Abstract
The investigation of gaseous nebulae, emitting in forbidden lines, is often based extensively on diagnostic diagrams. The special physics of these lines often allows for disentangling with a few line ratios normally coupled thermodynamic parameters like electron temperature, density and properties of the photo-ionizing radiation field. Diagnostic diagrams are usually used for the investigation of planetary nebulae as a total. We investigated the extension of such integrated properties towards spatially resolved 2D diagnostics, using Hubble Space Telescope/Wide Field Planetary Camera 2 (HST/WFPC2) narrow band images. For this purpose, we also derived a method to isolate pure Hα emission from the [N ii] contamination as normally suffering in the F656N HST/WFPC2 filter.
Highlights
According to the standard Interacting Stellar Winds (ISW) model, Planetary Nebula (PN singular, PNe plural) result from the interaction of a fast, hot and, thin wind developed at the post-AGB phase, which compresses and accelerates the dense material ejected during the final AGB phase [1]
The log (Hα/[N II]) versus log (Hα/[S II]) diagnostic diagrams normally were used for spectroscopic results of the nebulae as a total [23,24,28]
There, the data along a long slit spectroscopy was used in detail, to derive a regression line, which was applied to the entire 2D image from HST
Summary
According to the standard Interacting Stellar Winds (ISW) model, Planetary Nebula (PN singular, PNe plural) result from the interaction of a fast, hot and, thin wind developed at the post-AGB phase, which compresses and accelerates the dense material ejected during the final AGB phase [1]. We investigated the extension of such integrated properties towards spatially resolved 2D diagnostics, using Hubble Space Telescope/Wide Field Planetary Camera 2 (HST/WFPC2) narrow band images. These so-called Multiple Shell Planetary Nebulae (MSPNe) are ideal candidates to study both macro and micro structures at PNe. Mainly thanks to the great detail on HST images, remarkable low ionization structures such as FLIERs (Fast Low Ionization Emission Regions) or LISs (Low Ionization emission line Structures) have been observed in several MSPNe (see e.g., [12,13,14]).
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