Por favor, use este identificador para citar o enlazar este ítem:
http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/1817| Abundance determination of multiple star-forming regions in the Hɪɪ galaxy SDSS J165712.75+321141.4 | |
| Elena Kirilovsky Terlevich | |
| Acceso Abierto | |
| Atribución-NoComercial-SinDerivadas | |
| ISM: abundances HII regions Galaxies: abundances Galaxies: fundamental parameters Galaxies: starburst Galaxies: stellar content | |
| 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 Hɪɪ galaxy SDSS J165712.75+321141.4. We have measured four line temperaturas – Tₑ([O ɪɪɪ]), Tₑ([S ɪɪɪ]), Tₑ([O ɪɪ]) and Tₑ([S ɪɪ]) – 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 O2²⁺ -measured termal 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 2.5×10¹°Mꙩ is derived from the rotation curve. | |
| Monthly Notices of the Royal Astronomical Society | |
| 2011 | |
| Artículo | |
| Inglés | |
| Estudiantes Investigadores Público en general | |
| Hagele, Guillermo F., et al., (2011), Abundance determination of multiple star-forming regions in the Hɪɪ galaxy SDSS J165712.75+321141.4, Monthly Notices of the Royal Astronomical Society, Vol. 414: 272–288 | |
| ASTRONOMÍA Y ASTROFÍSICA | |
| Versión aceptada | |
| acceptedVersion - Versión aceptada | |
| Aparece en las colecciones: | Artículos de Astrofísica |
Cargar archivos:
| Fichero | Tamaño | Formato | |
|---|---|---|---|
| 22 Hagele_MNRAS414-272.pdf | 9.78 MB | Adobe PDF | Visualizar/Abrir |