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Buzzoni, A., & Arnaboldi, M.:
"Planetary Nebulae as tracers of the Intergalactic stellar background: a population synthesis theoretical approach",
2004, ESO intl. Workshop on "Planetary Nebulae beyond the Milky Way", Garching bei München (Germany), May 19-21, 2004 - ESO Astrophysics Symposia, eds. L. Stanghellini, J.R. Walsh & N.G. Douglas, (Springer Verlag: Heidelberg), p. 355.

Summary:
We wish to assess the relationship between the population of planetary nebulae (PNe) and a given parent stellar population from a theoretical point of view. Our results rely on original population synthesis models used to estimate the expected luminosity-specific PN density accounting for different evolutionary scenarios and star formation histories, as observed in galaxies in the near Universe. For a complete PN sample, we find that 1 PN/1.5E06 L(sun) a safe (IMF-independent) lower limit to the traced global bolometric luminosity of the parent stellar population. A tentative application to Virgo cluster data allows us to place a lower limit at ~7% for the global B luminosity of the cluster provided by "loose" intergalactic stars.






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  Unpublished data -

Set 1: PN lifetime and luminosity-specific PN density for SSP synthesis models. ASCII data sources for Figs. 2 and 3.

Set 2: luminosity-specific PN density (in bolometric) for template galaxy models, according to Buzzoni (2002). ASCII data sources for Fig. 4.
Figure 1 - Theoretical fuel consumption for stars along the Hot-PAGB evolution according to the models of Paczynski (1971; solid curve) and Vassiliadis and Wood (1994; solid dots and triangles). Fuel is expressed in Hydrogen-equivalent solar mass. The stellar core-mass range to produce PNe is marked, after Dorman et al. (1993).
Figure 2 - Hot-PAGB core mass lifetime, for SSP evolution according to B89 synthesis models. A Salpeter IMF is assumed, and a Reimers mass loss rate coefficient η = 0.3. The explored metallicity spans the range from Z~1/20--2 Z(sun), as labeled in the plot. The PN dynamical timescale [τ(dyn)] is also marked, for reference.
Figure 3 - Theoretical luminosity-specific PN density for SSPs of different metallicity. Models are according to Buzzoni (1989), with the distinctive parameters as in Fig. 2.
Figure 4 - Expected luminosity-specific PN density for template galaxy models (labeled with the corresponding Hubble type), according to Buzzoni (2002). Each curve tracks galaxy evolution from 5 Gyr to 15 Gyr (small solid dots), as labeled for the case of Ellipticals. Big triangles report the empirical estimate of α = N(PN)/L(gal) from the PN census of Jacoby (1980) for the galaxies in the Local Group. The case of the Milky Way is singled out in the plot by the big solid dot.



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AB/Apr 2006