We present a flexible interactive 3D morpho-kinematical modeling application for astrophysics. Compared to other systems, our application reduces the restrictions on the physical assumptions, data type, and amount that is required for a reconstruction of an object's morphology. It is one of the first publicly available tools to apply interactive graphics to astrophysical modeling. The tool allows astrophysicists to provide a priori knowledge about the object by interactively defining 3D structural elements. By direct comparison of model prediction with observational data, model parameters can then be automatically optimized to fit the observation. The tool has already been successfully used in a number of astrophysical research projects.
An early tool for the rendering part of the astrophysical modeling process was our earlier work @cite_8 which was able to reproduce many standard forms of observational data from a given model. Similar codes have been used by Santander-Garc ' @cite_19 and @cite_28 . The model itself, however, still had to be hard-coded into the program, making the modeling part inherently cumbersome. Steffen and L 'opez @cite_17 later incorporated their spectral renderer into a commercial modeling system as a plugin. This simplified the modeling process to a large extent, but performance and usability were still far from the quality of an integrated modeling and rendering system.
@cite_28 @cite_19 @cite_17 @cite_8
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We present an atlas of Hubble Space Telescope images and ground-based, long-slit, narrowband spectra centered on the 6584 A line of [N II] and the 5007 A line of [O III]. The spectra were obtained for a variety of slit positions across each target (as shown on the images) in an effort to account for nonspherical nebular geometries in a robust manner. We have extended the prolate ellipsoidal shell model originally devised by Aaquist, Zhang, and Kwok to generate synthetic images, as well as long-slit spectra. Using this model, we have derived basic parameters for the subsample of PNe that present ellipsoidal appearances and regular kinematic patterns. We find differences between our parameters for the target PNe as compared to those of previous studies, which we attribute to increased spatial resolution for our image data and the inclusion of kinematic data in the model fits. The data and analysis presented in this paper can be combined with detections of nebular angular expansion rates to determine precise distances to the PN targets. The structure and kinematics of the bipolar nebula Mz 3 have been investigated by means of HST, CTIO and ESO images and spectra. At least four distinct outflows have been identified which, from the inside to the outside, are the following: a pair of bright bipolar lobes, two opposite highly collimated column-shaped outflows, a conical system of radial structure, and a very dim, previously unnoticed, low-latitude and flattened (ring-like) radial outflow. A simple Hubble-law describes the velocity field of the ballisticaly expanding lobes, columns and rays, suggesting that their shaping has being done at very early stages of evolution, in a sort of eruptive events with increasing degree of collimation and expansion ages ranging from ∼600 for the inner structures to ∼1600 years (per kpc to the nebula) for the largest ones. We present a powerful new tool to analyse and disentangle the 3-D geometry and kinematic structure of gaseous nebulae. The method consists in combining commercially available digital animation software to simulate the 3-D structure and expansion pattern of the nebula with a dedicated, purpose-built rendering software that produces the final images and long slit spectra which are compared to the real data. We show results for the complex planetary nebulae NGC 6369 and Abell 30 ABSTRACT We have used high resolution longslit spectroscopy to investigate the ionized gasin the active galaxy IRAS 04210+0400 and its association with the radio structure.We suggest that two of the ionized components are associated with the centraldouble radio source and observe that the relative positions of these components varyfor diﬀerent emission lines. Both results are consistent with the radio componentsrepresenting the working surfaces of a pair of jets emerging from the centre of thegalaxy. In this scenario, the optical emission in the centre arises behind the bowshocksproduced by the jets in the interstellar medium.The emission lines are detected and show a dramatic (≈900 km s −1 ) spreadin velocity at the position of the radio lobe hotspots. We suggest a model whichexplains this phenomenon as the result of a jet head emerging through the boundarybetween the interstellar and intergalactic medium. A similar scenario has previouslybeen suggested as a model to explain wide angle tail radio sources (WAT’s). Based onthis model, we simulate the longslit spectra of these regions and compare the resultswith the observations.Key words: galaxies: active - galaxies: individual: IRAS 04210+0400 - galaxies: jets- galaxies: kinematics and dynamics - galaxies: Seyfert