Using the Cloudy_3D code (Morisset, this conference), we run a set of models to build a catalog of emission line profiles of PNe. The goal is to cover the main morphologies (spherical, ellipsoidal, bipolar, thin or thick shells) and to compute profiles changing the orientation of the nebula, the expansion velocity law (including or not turbulence), the position/size of the aperture. The results is a huge set of profiles and PV-diagrams that can be compared to observations as a help to derive morpho-kinematical properties of real objects.

Recent intensive campaigns to monitor the variable broad emission lines of AGN have provided a wealth of observational data. To reliably derive the BLR structure from such data requires a detailed comparison with physically realistic models. To provide such models we have combined photoionization calculations with a BLR modelling code. We find that the line emission is significantly anisotropic for the majority of lines at some radii in our models, particularly where the ionization parameter is large. As both anisotropic line emission and negative responsivity can have a substantial impact on the form of response functions, they must be taken into account when comparing BLR models to monitoring data. Differentiating between the effects of anisotropy and negative responsivity requires comparison of the variability behaviour of lines covering a wide range in ionization state with detailed photoionization models similar to those presented here. Failure to take such physical effects into account will lead to incorrect conclusions regarding the BLR structure.

Based on the form of the anisotropic response functions for our models, we argue that in NGC5548 the high ionization lines (including CIII] λ1909) can be explained by a spherical BLR component which has a significant radial ionization parameter gradient. The clouds in this component may be optically thin at the Lyman limit in the inner part of the BLR due to the high ionization parameter. The bulk of the low ionization lines, and in particular almost all of the Balmer line emission, arises from a non-spherical BLR component, possibly an accretion disc.

We have also investigated the accuracy of the linear response approximation by implicitly calculating the emissivity as a function of continuum level. For several lines the response is significantly non-linear over the typical continuum variability range of AGN. The form of the response functions is therefore luminosity dependent. Work is under way to incorporate this effect into the maximum-entropy-method used to recover response functions from monitoring data.

We present a detailed study of the warmers phase in a starburst as a scenario for AGN (Terlevich & Melnick 1985). A numerical code (“ET”) was developed to compute the time evolution of the total spectrum of an ionizing cluster. ET is based in Maeder & Meynet (1988) and Maeder (1990) tracks and in model atmospheres. The ionizing spectra were input into the photoionization code Aangaba (Gruenwald & Viegas 1991) to calculate the nebular emission for a grid of models covering different densities, ionization parameters, metallicities and cluster ages. The emission line spectrum go through an “active phase” beginning at ≍ 3 Myrs, which lasts for about 3 Myrs, when the population of warmers disapears. Metallicities between 1/2 and 2 Z⊙ are necessary to generate AGN line ratios. The lower limmit is due to the fact that fewer warmers occur in metal poor regions (due to the smaller mass loss rates) and even if some do occur the line ratios would resemble an HII galaxy rather than a Seyfert 2 or a LINER. The upper limmit is set by strong line cooling of the emission nebula. The chemical pollution of the gas by the processed stellar winds from the very massive stars produce straightforwardly a N overabundance as that observed in many AGN. In Figure 1a and b, we show the process of heavy element enrichment as a function of time parametrized by γ—a quantity which measures the mass ejected by stars relative to the mass of gas surrounding the stellar association (see Cid Fernandes et al. 1991). The chemical yields were taken from Maeder (1990) models.