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3D Reconstruction of Emission and Absorption in Planetary Nebulae

MPG-Autoren
http://pubman.mpdl.mpg.de/cone/persons/resource/persons44928

Lintu,  Andrei
Computer Graphics, MPI for Informatics, Max Planck Society;
Graphics - Optics - Vision, MPI for Informatics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons44911

Lensch,  Hendrik P. A.
Computer Graphics, MPI for Informatics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons44965

Magnor,  Marcus
Graphics - Optics - Vision, MPI for Informatics, Max Planck Society;

El-Abed,  Sasha
Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons45449

Seidel,  Hans-Peter
Computer Graphics, MPI for Informatics, Max Planck Society;

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Zitation

Lintu, A., Lensch, H. P. A., Magnor, M., El-Abed, S., & Seidel, H.-P. (2007). 3D Reconstruction of Emission and Absorption in Planetary Nebulae. In D. Fellner, T. Möller, & S. Fraser (Eds.), Volume Graphics 2007: Eurographics / IEEE VGTC Symposium Proceedings Sixth International Symposium on Volume Graphics (pp. 9-16). Aire-la-Ville, Switzerland: Eurographics Association.


Zitierlink: http://hdl.handle.net/11858/00-001M-0000-000F-1DCB-1
Zusammenfassung
This paper addresses the problem of reconstructing the 3D structure of planetary nebulae from 2D observations. Assuming axial symmetry, our method jointly reconstructs the distribution of dust and ionized gas in the nebulae from observations at two different wavelengths. In an inverse rendering framework we optimize for the emission and absorption densities which are correlated to the gas and dust distribution present in the nebulae. First, the density distribution of the dust component is estimated based on an infrared image, which traces only the dust distribution due to its intrinsic temperature. In a second step, we optimize for the gas distribution by comparing the rendering of the nebula to the visible wavelength image. During this step, besides the emission of the ionized gas, we further include the effect of absorption and scattering due to the already estimated dust distribution. Using the same approach, we can as well start with a radio image from which the gas distribution is derived without absorption, then deriving the dust distribution from the visible wavelength image considering absorption and scattering. The intermediate steps and the final reconstruction results are visualized at real-time frame rates using a volume renderer. Using our method we recover both gas and dust density distributions present in the nebula by exploiting the distinct absorption or emission parameters at different wavelengths.