Proper Plasma Analysis Practice (PPAP), an Integrated Procedure of the Extinction Correction and Plasma Diagnostics: a Demo with an HST/WFC3 Image Set of NGC6720

TL;DR

This paper introduces PPAP, an integrated method for plasma diagnostics that combines extinction correction and plasma analysis iteratively, validated with HST images of NGC 6720, leading to consistent abundance and physical parameter maps.

Contribution

The paper presents PPAP, a novel integrated procedure that improves plasma diagnostics accuracy by simultaneous analysis of extinction and plasma parameters in spatially-resolved spectroscopy.

Findings

Self-consistent extinction and plasma maps were derived.

Metal abundance maps from different lines were consistent.

Ionized gas-to-dust ratio was estimated between 437 and 1600.

Abstract

In this work, we propose a proper plasma analysis practice (PPAP), an updated procedure of plasma diagnostics in the era of spatially-resolved spectroscopy. In particular, we emphasize the importance of performing both of the extinction correction and the direct method of plasma diagnostics simultaneously as an integrated process. This approach is motivated by the reciprocal dependence between critical parameters in these analyses, which can be resolved by iteratively seeking a converged solution. The use of PPAP allows us to eliminate unnecessary assumptions that prevent us from obtaining an exact solution at each element of the spectral imaging data. Using a suite of HST/WFC3 narrowband images of the planetary nebula, NGC 6720, we validate PPAP by (1) simultaneously and self-consistently deriving the extinction, c(Hb), and electron density/temperature distribution, (n_e, T_e), maps that are consistent with each other, and (2) obtaining identical metal abundance distribution maps, (n(N^+)/n(H^+), n(S^+)/n(H^+)), from multiple emission line maps at different wavelengths/transition energies. We also determine that the derived c(Hb) consists both of the ISM and circumsource components and that the ionized gas-to-dust mass ratio in the main ring is at least 437 and as high as about 1600. We find that, unless we deliberately seek self-consistency, uncertainties at tens of per cent can easily arise in outcomes, making it impossible to discern actual spatial variations that occurs at the same level, defeating the purpose of conducting spatially resolved spectroscopic observations.