The FUSE Spectrum of the Planetary Nebula SwSt 1: Evidence for Inhomogeneities in the Gas and Dust

Details The FUSE Spectrum of the Planetary Nebula SwSt 1: Evidence for Inhomogeneities in the Gas and Dust The FUSE Spectrum of the Planetary Nebula SwSt 1: Evidence for Inhomogeneities in the Gas and Dust

2005-02-16

arxiv.org/abs/astro-ph/0502321v1

Astrophys.J. 625 (2005) 368-384

Astronomy and Astrophysics

Astrophysics

46 pages, 4 figures. Accepted for publication in the Astrophysical Journal

Scientific paper

10.1086/429613

[Abridged] We present Far Ultraviolet Spectroscopic Explorer (FUSE) observations of the young, compact planetary nebula (PN) SwSt 1 along the line of sight to its central star HD 167362. We detect circumstellar absorption lines from several species against the continuum of the central star. The physical parameters of the nebula derived from the FUSE data differ significantly from those found from emission lines. We derive an electron density n_e = 8800^{+4800}_{-2400} cm^{-3} from the column density ratio of the excited S III fine structure levels, which is at least a factor of 3 lower than all prior estimates. The gaseous iron abundance derived from the UV lines is quite high ([Fe/S] = -0.35+/-0.12), which implies that iron is not significantly depleted into dust. In contrast, optical and near-infrared emission lines indicate that Fe is more strongly depleted: [Fe/H] = -1.64+/-0.24 and [Fe/S] = -1.15+/-0.33. We do not detect nebular H_2 absorption, to a limit N(H_2) < 7\times10^14 cm^{-2}, at least four orders of magnitude lower than the column density estimated from infrared H_2 emission lines. Taken together, the lack of H_2 absorption, low n_e, and high gaseous Fe abundance derived from the FUSE spectrum provide strong evidence that dense structures (which can shield molecules and dust from the destructive effects of energetic stellar photons) are not present along the line of sight to the central star. On the other hand, there is substantial evidence for dust, molecular material, and dense gas elsewhere in SwSt 1. Therefore, we conclude that the nebula must have an inhomogeneous structure.

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