Detalles del recurso
Pertenece a:
UPCommons - E-prints UPC Universitat Politècnica de Catalunya
Descripción: The efficient use of Type Ia supernovae (SNIa) for cosmological studies requires knowledge of
any parameter that can affect their luminosity in either systematic or statistical ways. Observational
samples of SNIa commonly use the metallicity of the host galaxy, Zhost, as an estimator
of the supernova progenitor metallicity, ZIa, that is one of the primary factors affecting SNIa
magnitude. Here, we present a theoretical study of the relationship between ZIa and Zhost. We
follow the chemical evolution of homogeneous galaxy models together with the evolution of
the supernova rates in order to evaluate the metallicity distribution function, MDF( Z), i.e.
the probability that the logarithm of the metallicity of a SNIa exploding now differs in less
than Z from that of its host. We analyse several model galaxies aimed to represent from
active to passive galaxies, including dwarf galaxies prone to experience supernova driven outflows.
We analyse as well the sensitivity of the MDF to the most uncertain ingredients of our
approach: IMF, star-formation law, stellar lifetime, stellar yields, and SNIa delay-time distribution
(DTD). Our results show a remarkable degree of agreement between the mean ¯ZIa in
a galaxy and its Zhost when they both are measured as the CNO abundance, especially if the
DTD peaks at small time delays, while the average Fe abundance of host and SNIa may differ
up to 0.4-0.6 dex in passive galaxies. The dispersion of ZIa in active galaxy models is quite
small, meaning that Zhost is a quite good estimator of the supernovametallicity. Passive galaxies
present a larger dispersion, which is more pronounced in low mass galaxies.We present a
procedure to generate random SNIa metallicities, given the host metallicity. We also discuss
the use of differentmetallicity indicators: Fe vs. O, and gas-phasemetallicity vs. stellar metallicity.
Finally, the results of the application of our formalism to a galactic catalogue (VESPA)
suggest that SNIa come, in average, from small metallicity progenitors both at low redshifts
(contrary to expectations) and in galaxies with high star-formation activity. In spite of large
uncertainties in the metallicities derived from the catalogue, the gross trends of ¯ZIa vs. Zhost
obtained from VESPA for different galaxy types are roughly consistent with our theoretical
estimates.
Autor(es): Bravo Guil, Eduardo - Badenes Montoliu, Carles -
Id.: 52940862
Idioma:
inglés
-
Versión: 1.0
Estado: Final
Tipo: 15 p. -
Palabras clave: Àrees temàtiques de la UPC - Física - Astronomia i astrofísica -
Tipo de recurso:
Article
-
Tipo de Interactividad: Expositivo
Nivel de Interactividad: muy bajo
Audiencia:
Estudiante
- Profesor
- Autor
-
Estructura: Atomic
Coste: no
Copyright: sí
: Open Access
Formatos: 15 p. -
Requerimientos técnicos: Browser: Any -
Relación:
[References] http://arxiv.org/abs/1102.1586
Fecha de contribución: 05-may-2013
Contacto:
Localización:
* Bravo, E.; Badenes, C. Is the metallicity of their host galaxies a good measure of the metallicity of Type Ia supernovae?. "Monthly notices of the Royal Astronomical Society", Juny 2011, vol. 414, p. 1592-1606.
* 0035-8711
* doi:10.1111/j.1365-2966.2011.18498.x
