc.subject | Galaxies: starburst | es |
dc.subject | Galaxies: stellar content | es |
dc.subject | H II regions | es |
dc.subject | ISM: abundances | es |
dc.title | Abundance determination of multiple star-forming regions in the H II galaxy SDSS J165712.75+321141.4 | en |
dc.type | Articulo | es |
sedici.identifier.other | doi:10.1111/j.1365-2966.2011.18389.x | es |
sedici.identifier.other | eid:2-s2.0-79957920802 | es |
sedici.identifier.issn | 0035-8711 | es |
sedici.creator.person | Hägele, Guillermo Federico | es |
sedici.creator.person | García Benito, Rubén | es |
sedici.creator.person | Pérez Montero, Enrique | es |
sedici.creator.person | Díaz, Ángeles I. | es |
sedici.creator.person | Cardaci, Mónica Viviana | es |
sedici.creator.person | Firpo, Verónica | es |
sedici.creator.person | Terlevich, Elena | es |
sedici.creator.person | Terlevich, Roberto | es |
sedici.subject.materias | Ciencias Astronómicas | es |
sedici.description.fulltext | true | es |
mods.originInfo.place | Facultad de Ciencias Astronómicas y Geofísicas | es |
sedici.subtype | Articulo | es |
sedici.rights.license | Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) | |
sedici.rights.uri | http://creativecommons.org/licenses/by-nc-sa/4.0/ | |
sedici.description.peerReview | peer-review | es |
sedici.relation.journalTitle | Monthly Notices of the Royal Astronomical Society | es |
sedici.relation.journalVolumeAndIssue | vol. 414, no. 1 | es |
sedici.rights.sherpa | * Color: verde* Pre-print del autor: si* Post-print del autor: si* Versión de editor/PDF:si* Condiciones:>>El pre-print sólo puede depositarse antes de la aceptación>>Pre-print on author's personal website, employer website, free public server or pre-prints in subject area>>El pre-print debe acompañarse de una declaración establecida (ver enlace)>>Pre-print set statement must be amended upon publication (see policy)>>La versión de editor/PDF puede utilizarse>>Author's Post-print on Institutional repositories or Central repositories>>Publisher's version/PDF on Institutional repositories or Central repositories, with all rights reserved (see policy)>>La fuente editorial debe reconocerse>>Debe ir enlazado a la versión de editor>>La copia archivada debe acompañarse de la frase establecida (ver Política)* Link a Sherpa: http://sherpa.ac.uk/romeo/issn/0035-8711/es/ |